From owner-public@setileague.org Wed Jun 1 09:28:49 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j51GSkUw032409 for ; Wed, 1 Jun 2005 09:28:49 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id MAA10944 for public-list; Wed, 1 Jun 2005 12:18:43 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f29.bay103.hotmail.com [65.54.174.39]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id MAA10940; Wed, 1 Jun 2005 12:18:41 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 1 Jun 2005 09:18:06 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Wed, 01 Jun 2005 16:18:05 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: FW: Friends of PlanetQuest Newsletter Vol 1, No 4 Date: Wed, 01 Jun 2005 12:18:05 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 01 Jun 2005 16:18:06.0474 (UTC) FILETIME=[7E6006A0:01C566C5] Sender: owner-public@setileague.org Precedence: bulk >From: PlanetQuest Info >To: undisclosed-recipients: ; >Subject: Friends of PlanetQuest Newsletter Vol 1, No 4 >Date: Wed, 01 Jun 2005 08:57:48 -0700 > >Friends of PlanetQuest Newsletter Vol 1, No 4 > >**The PlanetQuest Mission: To inspire the people of the world with the >thrill of individual discovery, a better understanding of our uniquely >precious planet, and a wider perspective on our place in the universe.** > >Dear Friends, > >May has turned out to be a month of hard work. During the past month, we >have begun work on incorporating translations of some of our pages, added a >new director to our board, hosted a star party at Lick Observatory (well, >it was a cloud party spiced with historical observations!) with a UC Light >and Optics class of Dr. Doyle’s, added to the website, and begun equipment >modifications on our telescopes. > >We are forging ahead, looking forward to a very busy summer, and looking >forward to telling you, our friends and supporters, all about it. > >=================================== > >**A New Board of Directors Member** > >In early May, Dr. Zoran Ninkov of the Rochester Institute of Technology >accepted our invitation to become a member of the PlanetQuest Board of >Directors. Dr. Ninkov has collaborated with PlanetQuest cofounder and >President Dr. Laurance Doyle for many years, providing us with >state-of-the-art CCDs as well as technical and observational assistance for >nearly a decade in the world’s first search for extrasolar >terrestrial-sized planets. (References to this work can be found at >http://planetquest.org/about/research/extrasolar.html.) Dr. Ninkov has been >involved in the field of astronomy for many years. A current (although >brief) bio of him can be found on our website >(http://planetquest.org/about/people/). > >**Other Collaborations** > >We are pleased to announce that PlanetQuest and the SETI Institute >(http://www.seti.org) are joining forces. SETI Institute will provide >materials and technical support for the PlanetQuest mission, and the two >organizations will participate in selected joint fundraising efforts. This >is not only a mutually beneficial but also extremely natural collaboration. >For many years, SETI Institute has been engaged in a radio search for >extraterrestrial intelligence, and has now expanded that search with an >optical component. SETI also supported early distributed computing projects >(SETI@home) that many of you may have participated in, and that has >provided the foundation for the PlanetQuest Collaboratory. We are extremely >excited about our two organizations working together to bring the >excitement of discovery to you. > >**New Download!** > >Dr. Bob Slawson, one of our observing astronomers, has created a nifty >planet transit simulator. You can specify different types of observing >scenarios (both earth- and space-based), star and planet sizes, offset, and >signal to noise characteristics. The simulator then renders an animation of >your target as well as a sample light curve, based on your settings. It’s >a great way to understand the basics of the photometric detection method >you’ll use to detect planets and other phenomena. Download it at: >http://www.planetquest.org/download/PlanetTransit.jar. If you have Java >(required), you can run it by typing ‘java –jar PlanetTransit.jar’ (without >the quotes) in the directory where you saved it. > >**Our Education Project** > >We continue to add pages to our Learn category on the website >(http://www.planetquest.org/about/learn/). Several additional pages are >waiting “in the wings,” so to speak, as we await permissions on photos and >other input. As brief as the Learn pages are, we are very proud of the >content and information provided, and we of course provide links to other >sites of interest and reference materials. We will soon add an updated and >improved home page for Learn, as well as several new Learn offerings. And >if you have any requests, let us know! > >**The Collaboratory** > >Imagine the next generation of distributed computing—a way not just to >contribute your cpu cycles to other people’s science projects, but also to >perform your own experiments, collaborate with others around the world in >different types of observations, classify stars no one has ever classified >before, and learn about math, astronomy, and physics. Imagine a distributed >computing tool that encourages you to create and share your own >constellations and asterisms, that allows you to participate in global >observing missions, and that creates communities. Watch the PlanetQuest >website for additional details soon about what we’re building into the >Collaboratory—there’s nothing like it! > >**Astronomy and Observing** > >Astronomy is the most interesting science to work with… okay, let’s say “a” >most interesting science, not to be too biased. For one thing, the >scientist (astronomer) cannot control the experiment; either he/she is >ready to photograph the event when it occurs, or not. The event occurs >regardless. Years ago, we traveled to Baja California to view the 1991 >solar eclipse and had to set up cameras and other equipment in time to be >ready for it. We were ready, but some of the scientists from other fields >were nervous wrecks, realizing there would be no second chances! > >Such is it now, with our observations on the Crossley 0.9 meter telescope >at Lick Observatory. The field corrector we have ordered has been delayed, >which in turn has delayed our observations until mid-August or so. The part >of the Galaxy we will be observing will be “setting” toward the end of >September, or at least, not optimally observable. This is still a >developing issue and our astronomers are working with the company producing >the equipment. All is not lost, as we still have our month’s observing time >on the Siding Spring 1-meter as well as two months at Lick Observatory. > >**Your Help Is Most Appreciated** > >We value your interest in PlanetQuest, and your support of every kind. Some >have offered translations of website pages; others have offered materials >or other kinds of assistance. We are thankful. If you want to make a >difference and bring positive change to our world, please consider a >contribution (we’ve made this easy: just go to >http://www.planetquest.org/support/donate), and tell someone else about us. > For as little as $10 per month, you can help us build PlanetQuest into >the world-changing organization it can be! For those thinking of >contributing on a large scale, we are happy to meet with you and explain >our project in more detail. We are a registered 501(c)(3) US nonprofit >organization, so your donations are completely tax-deductible. As always, >thank you for your interest, enthusiasm and support! > >=================================== > >**Quote of the Month** > >“What a wonderful and amazing Scheme have we here of the magnificent >Vastness of the Universe! So many Suns, so many Earths…!” > >Christianus Huygens (1670) > >=================================== > >Best Wishes, > >J. Ellen Blue >Director of Publications > >Laurance Doyle, PhD >President and Cofounder > >David Gutelius, PhD >Executive Director and Cofounder > From owner-public@setileague.org Wed Jun 1 09:41:31 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j51GfUUw030209 for ; Wed, 1 Jun 2005 09:41:30 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id MAA11276 for public-list; Wed, 1 Jun 2005 12:33:22 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f11.bay103.hotmail.com [65.54.174.21]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id MAA11272; Wed, 1 Jun 2005 12:33:20 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 1 Jun 2005 09:32:49 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Wed, 01 Jun 2005 16:32:48 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Quantifying orbital migration from exoplanet statistics and host metallicities Date: Wed, 01 Jun 2005 12:32:48 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 01 Jun 2005 16:32:49.0390 (UTC) FILETIME=[8CA250E0:01C566C7] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0505609 Date: Mon, 30 May 2005 20:00:17 GMT (49kb) Title: Quantifying orbital migration from exoplanet statistics and host metallicities Authors: W.K.M. Rice, Philip J. Armitage Comments: ApJ, in press \\ We investigate how the statistical distribution of extrasolar planets may be combined with knowledge of the host stars' metallicity to yield constraints on the migration histories of gas giant planets. At any radius, planets that barely manage to form around the lowest metallicity stars accrete their envelopes just as the gas disk is being dissipated, so the lower envelope of planets in a plot of metallicity vs semi-major axis defines a sample of non-migratory planets that will have suffered less than average migration subsequent to gap opening. Under the assumption that metallicity largely controls the initial surface density of planetesimals, we use simplified core accretion models to calculate how the minimum metallicity needed for planet formation varies as a function of semi-major axis. Models that do not include core migration prior to gap opening (Type I migration) predict that the critical metallicity is largely flat between the snow line and a semimajor axis of about 6 AU, with a weak dependence on the initial surface density profile of planetesimals. When slow Type I migration is included, the critical metallicity is found to increase steadily from 1-10 AU. Large planet samples, that include planets at modestly greater orbital radii than present surveys, therefore have the potential to quantify the extent of migration in both Type I and Type II regimes. \\ ( http://arXiv.org/abs/astro-ph/0505609 , 49kb) From owner-public@setileague.org Thu Jun 2 05:22:32 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j52CMVUw026999 for ; Thu, 2 Jun 2005 05:22:31 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id IAA09438 for public-list; Thu, 2 Jun 2005 08:11:38 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f27.bay103.hotmail.com [65.54.174.37]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id IAA09434; Thu, 2 Jun 2005 08:11:35 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 2 Jun 2005 05:11:04 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Thu, 02 Jun 2005 12:11:03 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Development of an Electronic Readout System for the Detection of Radio Emission Date: Thu, 02 Jun 2005 08:11:03 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 02 Jun 2005 12:11:04.0461 (UTC) FILETIME=[262E13D0:01C5676C] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506007 Date: Wed, 1 Jun 2005 06:20:33 GMT (97kb) Title: Development of an Electronic Readout System for the Detection of Radio Emission from Extensive Cosmic Ray Air Showers Authors: Vladimir Tryanin Comments: 6 pages with 1 figure, to be published in Electron Devices, IEEE Trans Report-no: MEPhI-05-05 \\ This paper describes the methodic of the development of an electronic readout system for the detection of radio emission from extensive cosmic ray air showers. \\ ( http://arXiv.org/abs/astro-ph/0506007 , 97kb) From owner-public@setileague.org Thu Jun 2 05:35:24 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j52CZMUw005708 for ; Thu, 2 Jun 2005 05:35:23 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id IAA09784 for public-list; Thu, 2 Jun 2005 08:25:03 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f22.bay103.hotmail.com [65.54.174.32]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id IAA09780; Thu, 2 Jun 2005 08:25:01 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 2 Jun 2005 05:24:29 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Thu, 02 Jun 2005 12:24:29 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Low Luminosity Companions to White Dwarfs Date: Thu, 02 Jun 2005 08:24:29 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 02 Jun 2005 12:24:29.0944 (UTC) FILETIME=[06490780:01C5676E] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506017 Date: Wed, 1 Jun 2005 13:02:54 GMT (862kb) Title: Low Luminosity Companions to White Dwarfs Authors: J. Farihi, E.E. Becklin, B. Zuckerman Comments: 158 pages, 59 figures, 11 tables, accepted to ApJ Supplements \\ This paper presents results of a near-infrared imaging survey for low mass stellar and substellar companions to white dwarfs. A wide field proper motion survey of 261 white dwarfs was capable of directly detecting companions at orbital separations between $\sim100$ and 5000 AU with masses as low as 0.05 $M_{\odot}$, while a deep near field search of 86 white dwarfs was capable of directly detecting companions at separations between $\sim50$ and 1100 AU with masses as low as 0.02 $M_{\odot}$. Additionally, all white dwarf targets were examined for near-infrared excess emission, a technique capable of detecting companions at arbitrarily close separations down to masses of 0.05 $M_{\odot}$. No brown dwarf candidates were detected, which implies a brown dwarf companion fraction of $<0.5$% for white dwarfs. In contrast, the stellar companion fraction of white dwarfs as measured by this survey is 22%, uncorrected for bias. Moreover, most of the known and suspected stellar companions to white dwarfs are low mass stars whose masses are only slightly greater than the masses of brown dwarfs. Twenty previously unknown stellar companions were detected, five of which are confirmed or likely white dwarfs themselves, while fifteen are confirmed or likely low mass stars. Similar to the distribution of cool field dwarfs as a function of spectral type, the number of cool unevolved dwarf companions peaks at mid-M type. Based on the present work, relative to this peak, field L dwarfs appear to be roughly 2-3 times more abundant than companion L dwarfs. Additionally, there is no evidence that the initial companion masses have been altered by post main sequence binary interactions. \\ ( http://arXiv.org/abs/astro-ph/0506017 , 862kb) From