From owner-public@setileague.org Sun Jan 1 08:18:27 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k01GIRFA025523 for ; Sun, 1 Jan 2006 08:18:27 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id LAA09749 for public-list; Sun, 1 Jan 2006 11:12:37 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav17.bay114.hotmail.com [65.54.169.89]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id LAA09745 for ; Sun, 1 Jan 2006 11:12:34 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Sun, 1 Jan 2006 08:12:03 -0800 Message-ID: Received: from 71.123.18.73 by BAY114-DAV17.phx.gbl with DAV; Sun, 01 Jan 2006 16:12:02 +0000 X-Originating-IP: [71.123.18.73] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Subject: SETI public: Fw: Latest News from the Astrobiology Magazine Date: Sun, 1 Jan 2006 11:12:05 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_0032_01C60EC4.32FA4840" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Sun, 1 Jan 2006 11:12:05 -0500 X-OriginalArrivalTime: 01 Jan 2006 16:12:03.0313 (UTC) FILETIME=[1A508E10:01C60EEE] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_0032_01C60EC4.32FA4840 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable ----- Original Message -----=20 From: Astrobiology Magazine=20 To: ljk4@msn.com=20 Sent: Sunday, January 01, 2006 5:35 AM Subject: Latest News from the Astrobiology Magazine Columbia Survivors http://www.astrobio.net/news/article1821.html On board the Space Shuttle Columbia mission STS-107, researchers were = studying the growth and reproductive behavior of the nematode worm = Caenorhabditis elegans, but the mission ended in tragedy in 2003 when = the shuttle broke up during reentry. Remarkably, the worms, housed in = specially designed canisters, survived the virtually unprotected reentry = into the Earth's atmosphere and were recovered alive during the = extensive recovery effort following the crash. Evolution of Movement Design is Deterministic http://www.astrobio.net/news/article1820.html A single unifying physics theory can essentially describe how animals of = every ilk, from flying insects to fish, get around, researchers at Duke = University's Pratt School of Engineering and Pennsylvania State = University have found. The team reports that all animals bear the same = stamp of physics in their design. Reading Space Dust http://www.astrobio.net/news/article1819.html The University of Colorado at Boulder's long heritage with NASA = planetary missions will continue Jan. 17 with the launch of a student = space dust instrument on the New Horizons Mission to Pluto from = Florida's Kennedy Space Center. Journey to Another Planet http://www.astrobio.net/news/article1818.html Some of the highest lakes in the world can be found at the summits of = volcanic mountains in the Andes, straddling the border between Chile and = Bolivia. The High Lakes 2005 research team has just completed an = expedition to explore two of those lakes. The lakes offer researchers an = opportunity to study life in an extreme environment on Earth that in = many ways mimic conditions on Mars. Expedition leader, Nathalie Cabrol, = continues her series of captain's logs. Sunday, January 01=20 ------------------------ For more astrobiology news, visit = http://www.astrobio.net To unsubscribe, send subject UNSUBSCRIBE to = astronaut@astrobio.net ------=_NextPart_000_0032_01C60EC4.32FA4840 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
 
----- Original = Message -----=20
Sent: Sunday, January 01, 2006 5:35 AM
Subject: Latest News from the Astrobiology = Magazine


Columbia Survivors
http://www.astrobi= o.net/news/article1821.html

On=20 board the Space Shuttle Columbia mission STS-107, researchers were = studying the=20 growth and reproductive behavior of the nematode worm Caenorhabditis = elegans,=20 but the mission ended in tragedy in 2003 when the shuttle broke up = during=20 reentry. Remarkably, the worms, housed in specially designed canisters, = survived=20 the virtually unprotected reentry into the Earth's atmosphere and were = recovered=20 alive during the extensive recovery effort following the = crash.

Evolution=20 of Movement Design is Deterministic
http://www.astrobi= o.net/news/article1820.html

A=20 single unifying physics theory can essentially describe how animals of = every=20 ilk, from flying insects to fish, get around, researchers at Duke = University's=20 Pratt School of Engineering and Pennsylvania State University have = found. The=20 team reports that all animals bear the same stamp of physics in their=20 design.

Reading Space Dust
http://www.astrobi= o.net/news/article1819.html

The=20 University of Colorado at Boulder's long heritage with NASA planetary = missions=20 will continue Jan. 17 with the launch of a student space dust instrument = on the=20 New Horizons Mission to Pluto from Florida's Kennedy Space=20 Center.