owner-public@setileague.org Thu Jun 2 05:48:19 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j52CmIUw032391 for ; Thu, 2 Jun 2005 05:48:19 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id IAA10027 for public-list; Thu, 2 Jun 2005 08:33:05 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f20.bay103.hotmail.com [65.54.174.30]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id IAA10023; Thu, 2 Jun 2005 08:33:03 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 2 Jun 2005 05:32:32 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Thu, 02 Jun 2005 12:32:32 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org, bioastro@setileague.org Subject: SETI public: Direct detection of exo-planets: GQ Lupi Date: Thu, 02 Jun 2005 08:32:32 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 02 Jun 2005 12:32:32.0480 (UTC) FILETIME=[25E62E00:01C5676F] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506011 Date: Wed, 1 Jun 2005 08:45:17 GMT (49kb) Title: Direct detection of exo-planets: GQ Lupi Authors: Ralph Neuhaeuser (AIU Jena), Eike Guenther (TLS Tautenburg), Peter Hauschildt (Sternwarte Hamburg) Comments: Proceedings ESO Workshop on The power of optical/IR interferometry \\ We present a comparison of our VLT/NACO K-band spectrum of the GQ Lupi companion with the new GAIA-dusty model atmosphere grid for T=2000 and 2900 K and log g from 0 to 4. Then, we discuss the mass estimate for GQ Lup companion. \\ ( http://arXiv.org/abs/astro-ph/0506011 , 49kb) Paper: astro-ph/0506002 Date: Tue, 31 May 2005 22:17:03 GMT (52kb) Title: Low-Mass Runaway Stars from the Orion Trapezium Cluster Authors: Arcadio Poveda, Christine Allen and Alejandro Hernandez-Alcantara \\ In the course of a search for common proper motion binaries, in the Jones & Walker (JW) catalogue of proper motions in the Orion Nebula Cluster, we came across several faint stars with proper motions larger than one arcsecond per century and probabilities of membership P larger than 0.90. Such stars are interesting because they could be low-mass runaway stars recently accelerated by n-body interactions in compact multiple systems. Of particular interest among these stars is JW 451, which has a P = 0.98, the largest transverse velocity among all the stars with P larger or equal than 0.5 (69 km/s), and a proper motion vector which suggests that it was accelerated by the component C of the Trapezium some 1000 years ago. A closer examination of those JW stars with proper motion larger than one arcsec per century revealed that two other stars, JW 349 and JW 355 (with transverse velocities of 38 and 90 km/s respectively), in spite of being listed with P = 0 by JW, should also be considered part of the cluster, because these objects are also externally ionized proplyds. In fact, Hillenbrand (1997) assigns to them probabilities of membership of 0.99. Moreover, the proper motion errors of these two stars are relatively small, and so they are good candidates to be runaway stars recently accelerated in the Orion Nebula Cluster. \\ ( http://arXiv.org/abs/astro-ph/0506002 , 52kb) From owner-public@setileague.org Thu Jun 2 10:09:36 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j52H9YUw025834 for ; Thu, 2 Jun 2005 10:09:35 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id NAA16095 for public-list; Thu, 2 Jun 2005 13:02:02 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f27.bay103.hotmail.com [65.54.174.37]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id NAA16079; Thu, 2 Jun 2005 13:01:58 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 2 Jun 2005 10:01:26 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Thu, 02 Jun 2005 17:01:26 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: The Center for the Study of Life in the Universe Date: Thu, 02 Jun 2005 13:01:26 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 02 Jun 2005 17:01:26.0709 (UTC) FILETIME=[B6A62650:01C56794] Sender: owner-public@setileague.org Precedence: bulk Science/Astronomy: * The Center for the Study of Life in the Universe http://www.space.com/searchforlife/seti_drake_LITU_050602.html How does life start? How does it evolve, and what fabulous creatures can evolution produce? How often do intelligent creatures appear in the giant tapestry of life? It is exactly these questions, and all of them, which are being addressed by the scientists of the Center for the Study of Life in the Universe, LITU. * First Shooting Star Seen from Mars http://www.space.com/scienceastronomy/050601_mars_meteor.html NASA's Spirit rover photographed a streak of light that was likely part of a martian meteor shower, scientists announced today. From owner-public@setileague.org Fri Jun 3 11:09:01 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j53I8wUw018105 for ; Fri, 3 Jun 2005 11:09:01 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id NAA20586 for public-list; Fri, 3 Jun 2005 13:57:42 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f2.bay103.hotmail.com [65.54.174.12]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id NAA20581; Fri, 3 Jun 2005 13:57:40 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 3 Jun 2005 10:57:09 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Fri, 03 Jun 2005 17:57:08 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: FW: NASA SCIENTISTS CONFIRM LIQUID WATER ON EARLY EARTH Date: Fri, 03 Jun 2005 13:57:08 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 03 Jun 2005 17:57:09.0082 (UTC) FILETIME=[A9458BA0:01C56865] Sender: owner-public@setileague.org Precedence: bulk >From: "NASANEWS@mail.arc.nasa.gov" >To: ames-releases@lists.arc.nasa.gov >Subject: NASA SCIENTISTS CONFIRM LIQUID WATER ON EARLY EARTH >Date: Fri, 3 Jun 2005 10:12:03 -0700 > > > >Nicholas A. Veronico/Michael Mewhinney June 3, 2005 >Ames Research Center, Moffett Field, Calif, >Phone: 650/604-1939, 650/604-9000 >E-mail: nveronico@mail.arc.nasa.gov > >NEWS RELEASE: 05-35 > >NASA SCIENTISTS CONFIRM LIQUID WATER ON EARLY EARTH > >Research funded partly by NASA has confirmed the existence of liquid water >on the Earth's surface more than 4 billion years ago. > >Scientists have found that the Earth had formed patterns of crust >formation, erosion and sediment recycling as early as 4.35 billion years >ago. Their findings came during a study of zircon crystals formed during >the earliest period of Earth's history, the Hadean Eon (4.5 billion to 4.0 >billion years ago). > >"NASA is interested in how early the Earth had abundant liquid water. If >oceans form early in a planet's history, then so can life," said Carl >Pilcher, senior scientist for astrobiology at NASA Headquarters, >Washington. "Learning how early oceans formed on Earth will help us >understand where else oceans and perhaps even life may have formed in this >solar system and in planetary systems around other stars." > >"This work provides direct evidence that the Earth was probably habitable >within a hundred million years of its formation," said Bruce Runnegar, >director of the NASA Astrobiology Institute (NAI) at NASA Ames Research >Center, Moffett Field, Calif., which provided some of the study's funding. > >Published in the May 6, 2005, edition of Science, the research was >conducted by T. Mark Harrison of the Research School of Earth Sciences, >Australian National University, Canberra and the University of California, >Los Angeles; and E. Bruce Watson of the Department of Earth & Environmental >Sciences at Rensselaer Polytechnic Institute, Troy, N.Y. Field research was >completed in Western Australia's Jack Hills, which preserve a record of the >Hadean Eon. > >Watson and Harrison devised a new method of determining the temperatures at >which the rocks formed. The team extracted and examined more than 50,000 >zircons, crystals about the width of a human hair, which have been exposed >through natural erosion in the Jack Hills. From the 50,000 zircons, only a >couple of hundred were older than 4.2 billion years. Measuring the >temperature at which the rocks melt gives an indication of the conditions >in which they formed. > >"Rocks formed as a result of the thermal energy from meteorite impacts >would be bone dry and melt at greater than 900 degrees Celsius," said >Harrison. "In contrast, our study has found that Hadean rocks melted at a >consistent average temperature of 690 degrees Celsius. Water, which is a >very powerful catalyst, must have been present in very large amounts for >rocks to melt at such a relatively low temperature." > >This discovery supports the proposal by Harrison's group four years earlier >that a heavy oxygen isotope signature in the Hadean zircons is evidence for >liquid water at or near the Earth's surface by 4.3 billion years ago. > >The NAI, founded in 1997, is a partnership between NASA, 16 major U.S. >teams and five international consortia. NAI's goal is to promote, conduct >and lead integrated multidisciplinary astrobiology research and to train a >new generation of astrobiology researchers. > >For more information about the NAI on the Internet, visit: > >http://nai.arc.nasa.gov > >For information about NASA and agency programs on the Internet, visit: > >http://www.nasa.gov > >-end- > > > > >To receive Ames news releases, send an e-mail with the word "subscribe" in >the subject line to: ames-releases-request@lists.arc.nasa.gov. To >unsubscribe, send an e-mail to the same address with "unsubscribe" in the >subject line. Also, the NASA Ames News homepage at URL, >http://www.nasa.gov/centers/ames/news/index.html includes news releases and >JPEG images in AP Leaf Desk format minus embedded captions. > From owner-public@setileague.org Fri Jun 3 20:55:20 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j543tIUw010693 for ; Fri, 3 Jun 2005 20:55:19 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id XAA05312 for public-list; Fri, 3 Jun 2005 23:47:51 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-dav2.bay103.hotmail.com [65.54.174.74]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id XAA05302; Fri, 3 Jun 2005 23:47:33 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 3 Jun 2005 20:47:02 -0700 Message-ID: Received: from 65.54.174.207 by BAY103-DAV2.phx.gbl with DAV; Sat, 04 Jun 2005 03:47:02 +0000 X-Originating-IP: [65.54.174.207] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "BioAstro" Cc: "setipublic" Subject: SETI public: Stability of phantom wormholes Date: Fri, 3 Jun 2005 23:46:57 -0400 MIME-Version: 1.0 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: 7bit X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MIMEOLE: Produced By MSN MimeOLE V9.10.0011.1703 X-RFC2646: Format=Flowed; Original Seal-Send-Time: Fri, 3 Jun 2005 23:46:57 -0400 X-OriginalArrivalTime: 04 Jun 2005 03:47:02.0920 (UTC) FILETIME=[11A4A080:01C568B8] Sender: owner-public@setileague.org Precedence: bulk Paper (*cross-listing*): gr-qc/0506001 Date: Tue, 31 May 2005 22:23:46 GMT (27kb) Title: Stability of phantom wormholes Authors: Francisco S. N. Lobo Comments: 9 pages, 9 figures, Revtex4 \\ It has recently been shown that traversable wormholes may be supported by phantom energy. In this work phantom wormhole geometries are modelled by matching an interior traversable wormhole solution, governed by the equation of state $p=\omega \rho$ with $\omega<-1$, to an exterior vacuum spacetime at a finite junction interface. The stability analysis of these phantom wormholes to linearized spherically symmetric perturbations about static equilibrium solutions is carried out. A master equation dictating the stability regions is deduced, and by separating the cases of a positive and a negative surface energy density, it is found that the respective stable equilibrium configurations may be increased by strategically varying the wormhole throat radius. The first model considered, in the absence of a thin shell, is that of an asymptotically flat phantom wormhole spacetime. The second model constructed is that of an isotropic pressure phantom wormhole, which is of particular interest, as the notion of phantom energy is that of a spatially homogeneous cosmic fluid, although it may be extended to inhomogeneous spherically symmetric spacetimes. \\ ( http://arXiv.org/abs/gr-qc/0506001 , 27kb) From owner-public@setileague.org Sat Jun 4 12:49:40 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j54JndUw009807 for ; Sat, 4 Jun 2005 12:49:40 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id PAA28470 for public-list; Sat, 4 Jun 2005 15:40:52 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from host224.ipowerweb.com ([66.235.220.224]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id PAA28461 for ; Sat, 4 Jun 2005 15:40:47 -0400 (EDT) Received: from cpe-66-27-116-71.san.res.rr.com ([66.27.116.71] helo=Zeke) by host224.ipowerweb.com with smtp (Exim 4.43) id 1DeeV5-0004Wn-PI; Sat, 04 Jun 2005 12:40:07 -0700 Message-ID: <000f01c5693d$3b946670$887ba8c0@Zeke> From: "James Brown" To: "SETI League Public" , "SETI League Argus" Subject: SETI public: Remote SETI Back On Line Date: Sat, 4 Jun 2005 12:40:15 -0700 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_000C_01C56902.8EF79B10" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: Microsoft Outlook Express 6.00.2800.1478 X-MimeOLE: Produced By Microsoft MimeOLE V6.00.2800.1478 X-AntiAbuse: This header was added to track abuse, please include it with any abuse report X-AntiAbuse: Primary Hostname - host224.ipowerweb.com X-AntiAbuse: Original Domain - seti1.setileague.org X-AntiAbuse: Originator/Caller UID/GID - [47 12] / [47 12] X-AntiAbuse: Sender Address Domain - seti.net X-Source: X-Source-Args: X-Source-Dir: Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_000C_01C56902.8EF79B10 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable I wondered why no one was using the system lately until I tried it my = self - It was off line (duh). The problem was that I had blown up the address in the SETI Net server = and so no clients could find the computer connected to my antenna and = receiver.=20 The receiver and antenna are now on line and ready for use. If you need = a client download it at: http://www.seti.net/SETINet/SETINet.htm For control of the receiver follow the instructions at: http://www.seti.net/SETINet/Engineering/Engineering.htm item #67 If your interested how your client finds its way to my computer do this: Start www.SETI.net and then select View | Source. See the entry: That's the current = address of the Remote SETI Server and changes from time to time. Every = time you start your client it goes to this location and extracts the = current address and then connects to it. Argus Station: DM12jb James Brown W6KYP Jim@SETI.Net [put 'SETI' in subject line] www.seti.net ------=_NextPart_000_000C_01C56902.8EF79B10 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
I wondered why no one was using the = system lately=20 until I tried it my self - It was off line (duh).
The problem was that I had blown up the = address in=20 the SETI Net server and so no clients could find the computer connected = to my=20 antenna and receiver. 
 
The receiver and antenna are now on = line and ready=20 for use.  If you need a client download it at:
http://www.seti.net/SETI= Net/SETINet.htm
 
For control of the receiver follow the = instructions=20 at:
http://w= ww.seti.net/SETINet/Engineering/Engineering.htm =20 item #67
 
If your interested how your client = finds its way to=20 my computer do this:
Start www.SETI.net  and then select View = |=20 Source.  See the entry: <meta name=3D"RemoteSETI"=20 content=3D"66.27.116.71">  That's the current address of the = Remote SETI=20 Server and changes from time to time.  Every time you start your = client it=20 goes to this location and extracts the current address and then connects = to=20 it.
 
 
Argus Station: DM12jb
James = Brown
W6KYP
Jim@SETI.Net [put 'SETI' in subject = line]
www.seti.net
------=_NextPart_000_000C_01C56902.8EF79B10-- From owner-public@setileague.org Sat Jun 4 16:29:19 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j54NTIUw010919 for ; Sat, 4 Jun 2005 16:29:18 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id TAA04249 for public-list; Sat, 4 Jun 2005 19:21:32 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f40.bay103.hotmail.com [65.54.174.50]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id TAA04239; Sat, 4 Jun 2005 19:21:15 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Sat, 4 Jun 2005 16:20:45 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Sat, 04 Jun 2005 23:20:44 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: fpspace@friends-partners.org Cc: bioastro@setileague.org, public@setileague.org Subject: SETI public: I hope this GALEX film doesn't get turned into a UFO film Date: Sat, 04 Jun 2005 19:20:44 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 04 Jun 2005 23:20:45.0081 (UTC) FILETIME=[0885A090:01C5695C] Sender: owner-public@setileague.org Precedence: bulk Check the second film from GALEX from this article. It looks like the satellites are doing a U-turn in orbit. I just want to nip in the bud any claims that NASA has captured another UFO via imagery and are suppressing the data, etc. GALEX PROVIDES ULTRAVIOLET GOODIES The Galaxy Evolution Explorer (GALEX) satellite inadvertently picked up an assortment of astronomical goodies in our solar neighborhood while surveying distant galaxies in ultraviolet light. The satellite's large field of view, 1.5 degrees, catches many nearby objects that unexpectedly flare and glow in this high-energy part of the spectrum. Barry Welsh (University of California, Berkeley) described some of the interesting phenomena that turned up in GALEX's "contaminated" observations, including an exciting flare in a red-dwarf star whose brightness increased more than 10,000 times. The unique capabilities of the GALEX cameras allow astronomers to make stellar observations on a much faster timescale than normal. Its photon counting camera can take a picture about once every 0.05 second... >http://SkyandTelescope.com/news/article_1523_1.asp From owner-public@setileague.org Sun Jun 5 00:06:19 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5576HUw009549 for ; Sun, 5 Jun 2005 00:06:18 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id CAA14287 for public-list; Sun, 5 Jun 2005 02:56:50 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from host224.ipowerweb.com ([66.235.220.224]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id CAA14283 for ; Sun, 5 Jun 2005 02:56:47 -0400 (EDT) Received: from cpe-66-27-116-71.san.res.rr.com ([66.27.116.71] helo=Zeke) by host224.ipowerweb.com with smtp (Exim 4.43) id 1Dep3P-0000Vc-1C for public@seti1.setileague.org; Sat, 04 Jun 2005 23:56:15 -0700 Message-ID: <000801c5699b$adf8ac90$887ba8c0@Zeke> From: "James Brown" To: "SETI League Public" Subject: SETI public: Doppler? Date: Sat, 4 Jun 2005 23:56:20 -0700 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_0005_01C56961.01609C20" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: Microsoft Outlook Express 6.00.2800.1478 X-MimeOLE: Produced By Microsoft MimeOLE V6.00.2800.1478 X-AntiAbuse: This header was added to track abuse, please include it with any abuse report X-AntiAbuse: Primary Hostname - host224.ipowerweb.com X-AntiAbuse: Original Domain - seti1.setileague.org X-AntiAbuse: Originator/Caller UID/GID - [47 12] / [47 12] X-AntiAbuse: Sender Address Domain - seti.net X-Source: X-Source-Args: X-Source-Dir: Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_0005_01C56961.01609C20 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable Here is a sort of SETI question that I have been wondering about. In 2003 my wife and I were traveling around Newfoundland in our RV and = we camped next to a light house for the night. At about 2 AM the fog = rolled in and the light's fog horn came on (damn their loud). I = listened to it for a while and noticed that the initial note of the horn = was echoed by a note slightly higher in frequency. I don't have much of = an idea why the echo should be higher. If you would like to hear the horn click on the lighthouse picture at: http://www.seti.net/family/Motor%20Home%20Trips/Keep%20On%20Trekin/New_Be= ginning/Newfoundland/Western%20Region/Codroy/codroy.htm Its about 6 meg AVI file and a set of earphones helps to hear the echo. Any ideas about this??? Regards..... Jim Argus Station: DM12jb James Brown W6KYP Jim@SETI.Net [put 'SETI' in subject line] www.seti.net ------=_NextPart_000_0005_01C56961.01609C20 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
Here is a sort of SETI question that I = have been=20 wondering about.
 
In 2003 my wife and I were traveling = around=20 Newfoundland in our RV and we camped next to a light house for the = night. =20 At about 2 AM the fog rolled in and the light's fog horn came on (damn = their=20 loud).  I listened to it for a while and noticed that the initial = note of=20 the horn was echoed by a note slightly higher in frequency.  I = don't have=20 much of an idea why the echo should be higher.
If you would like to hear the horn = click on the=20 lighthouse picture at:
http://w= ww.seti.net/family/Motor%20Home%20Trips/Keep%20On%20Trekin/New_Beginning/= Newfoundland/Western%20Region/Codroy/codroy.htm
Its about 6 meg AVI file and a set of = earphones=20 helps to hear the echo.
 
Any ideas about this???
 
Regards..... Jim
 
Argus Station: DM12jb
James = Brown
W6KYP
Jim@SETI.Net [put 'SETI' in subject = line]
www.seti.net
------=_NextPart_000_0005_01C56961.01609C20-- From owner-public@setileague.org Mon Jun 6 06:26:41 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j56DQcUw012907 for ; Mon, 6 Jun 2005 06:26:40 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id JAA24920 for public-list; Mon, 6 Jun 2005 09:17:19 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f13.bay103.hotmail.com [65.54.174.23]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id JAA24916; Mon, 6 Jun 2005 09:17:16 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Mon, 6 Jun 2005 06:16:44 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Mon, 06 Jun 2005 13:16:44 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Young, Jupiter-Mass Objects in Ophiuchus Date: Mon, 06 Jun 2005 09:16:44 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 06 Jun 2005 13:16:44.0987 (UTC) FILETIME=[FC91A0B0:01C56A99] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506079 Date: Fri, 3 Jun 2005 15:52:29 GMT (132kb) Title: Young, Jupiter-Mass Objects in Ophiuchus Authors: K. N. Allers, D. T. Jaffe, N. S. van der Bliek, F. Allard, I. Baraffe Comments: 4 pages, 2 figures, to appear in the proceedings of "The Spitzer Space Telescope: New Views of the Cosmos" a meeting held 9-12 November 2004 \\ We have used 3.5 to 8 micron data from the Cores to Disks (c2d) Legacy survey and our own deep IJHKs images of a 0.5 square degree portion of the c2d fields in Ophiuchus to produce a sample of candidate young objects with probable masses between 1 and 10 Jupiter masses. The availability of photometry over whole range where these objects emit allows us to discriminate between young, extremely low-mass candidates and more massive foreground and background objects and means our survey will have fewer false positives than existing near-IR surveys. The sensitive inventory of a star forming cloud from the red to the mid-IR will allow us to constrain the IMF for these non-clustered star formation regions to well below the deuterium burning limit. For stars with fluxes in the broad gap between the 2MASS limits and our limits, our data will provide information about the photospheres. We will use the Spitzer results in combination with current disk models to learn about the presence and nature of circumstellar disks around young brown dwarfs. \\ ( http://arXiv.org/abs/astro-ph/0506079 , 132kb) From owner-public@setileague.org Mon Jun 6 08:48:32 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j56FmUUw012940 for ; Mon, 6 Jun 2005 08:48:31 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id LAA28517 for public-list; Mon, 6 Jun 2005 11:37:56 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f6.bay103.hotmail.com [65.54.174.16]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id LAA28497; Mon, 6 Jun 2005 11:37:15 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Mon, 6 Jun 2005 08:36:44 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Mon, 06 Jun 2005 15:36:43 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: bioastro@setileague.org Cc: public@setileague.org Subject: SETI public: FW: Cornell News: Study supports theory of quasars Date: Mon, 06 Jun 2005 11:36:43 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 06 Jun 2005 15:36:44.0108 (UTC) FILETIME=[8AD5C8C0:01C56AAD] Sender: owner-public@setileague.org Precedence: bulk >From: cunews@cornell.edu >Reply-To: cunews@cornell.edu >To: CUNEWS-PHYSICAL_SCIENCE-L@cornell.edu, CUNEWS-SCIENCE-L@cornell.edu >Subject: Cornell News: Study supports theory of quasars >Date: Mon, 6 Jun 2005 09:07:46 -0400 > >Cornell astronomers find key evidence supporting theory of quasars > >June 6, 2005 > >Contact: Lauren Gold >Phone: (607) 255-9736 >E-mail: lg34@cornell.edu > >Media Contact: Press Relations Office >Phone: (607) 255-6074 >E-mail: pressoffice@cornell.edu > >ITHACA, N.Y. -- The office that astronomer Lei Hao shares with her fellow >research associates on the first floor of the Space Sciences Building at >Cornell University is tidy and organized. But Hao has been thinking a lot >lately about dust. > >Actually, she's recently found a great deal of it. And she's thrilled. > >The dust in question is between 0.88 and 2.4 billion light years away from >Hao's office, in galaxies scientists classify as active galactic nuclei >(AGNs). By confirming that the dust exists, Hao and her team of researchers >from Cornell and several other institutions have given new weight to a >popular, but not universally accepted, theory of AGNs. Their new evidence >is published in the June 1 issue of Astrophysical Journal Letters (Vol. >625, pp. L75-L78). > >Since the early 1980s, the most widely accepted model of AGNs, called the >unified theory, involves a basic structure: a black hole at the center, an >accretion disc (a round, flat sheet of gas) around it and a doughnut-shaped >ring of dusty gas, called a torus, around the accretion disc. Jets of >matter are propelled out from the center perpendicular to the plane of the >accretion disc. > >The model holds that all AGNs share the same fundamental characteristics, >but it allows for different radiation patterns with the premise that how an >AGN looks depends on the perspective of the observer. An AGN viewed >face-on, classified as type 1, will show features from its central region; >an AGN viewed from the side (type 2) will have those features obscured by >the dusty torus. AGNs include quasars, which look like stars in optical >telescopes but emit massive amounts of radiation; Seyfert galaxies, >low-energy counterparts of quasars; and blazars, which are AGNs viewed >pole-on and which show rapid variations in radiation output over short >intervals. > >From an observational standpoint, the model has been largely successful. >But for years, a key piece of evidence has been missing. > >Astronomers can determine the composition and temperature of extragalactic >material by analyzing the way radiation passing through it is distributed >along an infrared spectrum. When radiation passes through silicate dust (a >fine, sandy substance common in interstellar dust), the dust grains absorb >it at specific wavelengths and leave dips in the infrared spectrum around >10 and 18 microns. > >When scientists observe type 2 AGNs, they recognize the silicate component >of the dusty torus by the telltale 10- and 18-micron absorption dips. But >in order for