Journey to Another Planet
http://www.astrobi= o.net/news/article1818.html

Some=20 of the highest lakes in the world can be found at the summits of = volcanic=20 mountains in the Andes, straddling the border between Chile and Bolivia. = The=20 High Lakes 2005 research team has just completed an expedition to = explore two of=20 those lakes. The lakes offer researchers an opportunity to study life in = an=20 extreme environment on Earth that in many ways mimic conditions on Mars. = Expedition leader, Nathalie Cabrol, continues her series of captain's=20 logs.

Sunday, January 01

------------------------
For = more=20 astrobiology news, visit http://www.astrobio.net

To=20 unsubscribe, send subject UNSUBSCRIBE to astronaut@astrobio.net

=


------=_NextPart_000_0032_01C60EC4.32FA4840-- From owner-public@setileague.org Mon Jan 2 19:35:12 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k033ZCkV002344 for ; Mon, 2 Jan 2006 19:35:12 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id WAA01695 for public-list; Mon, 2 Jan 2006 22:30:20 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav5.bay114.hotmail.com [65.54.169.77]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id WAA01691; Mon, 2 Jan 2006 22:30:17 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Mon, 2 Jan 2006 19:29:46 -0800 Message-ID: Received: from 71.240.242.196 by BAY114-DAV5.phx.gbl with DAV; Tue, 03 Jan 2006 03:29:45 +0000 X-Originating-IP: [71.240.242.196] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: The Study of the Pioneer Anomaly: New Data and Objectives for New Investigation Date: Mon, 2 Jan 2006 22:29:48 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_0147_01C60FEC.09FAFCE0" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Mon, 2 Jan 2006 22:29:48 -0500 X-OriginalArrivalTime: 03 Jan 2006 03:29:46.0215 (UTC) FILETIME=[F1B4BF70:01C61015] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_0147_01C60FEC.09FAFCE0 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable General Relativity and Quantum Cosmology, abstract=20 gr-qc/0512121=20 From: Slava G. Turyshev [view email] Date: Wed, 21 Dec 2005 21:49:36 GMT (882kb) The Study of the Pioneer Anomaly: New Data and Objectives for New = Investigation Authors: Slava G. Turyshev, Viktor T. Toth, Larry R. Kellogg, Eunice. L. = Lau, Kyong J. Lee Comments: 42 pages, 40 figures, 3 tables Radiometric tracking data from Pioneer 10 and 11 spacecraft has = consistently indicated the presence of a small, anomalous, Doppler = frequency drift, uniformly changing with a rate of ~6 x 10^{-9} Hz/s; = the drift can be interpreted as a constant sunward acceleration of each = particular spacecraft of a_P =3D (8.74 \pm 1.33) x 10^{-10} m/s^2. This = signal is known as the Pioneer anomaly; the nature of this anomaly = remains unexplained. We discuss the efforts to retrieve the entire data = sets of the Pioneer 10/11 radiometric Doppler data. We also report on = the recently recovered telemetry files that may be used to reconstruct = the engineering history of both spacecraft using original project = documentation and newly developed software tools. We discuss possible = ways to further investigate the discovered effect using these telemetry = files in conjunction with the analysis of the much extended Doppler = data. We present the main objectives of new upcoming study of the = Pioneer anomaly, namely i) analysis of the early data that could yield = the direction of the anomaly, ii) analysis of planetary encounters, that = should tell more about the onset of the anomaly, iii) analysis of the = entire dataset, to better determine the anomaly's temporal behavior, iv) = comparative analysis of individual anomalous accelerations for the two = Pioneers, v) the detailed study of on-board systematics, and vi) = development of a thermal-electric-dynamical model using on-board = telemetry. The outlined strategy may allow for a higher accuracy = solution for a_P and, possibly, will lead to an unambiguous = determination of the origin of the Pioneer anomaly.=20 http://arxiv.org/abs/gr-qc/0512121 ------=_NextPart_000_0147_01C60FEC.09FAFCE0 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
General = Relativity and=20 Quantum Cosmology, abstract
gr-qc/0512121=20

From: Slava G. Turyshev [view email]

Date: Wed, 21 Dec 2005 21:49:36 GMT (882kb)

The Study of the Pioneer Anomaly: New Data and Objectives for New=20 Investigation