the unified theory to be correct, scientists looking down from >the top or up from below a type 1 AGN would expect to see excess radiation >from the silicate dust at 10 and 18 microns. They didn't -- and that >inconsistency led some to wonder if the theory was flawed. > >Hao's observations of silicate emission bands from type 1 AGNs are likely >to quell those doubts. > >In their paper, Hao and her colleagues describe five quasars (type 1 AGNs) >for which clear bumps in infrared emissions have been discovered at 10 and >18 microns. The measurements were taken by the Spitzer Space Telescope's >infrared spectrograph, which was developed by Cornell professor of >astronomy James Houck and is one of three instruments on the orbiting space >telescope. > >"People have been expecting this feature for a long time," says Hao. And it >has always been there, she adds, but nobody had recognized it until now -- >partly because the Spitzer's technology is more sensitive than earlier >versions and partly because other instruments didn't include a wide enough >spectral range to catch the 10 and 18 micron features. > >Finding evidence of dust may not seem important to non-astronomer types, >Hao allows. But she's not letting that dampen her enthusiasm. "For us it's >quite dramatic," she says. And by comparing the two emission bumps, >scientists can begin to learn even more about the AGNs. "The relative ratio >between the two features can give some information on the inner temperature >of the dusty torus," she says. Those calculations are just preliminary, but >finding long-sought evidence of the dust in the first place is enough to >make Hao grin. "You can see," she says, "that we verified the unification >model." > >Co-authors of the paper are Henrik Spoon, Gregory C. Sloan, J.A. Marshall, >Daniel Weedman, Vassilis Charmandaris and James Houck of Cornell; L. Armus >of the California Institute of Technology; A.G.G.M. Tielens of the >Netherlands' SRON National Institute for Space Research and Kapteyn >Institute; Benjamin A. Sargent of the University of Rochester; and Ilse M. >van Bemmel of Baltimore's Space Telescope Institute. > > >-30- > > >--Spitzer Space Telescope: >--Cornell's Department of Astronomy: >--James Houck: > > >-30- > >The web version of this story, with accompanying photos, is available at >http://www.news.cornell.edu/stories/June05/spitzer.quasars.hao.lg.html >-- > >Cornell University News Service >312 College Ave. >Ithaca, NY 14850 >607-255-4206 >cunews@cornell.edu >http://www.news.cornell.edu > From owner-public@setileague.org Tue Jun 7 07:44:42 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j57EicUw029334 for ; Tue, 7 Jun 2005 07:44:42 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id KAA02372 for public-list; Tue, 7 Jun 2005 10:32:01 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f14.bay103.hotmail.com [65.54.174.24]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id KAA02364; Tue, 7 Jun 2005 10:31:59 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Tue, 7 Jun 2005 07:31:28 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Tue, 07 Jun 2005 14:31:27 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Measurement of Spin-Orbit Alignment in an Extrasolar Planetary System Date: Tue, 07 Jun 2005 10:31:27 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 07 Jun 2005 14:31:28.0567 (UTC) FILETIME=[97676470:01C56B6D] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0504555 replaced with revised version Mon, 6 Jun 2005 02:47:46 GMT (742kb) Title: Measurement of Spin-Orbit Alignment in an Extrasolar Planetary System Authors: Joshua N. Winn, Robert W. Noyes, Matthew J. Holman, David Charbonneau, Yasuhiro Ohta, Atsushi Taruya, Yasushi Suto, Norio Narita, Edwin L. Turner, John A. Johnson, Geoffrey W. Marcy, R. Paul Butler, Steven S. Vogt Comments: 21 pages, 6 figures. To appear in ApJ [revised version includes calculation of tidal heating, other minor changes] \\ ( http://arXiv.org/abs/astro-ph/0504555 , 742kb) From owner-public@setileague.org Tue Jun 7 08:04:00 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j57F3xUw004216 for ; Tue, 7 Jun 2005 08:03:59 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id KAA03035 for public-list; Tue, 7 Jun 2005 10:53:21 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f41.bay103.hotmail.com [65.54.174.51]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id KAA03031; Tue, 7 Jun 2005 10:53:19 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Tue, 7 Jun 2005 07:52:48 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Tue, 07 Jun 2005 14:52:48 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org, fpspace@friends-partners.org Cc: bioastro@setileague.org Subject: SETI public: Galactic Gradients, Postbiological Evolution and the Apparent Failure of SETI Date: Tue, 07 Jun 2005 10:52:48 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 07 Jun 2005 14:52:48.0760 (UTC) FILETIME=[92755780:01C56B70] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506110 Date: Mon, 6 Jun 2005 14:10:44 GMT (77kb) Title: Galactic Gradients, Postbiological Evolution and the Apparent Failure of SETI Authors: Milan M. Cirkovic and Robert J. Bradbury Comments: 30 pages, 2 figures \\ Motivated by recent developments impacting our view of Fermi's paradox (absence of extraterrestrials and their manifestations from our past light cone), we suggest a reassessment of the problem itself, as well as of strategies employed by SETI projects so far. The need for such reevaluation is fueled not only by the failure of searches thus far, but also by great advances recently made in astrophysics, astrobiology, computer science and future studies, which have remained largely ignored in SETI practice. As an example of the new approach, we consider the effects of the observed metallicity and temperature gradients in the Milky Way on the spatial distribution of hypothetical advanced extraterrestrial intelligent communities. While, obviously, properties of such communities and their sociological and technological preferences are entirely unknown, we assume that (1) they operate in agreement with the known laws of physics, and (2) that at some point they typically become motivated by a meta-principle embodying the central role of information-processing; a prototype of the latter is the recently suggested Intelligence Principle of Steven J. Dick. There are specific conclusions of practical interest to be drawn from coupling of these reasonable assumptions with the astrophysical and astrochemical structure of the Galaxy. In particular, we suggest that the outer regions of the Galactic disk are most likely locations for advanced SETI targets, and that intelligent communities will tend to migrate outward through the Galaxy as their capacities of information-processing increase, for both thermodynamical and astrochemical reasons. This can also be regarded as a possible generalization of the Galactic Habitable Zone, concept currently much investigated in astrobiology. \\ ( http://arXiv.org/abs/astro-ph/0506110 , 78kb) From owner-public@setileague.org Tue Jun 7 08:41:24 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j57FfNUw014871 for ; Tue, 7 Jun 2005 08:41:24 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id LAA03903 for public-list; Tue, 7 Jun 2005 11:25:18 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from emperor.canarie.ca (emperor.canarie.ca [205.189.33.88]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id LAA03893; Tue, 7 Jun 2005 11:25:12 -0400 (EDT) Received: from localhost (emperor [127.0.0.1]) by emperor.canarie.ca (Postfix) with ESMTP id 26FED7750A; Tue, 7 Jun 2005 11:24:37 -0400 (EDT) Received: from emperor.canarie.ca ([127.0.0.1]) by localhost (emperor [127.0.0.1]) (amavisd-new, port 10024) with ESMTP id 16677-08; Tue, 7 Jun 2005 11:24:36 -0400 (EDT) Received: from amarillo (emperor.canarie.ca [205.189.33.88]) by emperor.canarie.ca (Postfix) with ESMTP id CFFB3774F4; Tue, 7 Jun 2005 11:24:36 -0400 (EDT) Reply-To: From: "Bill St.Arnaud" To: "'LARRY KLAES'" , , Cc: Subject: SETI public: Drake like equation on probablity of finding archelogical evidence of hominids on earth? Date: Tue, 7 Jun 2005 11:24:35 -0400 Message-ID: <00e201c56b75$03324920$1221bdcd@amarillo> MIME-Version: 1.0 Content-Type: text/plain; charset="us-ascii" X-Priority: 3 (Normal) X-MSMail-Priority: Normal X-Mailer: Microsoft Outlook, Build 10.0.6626 Importance: Normal In-Reply-To: X-MimeOLE: Produced By Microsoft MimeOLE V6.00.2900.2180 X-Virus-Scanned: by amavisd-new at canarie.ca Content-Transfer-Encoding: 8bit X-MIME-Autoconverted: from quoted-printable to 8bit by seti1.setileague.org id LAA03894 Sender: owner-public@setileague.org Precedence: bulk Has there ever been a Drake like equation on the probability of finding archeological evidence of past intelligent beings on earth e.g, hominids ? To my mind the search for hominids is similar to the search for ET. They both would be unaware of our modern day existence as we exist in their futures. So assuming they had no intent of directly sending a signal or message to us, we can only discover their existence through archeological techniques. Given that we only recognized that humans are part of the hominid tree in the last 100 years, and the first real evidence of hominids was only made 50 years ago, and most of the evidence is made up of small fragments of bone, teeth, stone tools, etc, after years of research and excavation, then one can only assume the search for ET will probably be considerably longer. The lack of evidence of ET so far would be comparable to saying there were no hominids, after spending 3 weeks digging up our back yard. Bill > -----Original Message----- > From: owner-public@setileague.org [mailto:owner-public@setileague.org] On > Behalf Of LARRY KLAES > Sent: Tuesday, June 07, 2005 10:53 AM > To: public@setileague.org; fpspace@friends-partners.org > Cc: bioastro@setileague.org > Subject: SETI public: Galactic Gradients, Postbiological Evolution and the > Apparent Failure of SETI > > Paper: astro-ph/0506110 > Date: Mon, 6 Jun 2005 14:10:44 GMT (77kb) > > Title: Galactic Gradients, Postbiological Evolution and the Apparent > Failure > of > SETI > > Authors: Milan M. Cirkovic and Robert J. Bradbury > Comments: 30 pages, 2 figures > \\ > > Motivated by recent developments impacting our view of Fermi's paradox > (absence of extraterrestrials and their manifestations from our past light > cone), we suggest a reassessment of the problem itself, as well as of > strategies employed by SETI projects so far. The need for such > reevaluation > is > fueled not only by the failure of searches thus far, but also by great > advances > recently made in astrophysics, astrobiology, computer science and future > studies, which have remained largely ignored in SETI practice. As an > example > of > the new approach, we consider the effects of the observed metallicity and > temperature gradients in the Milky Way on the spatial distribution of > hypothetical advanced extraterrestrial intelligent communities. While, > obviously, properties of such communities and their sociological and > technological preferences are entirely unknown, we assume that (1) they > operate > in agreement with the known laws of physics, and (2) that at some point > they > typically become motivated by a meta-principle embodying the central role > of > information-processing; a prototype of the latter is the recently > suggested > Intelligence Principle of Steven J. Dick. There are specific conclusions > of > practical interest to be drawn from coupling of these reasonable > assumptions > with the astrophysical and astrochemical structure of the Galaxy. In > particular, we suggest that the outer regions of the Galactic disk are > most > likely locations for advanced SETI targets, and that intelligent > communities > will tend to migrate outward through the Galaxy as their capacities of > information-processing increase, for both thermodynamical and > astrochemical > reasons. This can also be regarded as a possible generalization of the > Galactic > Habitable Zone, concept currently much investigated in astrobiology. > > \\ ( http://arXiv.org/abs/astro-ph/0506110 , 78kb) From owner-public@setileague.org Wed Jun 8 06:18:23 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j58DIMUw001957 for ; Wed, 8 Jun 2005 06:18:23 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id JAA06096 for public-list; Wed, 8 Jun 2005 09:07:54 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f11.bay103.hotmail.com [65.54.174.21]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id JAA06092; Wed, 8 Jun 2005 09:07:51 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 8 Jun 2005 06:07:20 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Wed, 08 Jun 2005 13:07:20 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: FW: Marsbugs Vol. 12, No. 19 Date: Wed, 08 Jun 2005 09:07:20 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 08 Jun 2005 13:07:20.0890 (UTC) FILETIME=[012AC1A0:01C56C2B] Sender: owner-public@setileague.org Precedence: bulk >From: "Dr. David J. Thomas" >To: "Dr. David J. Thomas" >Subject: Marsbugs Vol. 12, No. 19 >Date: Tue, 7 Jun 2005 16:19:49 -0500 > >The 7 June 2005 issue of Marsbugs: The Electronic Astrobiology >Newsletter is online. >Text: http://www.lyon.edu/projects/marsbugs/2005/20050607.txt >PDF: http://www.lyon.edu/projects/marsbugs/2005/20050607.pdf >Word: http://www.lyon.edu/projects/marsbugs/2005/20050607.doc > >Articles and News > >Page 2 SIGNIFICANT RUNOFF ON EARLY MARS IDENTIFIED IN RIVER CHANNELS >BY NATIONAL AIR AND SPACE MUSEUM GEOLOGISTS >National Air and Space Museum release > >Page 2 TOP 10 WAYS TO DESTROY EARTH >By Sam Hughs > >Page 3 TITAN'S FACE LIFTED >By Leslie Mullen > >Page 4 NEW UNDERWATER VOLCANO FOUND NEAR SAMOA >Woods Hole Oceanographic Institute release > >Page 5 EXTRATERRESTRIAL: IMAGINING OTHER WORLDS >By Edna DeVore > >Page 5 APPROACHING MARS >By Tony Phillips > >Page 6 MARS: WINDOWS ON THE WORLD >By Joy Crisp > >Page 8 BOMBING THE COMET >From Astrobiology Magazine > >Page 8 MOST AMERICANS BELIEVE ALIEN LIFE IS POSSIBLE, STUDY SHOWS >By Tariq Malik > >Page 8 SPIRIT, THE PROBLEM CHILD >By Joy Crisp > >Page 9 COMET PUT ON LIST OF POTENTIAL EARTH IMPACTORS >From New Scientist > >Page 9 FUNDING FOR MOON, MARS PROJECTS PROMISED >By Pam Easton > >Page 9 SCRIPPS-LED GLOBAL OCEAN WARMING RESEARCH PAPER PUBLISHED IN >SCIENCE EXPRESS >Scripps Institution of Oceanography release > >Page 10 THE CENTER FOR THE STUDY OF LIFE IN THE UNIVERSE >By Frank Drake > >Page 10 NASA SCIENTISTS CONFIRM LIQUID WATER ON EARLY EARTH >NASA/ARC release 05-35 > >Page 10 NASA NAPS >By Patrick L. Barry and Tony Phillips > >Page 11 DRIVING ON THE ROADMAP >From Astrobiology Magazine > >Page 12 OPPORTUNITY'S ESCAPE FROM DUNE >By Joy Crisp > >Announcements > >Page 13 GRIFFIN SUPPORTS ISRU >Mars Society release > >Page 13 BOOK PREVIEW: SEEDING THE UNIVERSE WITH LIFE-SECURING OUR >COSMOLOGICAL FUTURE >By Michael Mautner > >Page 14 ABSTRACT DEADLINE EXTENDED FOR MARS SOCIETY CONVENTION >Mars Society release > >Mission Reports > >Page 14 CASSINI UPDATES >Multiple agencies' releases > >Page 18 NASA'S SPACE EYES FOCUS ON DEEP IMPACT TARGET >NASA release 05-139 > >Page 19 HOW TO WATCH JULY 4 COMET IMPACT >By Joe Rao > >Page 19 MER UPDATES >NASA/JPL releases > >Page 20 MARS EXPRESS: ANCIENT FLOODS ON MARS >ESA release > >Page 22 MARS GLOBAL SURVEYOR IMAGES >NASA/JPL/MSSS releases > >Page 22 MARS ODYSSEY THEMIS IMAGES >NASA/JPL/ASU releases > >Page 22 NASA'S PHOENIX MARS MISSION BEGINS LAUNCH PREPARATIONS >NASA release 05-141 > >David J. Thomas, PhD >Assoc. Professor of Biology >Lyon College, Science Division >2300 Highland Road >Batesville, AR 72501 USA >Phone: 870-698-4269 >Fax: 870-698-4692 >http://www.lyon.edu/webdata/users/dthomas > >NASA/JPL Solar System Ambassador >http://www2.jpl.nasa.gov/ambassador >Editor of Marsbugs: The Electronic Astrobiology Newsletter >http://www.lyon.edu/projects/marsbugs > > From owner-public@setileague.org Wed Jun 8 06:32:54 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j58DWpUw010239 for ; Wed, 8 Jun 2005 06:32:52 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id JAA06489 for public-list; Wed, 8 Jun 2005 09:22:49 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f29.bay103.hotmail.com [65.54.174.39]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id JAA06479; Wed, 8 Jun 2005 09:22:37 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 8 Jun 2005 06:22:06 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Wed, 08 Jun 2005 13:22:06 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: bioastro@setileague.org Cc: public@setileague.org Subject: SETI public: Oliviine weathering may be the culprit for the Mars Methane Date: Wed, 08 Jun 2005 09:22:06 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 08 Jun 2005 13:22:06.0756 (UTC) FILETIME=[112F2E40:01C56C2D] Sender: owner-public@setileague.org Precedence: bulk http://www.dartmouth.edu/~news/releases/2005/06/07a.html In their paper published online in May in the American Geophysical Union's journal, Geophysical Research Letters, Sharma and Oze describe how methane on Mars can be made from abiotic, or non-living, sources. When water containing dissolved carbon dioxide comes in contact with olivine, it produces hydrogen, which then combines with carbon dioxide to produce methane. The authors contend that olivine is abundant on Mars at shallow depths, and it could easily react with fluids just beneath the surface. "Most methane on Earth is produced by bacteria, and methane has been cited as an indicator of life on other planets," explains Sharma. "However, we show in our paper that the mineral olivine can be altered in the presence of water and carbon dioxide, which can produce copious quantities of methane. It's quite easy to do, and there is nothing bacterial about it. If there is life on Mars, I would like to see better evidence than methane." From owner-public@setileague.org Wed Jun 8 10:24:42 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j58HOcUw030846 for ; Wed, 8 Jun 2005 10:24:41 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id NAA12550 for public-list; Wed, 8 Jun 2005 13:14:55 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f42.bay103.hotmail.com [65.54.174.52]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id NAA12544; Wed, 8 Jun 2005 13:14:53 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 8 Jun 2005 10:14:18 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Wed, 08 Jun 2005 17:14:17 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Self-Sustained Ionization and Vanishing Dead Zones in Protoplanetary Disks Date: Wed, 08 Jun 2005 13:14:17 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 08 Jun 2005 17:14:18.0096 (UTC) FILETIME=[80E8F700:01C56C4D] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506131 Date: Tue, 7 Jun 2005 03:49:45 GMT (57kb) Title: Self-Sustained Ionization and Vanishing Dead Zones in Protoplanetary Disks Authors: Shu-ichiro Inutsuka, Takayoshi Sano Comments: 10 pages, 2 figures \\ We analyse the ionization state of the magnetohydrodynamically turbulent protoplanetary disks and propose a new mechanism of sustaining ionization. First, we show that in the quasi-steady state of turbulence driven by magnetorotational instability in a typical protoplanetary disk with dust grains the amount of energy dissipation should be sufficient for providing the ionization energy that is required for activating magnetorotational instability. Second, we show that in the disk with dust grains the energetic electrons in weakly ionized gas can provide collisional ionization, depending upon the actual saturation state of magnetorotational turbulence. Finally, we show that in the protoplanetary disks with the reduced effect of dust grains, the turbulent motion can homogenize the ionization degree, which can solely activate magnetorotational instability. The results in this letter indicate that the most of the regions in protoplanetary disks remain magnetically active, thus, require a change in theoretical modeling of planet formation. \\ ( http://arXiv.org/abs/astro-ph/0506131 , 57kb) From owner-public@setileague.org Wed Jun 8 13:25:28 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j58KPQUw020371 for ; Wed, 8 Jun 2005 13:25:28 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id QAA17493 for public-list; Wed, 8 Jun 2005 16:17:29 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f24.bay103.hotmail.com [65.54.174.34]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id QAA17489; Wed, 8 Jun 2005 16:17:25 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 8 Jun 2005 13:16:54 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Wed, 08 Jun 2005 20:16:53 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org, fpspace@friends-partners.org Subject: SETI public: FW: Scientists Discover Possible Titan Volcano Date: Wed, 08 Jun 2005 16:16:53 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 08 Jun 2005 20:16:54.0548 (UTC) FILETIME=[0376DD40:01C56C67] Sender: owner-public@setileague.org Precedence: bulk >From: "NASA Jet Propulsion Laboratory" >Reply-To: >To: "Larry Klaes" >Subject: Scientists Discover Possible Titan Volcano >Date: Wed, 08 Jun 2005 12:41:05 -0700 > >MEDIA RELATIONS OFFICE >JET PROPULSION LABORATORY >CALIFORNIA INSTITUTE OF TECHNOLOGY >NATIONAL AERONAUTICS AND SPACE ADMINISTRATION >PASADENA, CALIF. 91109 TELEPHONE (818) 354-5011 >http://www.jpl.nasa.gov > >Carolina Martinez (818) 354-9382 >Jet Propulsion Laboratory, Pasadena, Calif. > >News Release: 2005-096 June 8, 2005 > >Scientists Discover Possible Titan Volcano > >A recent flyby of Saturn's hazy moon Titan by the Cassini spacecraft has >revealed >evidence of a possible volcano, which could be a source of methane in >Titan's >atmosphere. > >Images taken in infrared light show a circular feature roughly 30 >kilometers (19 miles) in >diameter that does not resemble any features seen on Saturn's other icy >moons. >Scientists interpret the feature as an "ice volcano," a dome formed by >upwelling icy >plumes that release methane into Titan's atmosphere. The findings appear >in the June >9 issue of Nature. > >"Before Cassini-Huygens, the most widely accepted explanation for the >presence of >methane in Titan's atmosphere was the presence of a methane-rich >hydrocarbon >ocean," said Dr. Christophe Sotin, distinguished visiting scientist at >NASA's Jet >Propulsion Laboratory, Pasadena, Calif. > >"The suite of instruments onboard Cassini and the observations at the >Huygens landing >site reveal that a global ocean is not present," said Sotin, a team member >of the Cassini >visual and infrared mapping spectrometer instrument and professor at the >Université de >Nantes, France. > >"Interpreting this feature as a cryovolcano provides an alternative >explanation for the >presence of methane in Titan's atmosphere. Such an interpretation is >supported by >models of Titan's evolution," Sotin said. > >Titan, Saturn's largest moon, is the only known moon to have a significant >atmosphere, >composed primarily of nitrogen, with 2 to 3 percent methane. One goal of >the Cassini >mission is to find an explanation for what is replenishing and maintaining >this >atmosphere. This dense atmosphere makes the surface very difficult to >study with >visible-light cameras, but infrared instruments like the visual and >infrared mapping >spectrometer can peer through the haze. Infrared images provide >information about >both the composition and the shape of the area studied. > >The highest resolution image obtained by the visual and infrared mapping >spectrometer >instrument covers an area 150 kilometers square (90 miles) that includes a >bright >circular feature about 30 kilometers (19 miles) in diameter, with two >elongated wings >extending westward. This structure resembles volcanoes on Earth and Venus, >with >overlapping layers of material from a series of flows. > >"We all thought volcanoes had to exist on Titan, and now we've found the >most >convincing evidence to date. This is exactly what we've been looking for," >said Dr. >Bonnie Buratti, team member of the Cassini visual and infrared mapping >spectrometer >at JPL. > >In the center of the area, scientists clearly see a dark feature that >resembles a caldera, >a bowl-shaped structure formed above chambers of molten material. The >material >erupting from the volcano might be a methane-water ice mixture combined >with other >ices and hydrocarbons. Energy from an internal heat source may cause these >materials >to upwell and vaporize as they reach the surface. Future Titan flybys will >help >determine whether tidal forces can generate enough heat to drive the >volcano, or >whether some other energy source must be present. Black channels seen by >the >European Space Agency's Huygens probe, which piggybacked on Cassini and >landed >on Titan's surface in January 2005, could have been formed by erosion from >liquid >methane rains following the eruptions. > >Scientists have considered other explanations. They say the feature cannot >be a cloud >because it does not appear to move and it is the wrong composition. >Another >alternative is that an accumulation of solid particles was transported by >gas or liquid, >similar to sand dunes on Earth. But the shape and wind patterns don't >match those >normally seen in sand dunes. > >The data for these findings are from Cassini's first targeted flyby of >Titan on Oct. 26, >2004, at a distance of 1,200 kilometers (750 miles) from the moon's >surface. > >The visual and infrared mapping spectrometer instrument can detect 352 >wavelengths >of light from 0.35 to 5.1 micrometers. It measures the intensities of >individual >wavelengths and uses the data to infer the composition and other properties >of the >object that emitted the light; each chemical has a unique spectral >signature that can be >identified. > >Forty-five flybys of Titan are planned during Cassini's four-year prime >mission. The next >one is Aug. 22, 2005. Radar data of the same sites observed by the visual >and infrared >mapping spectrometer may provide additional information. > >For more information about the Cassini-Huygens mission visit >http://saturn.jpl.nasa.gov >and http://www.nasa.gov/cassini . The visual and infrared mapping >spectrometer page >is at http://wwwvims.lpl.arizona.edu . > >The Cassini-Huygens mission is a cooperative project of NASA, the European >Space >Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a >division of the >California Institute of Technology in Pasadena, manages the mission for >NASA's >Science Mission Directorate, Washington, D.C. The Cassini orbiter was >designed, >developed and assembled at JPL. The visual and infrared mapping >spectrometer team >is based at the University of Arizona. > >-end- > > > From owner-public@setileague.org Wed Jun 8 14:21:37 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j58LLaUw014268 for ; Wed, 8 Jun 2005 14:21:37 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id RAA18883 for public-list; Wed, 8 Jun 2005 17:13:22 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f12.bay103.hotmail.com [65.54.174.22]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id RAA18879; Wed, 8 Jun 2005 17:13:20 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 8 Jun 2005 14:12:49 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Wed, 08 Jun 2005 21:12:48 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Three papers on circumstellar protoplanetary disks Date: Wed, 08 Jun 2005 17:12:48 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 08 Jun 2005 21:12:49.0424 (UTC) FILETIME=[D3205100:01C56C6E] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506132 Date: Tue, 7 Jun 2005 07:23:20 GMT (260kb) Title: Where Are The M Dwarf Disks Older Than 10 Million Years? Authors: Peter Plavchan, M. Jura, & S. J. Lipscy Comments: 24 pages, 2 figures, accepted to ApJ \\ We present 11.7-micron observations of nine late-type dwarfs obtained at the Keck I 10-meter telescope in December 2002 and April 2003. Our targets were selected for their youth or apparent IRAS 12-micron excess. For all nine sources, excess infrared emission is not detected. We find that stellar wind drag can dominate the circumstellar grain removal and plausibly explain the dearth of M Dwarf systems older than 10 Myr with currently detected infrared excesses. We predict M dwarfs possess fractional infrared excess on the order of L_{IR}/L_{*}\sim10^{-6} and this may be detectable with future efforts. \\ ( http://arXiv.org/abs/astro-ph/0506132 , 260kb) Paper: astro-ph/0506134 Date: Tue, 7 Jun 2005 08:33:35 GMT (344kb) Title: Bright X-ray flares in Orion young stars from COUP: evidence for star-disk magnetic fields? Authors: F. Favata, E. Flaccomio, F. Reale, G. Micela, S. Sciortino, H. Shang, K. Stassun, E.D. Feigelson Comments: Accepted to ApJS, COUP special issue \\ We have analyzed a number of intense X-ray flares observed in the Chandra Orion Ultradeep Project (COUP), a 13 days observation of the Orion Nebula Cluster (ONC). Analysis of the flare decay allows to determine the size, peak density and magnetic field of the flaring structure. A total of 32 events (the most powerful 1% of COUP flares), have sufficient statistics for the analysis. A broad range of decay times (from 10 to 400 ks) are present in the sample. Peak flare temperatures are often very high, with half of the flares in the sample showing temperatures in excess of 100 MK. Significant sustained heating is present in the majority of the flares. The magnetic structures which are found, are in a number of cases very long, with semi-lengths up to 10^12 cm, implying the presence of magnetic fields of hundreds of G extending to comparable distance from the stellar photosphere. These very large sizes for the flaring structures ($ >> R_*) are not found in more evolved stars, where, almost invariably, the same type of analysis results in structures with L <= R_*. As the majority of young stars in the ONC are surrounded by disks, we speculate that the large magnetic structures which confine the flaring plasma are actually the same type of structures which channel the plasma in the magnetospheric accretion paradigm, connecting the star's photosphere with the accretion disk. \\ ( http://arXiv.org/abs/astro-ph/0506134 , 344kb) Paper: astro-ph/0506147 Date: Tue, 7 Jun 2005 18:00:28 GMT (19kb) Title: Jupiter's Obliquity and a Long-lived Circumplanetary Disk Authors: I. Mosqueira and P. R. Estrada Comments: 8 pages, 1 figure. Submitted note to Icarus \\ It has been claimed (Canup and Ward 2002; Ward 2003) that a long-lived massive (compared to the mass of the Galilean satellites) circumplanetary gas disk is inconsistent with Jupiter's low obliquity. Such a constraint could be downplayed on the basis that it deals with a single observation. Here we argue that this argument is flawed because it assumes a solar system much like that of the present day with the one exception of a circumjovian disk which is then allowed to dissipate on a long timescale (10^6-10^7 yrs). Given that the sequence of events in solar-system history that fit known constraints is non-unique, we choose for the sake of clarity of exposition the orbital architecture framework of Tsiganis et al. (2005), in which Jupiter and Saturn were once in closer, less inclined orbits than they are at present, and show that Jupiter's low obliquity is consistent with the SEMM (solids-enhanced minimum mass) satellite formation model of Mosqueira and Estrada (2003a,b). \\ ( http://arXiv.org/abs/astro-ph/0506147 , 19kb) From owner-public@setileague.org Thu Jun 9 03:47:37 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j59AlaUw002507 for ; Thu, 9 Jun 2005 03:47:36 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id GAA08744 for public-list; Thu, 9 Jun 2005 06:40:00 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-dav7.bay103.hotmail.com [65.54.174.79]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id GAA08725; Thu, 9 Jun 2005 06:39:56 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 9 Jun 2005 03:39:25 -0700 Message-ID: Received: from 65.54.174.209 by BAY103-DAV7.phx.gbl with DAV; Thu, 09 Jun 2005 10:39:24 +0000 X-Originating-IP: [65.54.174.209] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: Report by the ESA-ESO Working Group on Extra-Solar Planets Date: Thu, 9 Jun 2005 06:39:22 -0400 MIME-Version: 1.0 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: 7bit X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 X-RFC2646: Format=Flowed; Original Seal-Send-Time: Thu, 9 Jun 2005 06:39:22 -0400 X-OriginalArrivalTime: 09 Jun 2005 10:39:25.0287 (UTC) FILETIME=[814EF770:01C56CDF] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506163 Date: Wed, 8 Jun 2005 08:57:18 GMT (266kb) Title: Report by the ESA-ESO Working Group on Extra-Solar Planets Authors: M. Perryman, O. Hainaut, D. Dravins, A. Leger, A. Quirrenbach, H. Rauer, F. Kerber, R. Fosbury, F. Bouchy, F. Favata, M. Fridlund, R. Gilmozzi, A.-M. Lagrange, T. Mazeh, D. Rouan, S. Udry, J. Wambsganss Comments: ESA-ESO Working Groups Report No. 1, 92 pages, 7 figures, a pdf version including the cover pages is available from ESO and ESA websites: http://www.eso.org/gen-fac/pubs/esaesowg/ http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=36935 A printed version (A5 booklet) is available in limited numbers from Space Telescope-European Coordinating Facility (ST-ECF) on request: stdesk@eso.org \\ Various techniques are being used to search for extra-solar planetary signatures, including accurate measurement of radial velocity and positional (astrometric) displacements, gravitational microlensing, and photometric transits. Planned space experiments promise a considerable increase in the detections and statistical knowledge arising especially from transit and astrometric measurements over the years 2005-15, with some hundreds of terrestrial-type planets expected from transit measurements, and many thousands of Jupiter-mass planets expected from astrometric measurements. Beyond 2015, very ambitious space (Darwin/TPF) and ground (OWL) experiments are targeting direct detection of nearby Earth-mass planets in the habitable zone and the measurement of their spectral characteristics. Beyond these, `Life Finder' (aiming to produce confirmatory evidence of the presence of life) and `Earth Imager' (some massive interferometric array providing resolved images of a distant Earth) appear as distant visions. This report, to ESA and ESO, summarises the direction of exo-planet research that can be expected over the next 10 years or so, identifies the roles of the major facilities of the two organisations in the field, and concludes with some recommendations which may assist development of the field. The report has been compiled by the Working Group members and experts over the period June-December 2004. \\ ( http://arXiv.org/abs/astro-ph/0506163 , 266kb) From owner-public@setileague.org Thu Jun 9 03:49:42 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j59AnfUw009068 for ; Thu, 9 Jun 2005 03:49:41 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id GAA08837 for public-list; Thu, 9 Jun 2005 06:43:20 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-dav3.bay103.hotmail.com [65.54.174.75]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id GAA08833; Thu, 9 Jun 2005 06:43:18 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 9 Jun 2005 03:42:46 -0700 Message-ID: Received: from 65.54.174.209 by BAY103-DAV3.phx.gbl with DAV; Thu, 09 Jun 2005 10:42:46 +0000 X-Originating-IP: [65.54.174.209] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: Near infrared and the inner regions of protoplanetary disks Date: Thu, 9 Jun 2005 06:42:43 -0400 MIME-Version: 1.0 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: 7bit X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 X-RFC2646: Format=Flowed; Original Seal-Send-Time: Thu, 9 Jun 2005 06:42:43 -0400 X-OriginalArrivalTime: 09 Jun 2005 10:42:46.0964 (UTC) FILETIME=[F9846F40:01C56CDF] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506154 Date: Tue, 7 Jun 2005 22:01:39 GMT (193kb) Title: Near infrared and the inner regions of protoplanetary disks Authors: Dejan Vinkovic, Zeljko Ivezic, Tomislav Jurkic and Moshe Elitzur Comments: 14 pages, 10 figures, submitted to ApJ \\ We examine the ``puffed-up inner disk'' model (Dullemond, Dominik & Natta 2001), proposed for explaining the near-IR excess radiation from Herbig Ae/Be stars. Detailed model re-computations and comparison with the observed distribution of near-IR excess show that the model requires fine tuning of free parameters. In particular, only perfectly gray dust opacity can produce the observed near-IR excess, yet such dust is in conflict with the observed 10$\mu$m spectral feature. We find that an alternative model consisting of a compact ($\sim$ 10 AU) tenuous dusty halo around the disk inner regions readily explains the observed near-IR excess. Furthermore, this model also resolves the puzzling relationship noted by Monnier and Millan-Gabet (2002) between luminosity and the interferometric inner radii of disks. \\ ( http://arXiv.org/abs/astro-ph/0506154 , 193kb) From owner-public@setileague.org Thu Jun 9 03:50:09 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j59Ao8Uw025862 for ; Thu, 9 Jun 2005 03:50:08 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id GAA08806 for public-list; Thu, 9 Jun 2005 06:42:06 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-dav13.bay103.hotmail.com [65.54.174.85]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id GAA08802; Thu, 9 Jun 2005 06:42:04 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 9 Jun 2005 03:41:33 -0700 Message-ID: Received: from 65.54.174.209 by BAY103-DAV13.phx.gbl with DAV; Thu, 09 Jun 2005 10:41:32 +0000 X-Originating-IP: [65.54.174.209] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: 4,131 stars within 33 parsecs of Sol Date: Thu, 9 Jun 2005 06:41:30 -0400 MIME-Version: 1.0 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: 7bit X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 X-RFC2646: Format=Flowed; Original Seal-Send-Time: Thu, 9 Jun 2005 06:41:30 -0400 X-OriginalArrivalTime: 09 Jun 2005 10:41:33.0406 (UTC) FILETIME=[CDAC5FE0:01C56CDF] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506152 Date: Tue, 7 Jun 2005 20:43:27 GMT (762kb) Title: Nearby stars from the LSPM-north Proper Motion Catalog. I. Main Sequence Dwarfs and Giants Within 33 Parsecs of the Sun Authors: Sebastien Lepine Comments: 13 pages, accepted for publication in the Astronomical Journal \\ A list of 4,131 dwarfs, subgiants, and giants located, or suspected to be located, within 33 parsecs of the Sun is presented. All the stars are drawn from the new LSPM-north catalog of 61,976 stars with annual proper motions larger than 0.15''/yr$. Trigonometric parallax measurements are found in the literature for 1,676 of the stars in the sample; photometric and spectroscopic distance moduli are found for another 783 objects. The remaining 1,672 objects are reported here as nearby star candidates for the first time. Photometric distance moduli are calculated for the new stars based on the (M_V,V-J) relationship, calibrated with the subsample of stars which have trigonometric parallaxes. The list of new candidates includes 539 stars which are suspected to be within 25 parsecs of the Sun, including 63 stars estimated to be within only 15 parsecs. The current completeness of the census of nearby stars in the northern sky is discussed in light of the new candidates presented here. It is estimated that 32% (18%) of nuclear burning stars within 33 parsecs (25 parsecs) of the Sun remain to be located. The missing systems are expected to have proper motions below the 0.15''/yr limit of the LSPM catalog. \\ ( http://arXiv.org/abs/astro-ph/0506152 , 762kb) From owner-public@setileague.org Thu Jun 9 03:57:29 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j59AvRUw001683 for ; Thu, 9 Jun 2005 03:57:28 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id GAA09012 for public-list; Thu, 9 Jun 2005 06:45:46 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-dav15.bay103.hotmail.com [65.54.174.87]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id GAA09007; Thu, 9 Jun 2005 06:45:44 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 9 Jun 2005 03:45:13 -0700 Message-ID: Received: from 65.54.174.209 by BAY103-DAV15.phx.gbl with DAV; Thu, 09 Jun 2005 10:45:12 +0000 X-Originating-IP: [65.54.174.209] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: A Candidate Neutron Star Associated with Galactic Center Supernova Remnant Sagittarius A East Date: Thu, 9 Jun 2005 06:45:10 -0400 MIME-Version: 1.0 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: 7bit X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 X-RFC2646: Format=Flowed; Original Seal-Send-Time: Thu, 9 Jun 2005 06:45:10 -0400 X-OriginalArrivalTime: 09 Jun 2005 10:45:13.0143 (UTC) FILETIME=[50A59470:01C56CE0] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506168 Date: Wed, 8 Jun 2005 13:45:44 GMT (757kb) Title: A Candidate Neutron Star Associated with Galactic Center Supernova Remnant Sagittarius A East Authors: Sangwook Park (Penn State), Michael P. Muno (UCLA), Frederick K. Baganoff (MIT), Yoshitomo Maeda (ISAS), Mark Morris (UCLA), George Chartas (Penn State), Divas Sanwal (Penn State), David N. Burrows (Penn State), and Gordon P. Garmire (Penn State) Comments: ApJ preprint style 28 pages, 1 color fig (fig1), Accepted by ApJ \\ We present imaging and spectral studies of the supernova remnant (SNR) Sagittarius (Sgr) A East from deep observations with the {\it Chandra X-Ray Observatory}. The spatially-resolved spectral analysis of Sgr A East reveals the presence of a two-temperature thermal plasma ($kT$ $\sim$ 1 keV and 5 keV) near the center of the SNR. The central region is dominated by emission from highly-ionized Fe-rich ejecta. We estimate a conservative upper limit on the total Fe ejecta mass of the SNR, M$_{Fe}$ $<$ 0.27 M$_{\odot}$. Comparisons with standard SN nucleosynthesis models suggest that this Fe mass limit is consistent with a Type II SN explosion for the origin of Sgr A East. On the other hand, the soft X-ray emission extending toward the north of the SNR can be described by a single-temperature ($kT$ $\sim$ 1.3 keV) thermal plasma with normal chemical composition. This portion of the SNR is thus X-ray emission from the heated interstellar medium rather than the metal-rich stellar ejecta. We point out that a hard pointlike source CXOGC J174545.5$-$285829 (the so-called ``cannonball'') at the northern edge of the SNR shows unusual X-ray characteristics among other Galactic center sources. The morphological, spectral, and temporal characteristics of this source suggest an identification as a high-velocity neutron star. Based on the suggested Type II origin for the SNR Sgr A East and the proximity between the two, we propose that CXOGC J174545.5$-$285829 is a high-velocity neutron star candidate, born from the core-collapse SN which also created the SNR Sgr A East. \\ ( http://arXiv.org/abs/astro-ph/0506168 , 757kb) From owner-public@setileague.org Thu Jun 9 12:17:52 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j59JHnUw027282 for ; Thu, 9 Jun 2005 12:17:52 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id PAA21704 for public-list; Thu, 9 Jun 2005 15:08:33 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f40.bay103.hotmail.com [65.54.174.50]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id PAA21699; Thu, 9 Jun 2005 15:08:30 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 9 Jun 2005 12:07:59 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Thu, 09 Jun 2005 19:07:58 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: The "Star Wars" Worlds: More Science Than Fiction? Date: Thu, 09 Jun 2005 15:07:58 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 09 Jun 2005 19:07:59.0765 (UTC) FILETIME=[8D5ACC50:01C56D26] Sender: owner-public@setileague.org Precedence: bulk The "Star Wars" Worlds: More Science Than Fiction? http://news.nationalgeographic.com/news/2005/06/0603_050603_starwars.html From owner-public@setileague.org Fri Jun 10 08:41:09 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5AFf7Uw018337 for ; Fri, 10 Jun 2005 08:41:08 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id LAA21840 for public-list; Fri, 10 Jun 2005 11:30:00 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f34.bay103.hotmail.com [65.54.174.44]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id LAA21836; Fri, 10 Jun 2005 11:29:57 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 10 Jun 2005 08:29:26 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Fri, 10 Jun 2005 15:29:25 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective Date: Fri, 10 Jun 2005 11:29:25 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 10 Jun 2005 15:29:26.0198 (UTC) FILETIME=[2F790560:01C56DD1] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506187 Date: Wed, 8 Jun 2005 22:53:56 GMT (259kb) Title: Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective Authors: Sean M. Andrews & Jonathan P. Williams (University of Hawaii Institute for Astronomy) Comments: accepted by ApJ \\ We present a sensitive, multiwavelength submillimeter continuum survey of 153 young stellar objects in the Taurus-Auriga star formation region. The submillimeter detection rate is 61% to a completeness limit of ~10 mJy (3-sigma) at 850 microns. The inferred circumstellar disk masses are log-normally distributed with a mean mass of ~0.005 solar masses and a large dispersion (0.5 dex). Roughly one third of the submillimeter sources have disk masses larger than the minimal nebula from which the solar system formed. The median disk to star mass ratio is 0.5%. The empirical behavior of the submillimeter continuum is best described as F_nu ~ nu^(2.0 +/- 0.5) between 350 microns and 1.3 mm, which we argue is due to the combined effects of the fraction of optically thick emission and a flatter frequency behavior of the opacity compared to the ISM. This latter effect could be due to a substantial population of large dust grains, which presumably would have grown through collisional agglomeration. In this sample, the only stellar property that is correlated with the outer disk is the presence of a companion. We find evidence for significant decreases in submillimeter flux densities, disk masses, and submillimeter continuum slopes along the canonical infrared spectral energy distribution evolution sequence for young stellar objects. The fraction of objects detected in the submillimeter is essentially identical to the fraction with excess near-infrared emission, suggesting that dust in the inner and outer disk are removed nearly simultaneously. \\ ( http://arXiv.org/abs/astro-ph/0506187 , 259kb) From owner-public@setileague.org Fri Jun 10 08:51:38 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5AFpaUw015630 for ; Fri, 10 Jun 2005 08:51:37 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id LAA22286 for public-list; Fri, 10 Jun 2005 11:44:16 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f27.bay103.hotmail.com [65.54.174.37]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id LAA22263; Fri, 10 Jun 2005 11:44:12 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 10 Jun 2005 08:43:41 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Fri, 10 Jun 2005 15:43:40 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Systematic Analysis of 22 Microlensing Parallax Candidates Date: Fri, 10 Jun 2005 11:43:40 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 10 Jun 2005 15:43:41.0469 (UTC) FILETIME=[2D4104D0:01C56DD3] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506183 Date: Thu, 9 Jun 2005 19:16:03 GMT (140kb) Title: Systematic Analysis of 22 Microlensing Parallax Candidates Authors: Shawn Poindexter (1), Cristina Afonso (2), David P. Bennett (3), Jean-Francois Glicenstein (4), Andrew Gould (1), Michal K. Szymanski (5), and Andrzej Udalski (5) ((1) Ohio State, (2) Max-Planck fuer Astronomie, (3) Notre Dame, (4) CEA Saclay, (5) Warsaw University Observatory) Comments: 69 Pages, 10 Figures, 24 Tables, Submitted to ApJ \\ We attempt to identify all microlensing parallax events for which the parallax fit improves \Delta\chi^2 > 100 relative to a standard microlensing model. We outline a procedure to identify three types of discrete degeneracies (including a new one that we dub the ``ecliptic degeneracy'') and find many new degenerate solutions in 16 previously published and 6 unpublished events. Only four events have one unique solution and the other 18 events have a total of 44 solutions. Our sample includes three previously identified black-hole (BH) candidates. We consider the newly discovered degenerate solutions and determine the relative likelihood that each of these is a BH. We find the lens of event MACHO-99-BLG-22 is a strong BH candidate (78%), event MACHO-96-BLG-5 is a marginal BH candidate (37%), and MACHO-98-BLG-6 is a weak BH candidate (2.2%). The lens of event OGLE-2003-BLG-84 may be a Jupiter-mass free-floating planet candidate based on a weak 3 sigma detection of finite-source effects. We find that event MACHO-179-A is a brown dwarf candidate within ~100 pc of the Sun, mostly due to its very small projected Einstein radius, \tilde r_E = 0.23+-0.05 AU. As expected, these microlensing parallax events are biased toward lenses that are heavier and closer than average. These events were examined for xallarap (or binary-source motion), which can mimic parallax. We find that 23% of these events are strongly affected by xallarap. \\ ( http://arXiv.org/abs/astro-ph/0506183 , 140kb) From owner-public@setileague.org Fri Jun 10 09:08:04 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5AG82Uw024196 for ; Fri, 10 Jun 2005 09:08:03 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id LAA22590 for public-list; Fri, 10 Jun 2005 11:55:55 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f33.bay103.hotmail.com [65.54.174.43]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id LAA22586; Fri, 10 Jun 2005 11:55:52 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 10 Jun 2005 08:55:21 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Fri, 10 Jun 2005 15:55:20 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Understanding our Origins: Star Formation in H II Region Environments Date: Fri, 10 Jun 2005 11:55:20 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 10 Jun 2005 15:55:21.0665 (UTC) FILETIME=[CE9A7310:01C56DD4] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506190 Date: Thu, 9 Jun 2005 00:27:34 GMT (366kb) Title: Understanding our Origins: Star Formation in H II Region Environments Authors: J. Jeff Hester & Steven J. Desch (Dept. of Physics & Astronomy, Arizona State University) Comments: 25 pages, 10 figures. Refereed and accepted submission of an invited presentation to the Proceedings from the Workshop on Chondrites and the Protoplanetary Disk, Kaua'i Hawai'i, November 8-11, 2004. ASP conference series, editors A. Krot, E. Scott, & B. Reipurth. Higher quality copy available at http://eagle.la.asu.edu/hester/kauai/kauai_hester_final.pdf \\ Recent analysis of the decay products of short-lived radiounclides (SLRs) in meteorites, in particular the confirmation of the presence of live 60Fe in the early Solar System, provides unambiguous evidence that the Sun and Solar System formed near a massive star. We consider the question of the formation of low-mass stars in environments near massive stars, presenting a scenario for the evolution of a star and its disk around the periphery of an expanding H II region. The stages in this scenario begin with compression of molecular gas around the edge of an H II region, continue as forming stars are overrun by the advancing ionization front, and culminate when ejecta from one or more nearby supernova explosions sweeps over YSO disks located in the low density interior of the H II region, injecting SLRs including 26Al and 60Fe. We review the evidence that this mode of star formation is more characteristic of formation of low-mass stars than is the mode of star formation seen in regions such as the Taurus-Auriga molecular cloud. We discuss the implications of this scenario for our understanding of star formation, as well as the effects of the young Sun's astrophysical environment on the formation and evolution of the Solar System. We conclude that low-mass stars and their accompanying disks form and evolve very differently near massive stars than they do in regions like Taurus-Auriga, and that these differences have profound implications for our understanding of our origins. \\ ( http://arXiv.org/abs/astro-ph/0506190 , 366kb) From owner-public@setileague.org Fri Jun 10 10:50:35 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5AHoYUw017019 for ; Fri, 10 Jun 2005 10:50:35 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id NAA25336 for public-list; Fri, 10 Jun 2005 13:43:52 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f23.bay103.hotmail.com [65.54.174.33]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id NAA25332; Fri, 10 Jun 2005 13:43:49 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 10 Jun 2005 10:43:18 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Fri, 10 Jun 2005 17:43:17 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: NSF Media Advisory: Scientists Make New Discovery About Planets Outside Our Date: Fri, 10 Jun 2005 13:43:17 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 10 Jun 2005 17:43:18.0234 (UTC) FILETIME=[E2F073A0:01C56DE3] Sender: owner-public@setileague.org Precedence: bulk NSF Media Advisory: Scientists Make New Discovery About Planets Outside Our Solar System http://www.spaceref.com/news/viewpr.html?pid=17087 "Just within the past 10 years, astronomers have discovered well over a hundred planets in orbit around stars beyond our own Sun. Now the National Science Foundation invites reporters to a media briefing on a major advance in the search for such planets. The briefing will also be Webcast, and viewers will be able to submit questions via telephone and e-mail." From owner-public@setileague.org Fri Jun 10 14:10:58 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5ALAtUw026293 for ; Fri, 10 Jun 2005 14:10:57 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id RAA00466 for public-list; Fri, 10 Jun 2005 17:00:53 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f13.bay103.hotmail.com [65.54.174.23]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id RAA00462 for ; Fri, 10 Jun 2005 17:00:51 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 10 Jun 2005 14:00:20 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Fri, 10 Jun 2005 21:00:19 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Subject: SETI public: FW: [NOVA] "World in the Balance: The People Paradox" Date: Fri, 10 Jun 2005 17:00:19 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 10 Jun 2005 21:00:20.0278 (UTC) FILETIME=[696D3560:01C56DFF] Sender: owner-public@setileague.org Precedence: bulk >From: owner-nova-online@franz.wgbh.org (NOVA) >To: nova-online@franz.wgbh.org (NOVA Bulletin) >Subject: [NOVA] "World in the Balance: The People Paradox" >Date: Fri, 10 Jun 2005 14:24:42 -0400 (EDT) > >_____________________________________________________________________ >Next on NOVA: "World in the Balance: The People Paradox" (Repeat) > >http://www.pbs.org/nova/worldbalance/ > >Broadcast: June 14, 2005, 8 p.m. ET/PT >(NOVA airs Tuesdays on PBS at 8 p.m. Check your local listings.) > >It took all of human history until the year 1804 for our population >to reach its first billion. Now a billion new people are added every >dozen years. What does the future hold for Earth's growing human >family and its environmental health? In "The People Paradox," the >first installment of NOVA's two-hour special "World in the Balance," >our producers investigate three countries -- India, Kenya, and >Japan -- where social and economic forces have produced starkly >different population profiles. With moving personal stories, this >program gives an up-to-date global snapshot of today's human family, >now numbering 6.3 billion and likely to increase to nearly 9 billion >by 2050. > >Here's what you'll find online: > >Inquiry, Interviews, and More > > Out of House and Home > Can what happened on one small island in the South Pacific serve > as a cautionary tale for the entire planet? > > Voices of Concern > Interviews with five experts reveal the threats facing human > populations, national economies, and the global climate. > > Producer's Stories > Go behind the scenes with filmmakers as they struggle to capture > complex human stories. > > Material World > Open your eyes to the rich-poor divide with these photos showing > average families and their possessions. > > Population Campaigns > Compare how three developing nations have tried to slow rapid > population growth. > >Interactives > > Human Numbers Through Time > Examine the startling population growth over the past two > millennia, and see what's coming in the next 50 years. > > Global Trends Quiz > Test your understanding of the population trends and > environmental challenges facing nations around the world. > > Be a Demographer > Play a matching game to see how demographic data reflect and > shape the future of the U.S. and three other countries. > > Earth in Peril > How do consumption and rapid population growth affect our > planet's natural resources? Explore the many ways in this > collection of maps. > >Also, Links & Books, Educator Role Plays, a Teacher's Guide, a video >preview of the program, and the program transcript. > >http://www.pbs.org/nova/worldbalance/ > >_____________________________________________________________________ >_____________________________________________________________________ > >Thank you for visiting NOVA on the Web. We welcome your questions, >comments, and feedback. You can send a message directly to >nova@wgbh.org, or use our feedback form at >http://www.pbs.org/nova/feedback/ > >You are subscribed to the NOVA Bulletin. To unsubscribe, go to >http://www.pbs.org/nova/mailing/unsubscribe.html -- or send an >e-mail to majordomo@franz.wgbh.org and, on a line by itself in the >message, type: unsubscribe nova-online > >Major funding for NOVA is provided by the Park Foundation, Sprint, >and Microsoft. Additional funding provided by the Corporation for >Public Broadcasting and viewers like you. >_____________________________________________________________________ > From owner-public@setileague.org Fri Jun 10 14:32:38 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5ALWbUw029472 for ; Fri, 10 Jun 2005 14:32:38 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id RAA01089 for public-list; Fri, 10 Jun 2005 17:23:47 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f26.bay103.hotmail.com [65.54.174.36]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id RAA01085; Fri, 10 Jun 2005 17:23:44 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 10 Jun 2005 14:23:13 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Fri, 10 Jun 2005 21:23:13 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: The need for small-scale turbulence in atmospheres of substellar objects Date: Fri, 10 Jun 2005 17:23:13 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 10 Jun 2005 21:23:13.0667 (UTC) FILETIME=[9C07BD30:01C56E02] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506204 Date: Thu, 9 Jun 2005 13:54:28 GMT (472kb) Title: The need for small-scale turbulence in atmospheres of substellar objects Authors: Christiane Helling Comments: 7 pages, 2 figues, contribution to the Workshop on Interdisciplinary Aspects of Turbulence, April 18 - 22, 2005, Castle Ringberg, Germany \\ Brown dwarfs and giant gas planets are substellar objects whose spectral appearance is determined by the chemical composition of the gas and the solids/liquids in the atmosphere. Atmospheres of substellar objects possess two major scale regimes: large-scale convective motions + gravitational settling and small-scale turbulence + dust formation. Turbulence initiates dust formation spot-like on small scale, while the dust feeds back into the turbulent fluid field by its strong radiative cooling. Small, imploding dust containing areas result which eventually become isothermal. Multi-dimensional simulations show that these small-scale dust structures gather into large-scale structures, suggesting the formation of clouds made of dirty dust grains. The chemical composition of the grains, and thereby the chemical evolution of the gas phase, is a function of temperature and depends on the grain's history. \\ ( http://arXiv.org/abs/astro-ph/0506204 , 472kb) From owner-public@setileague.org Fri Jun 10 14:42:54 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5ALgrUw030318 for ; Fri, 10 Jun 2005 14:42:54 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id RAA01391 for public-list; Fri, 10 Jun 2005 17:34:21 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f28.bay103.hotmail.com [65.54.174.38]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id RAA01387; Fri, 10 Jun 2005 17:34:19 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 10 Jun 2005 14:33:48 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay103.hotmail.msn.com with HTTP; Fri, 10 Jun 2005 21:33:47 GMT X-Originating-IP: [65.54.174.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: public@setileague.org Cc: bioastro@setileague.org Subject: SETI public: Possible Giant Planets at Hundreds of AU in the HD141569 Disk Date: Fri, 10 Jun 2005 17:33:47 -0400 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 10 Jun 2005 21:33:48.0281 (UTC) FILETIME=[164A2690:01C56E04] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0506208 Date: Thu, 9 Jun 2005 15:10:42 GMT (460kb) Title: Spiral Structure when Setting up Pericentre Glow: Possible Giant Planets at Hundreds of AU in the HD141569 Disk Authors: M. C. Wyatt Comments: 13 pages, accepted by A&A \\ This paper discusses the impact of introducing a planet on an eccentric orbit into a planetesimal disk. That planet's secular perturbations cause the orbits of the planetesimals to evolve in such a way that at any one time planetesimals at the same distance from the star have common pericentres and eccentricities. This causes the surface density distribution of an extended planetesimal disk to exhibit two spirals, one exterior the other interior to the planet's orbit. These two spirals unwind in different directions and their structure is described by two parameters: the time since the planet was introduced and the planet's eccentricity. At late times the spirals become tightly wound and the offset centre of symmetry of the pericentre glow approximation is recovered. Comparison with spiral structure seen in the HD141569 disk shows that its spiral at 325 AU is similar to that caused by introducing a planet 5 Myr ago with a mass 0.2-2M_Jup orbiting at 235-250 AU with an eccentricity of 0.05-0.2; likewise a Saturn mass planet at 150 AU would cause structure like that seen at 200 AU. More definitive statements about any planets orbiting HD141569 from this model could be made once the effect of the binary companion on the disk is known, and once the disk's structure has been better characterised down to 100 AU, including the location of the star within the disk. The relatively young age of this system (~5 Myr) means that if giant planets really do exist at hundreds of AU from HD141569, this provides a unique opportunity to set constraints on the mechanism by which those planets came to be at such large distances. \\ ( http://arXiv.org/abs/astro-ph/0506208 , 460kb) From owner-public@setileague.org Mon Jun 13 11:29:18 2005 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.12.6/8.12.6) with ESMTP id j5DITHUw030106 for ; Mon, 13 Jun 2005 11:29:17 -0700 (PDT) Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id OAA12328 for public-list; Mon, 13 Jun 2005 14:18:38 -0400 (EDT) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay103-f31.bay103.hotmail.com [65.54.174.41]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id OAA12323; Mon, 13 Jun 2005 14:18:34 -0400 (EDT) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Mon, 13 Jun 2005 11:18:00 -0700 Message-ID: Received: from 65.54.174.200 by by103fd.bay1