Authors: Slava G. Turyshev, Viktor T. Toth, Larry R. Kellogg, Eunice. = L. Lau,=20 Kyong J. Lee

Comments: 42 pages, 40 figures, 3 tables

Radiometric tracking data from Pioneer 10 and 11 spacecraft has = consistently=20 indicated the presence of a small, anomalous, Doppler frequency drift, = uniformly=20 changing with a rate of ~6 x 10^{-9} Hz/s; the drift can be interpreted = as a=20 constant sunward acceleration of each particular spacecraft of a_P =3D = (8.74 \pm=20 1.33) x 10^{-10} m/s^2. This signal is known as the Pioneer anomaly; the = nature=20 of this anomaly remains unexplained. We discuss the efforts to retrieve = the=20 entire data sets of the Pioneer 10/11 radiometric Doppler data. We also = report=20 on the recently recovered telemetry files that may be used to = reconstruct the=20 engineering history of both spacecraft using original project = documentation and=20 newly developed software tools. We discuss possible ways to further = investigate=20 the discovered effect using these telemetry files in conjunction with = the=20 analysis of the much extended Doppler data. We present the main = objectives of=20 new upcoming study of the Pioneer anomaly, namely i) analysis of the = early data=20 that could yield the direction of the anomaly, ii) analysis of planetary = encounters, that should tell more about the onset of the anomaly, iii) = analysis=20 of the entire dataset, to better determine the anomaly's temporal = behavior, iv)=20 comparative analysis of individual anomalous accelerations for the two = Pioneers,=20 v) the detailed study of on-board systematics, and vi) development of a=20 thermal-electric-dynamical model using on-board telemetry. The outlined = strategy=20 may allow for a higher accuracy solution for a_P and, possibly, will = lead to an=20 unambiguous determination of the origin of the Pioneer anomaly.

http://arxiv.org/abs/gr-qc/0512121

------=_NextPart_000_0147_01C60FEC.09FAFCE0-- From owner-public@setileague.org Tue Jan 3 14:08:10 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k03M89ij007883 for ; Tue, 3 Jan 2006 14:08:09 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id RAA26547 for public-list; Tue, 3 Jan 2006 17:04:50 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f39.bay114.hotmail.com [65.54.169.49]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id RAA26543; Tue, 3 Jan 2006 17:04:47 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Tue, 3 Jan 2006 14:04:16 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Tue, 03 Jan 2006 22:04:15 GMT X-Originating-IP: [24.39.94.195] 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: Supernova-driven turbulence inhibits star formation globally rather than trigger Date: Tue, 03 Jan 2006 17:04:15 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 03 Jan 2006 22:04:16.0599 (UTC) FILETIME=[A38F9670:01C610B1] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0601005 Date: Sat, 31 Dec 2005 18:50:46 GMT (980kb) Title: Turbulent Structure of a Stratified Supernova-Driven Interstellar Medium Authors: M. K. Ryan Joung (1 and 2), Mordecai-Mark Mac Low (2 and 1) ((1) Columbia University, (2) AMNH) Comments: 15 pages, 11 figures, submitted to ApJ \\ To study how supernova feedback structures the turbulent interstellar medium, we construct 3D models of vertically stratified gas stirred by discrete supernova explosions, including vertical gravitational field and parametrized heating and cooling. The models reproduce many observed characteristics of the Galaxy such as global circulation of gas (i.e., galactic fountain) and the existence of cold dense clouds in the galactic disk. Global quantities of the model such as warm and hot gas filling factors in the midplane, mass fraction of thermally unstable gas, and the averaged vertical density profile are compared directly with existing observations, and shown to be broadly consistent. We find that energy injection occurs over a broad range of scales. There is no single effective driving scale, unlike the usual assumption for idealized models of incompressible turbulence. However, >90% of the total kinetic energy is contained in wavelengths shortward of 200 pc. The shape of the kinetic energy spectrum differs substantially from that of the velocity power spectrum, which implies that the velocity structure varies with the gas density. Velocity structure functions demonstrate that the phenomenological theory proposed by Boldyrev is applicable to the medium. We show that it can be misleading to predict physical properties such as the stellar initial mass function based on numerical simulations that do not include self-gravity of the gas. Even if all the gas in turbulently Jeans unstable regions in our simulation is assumed to collapse and form stars in local freefall times, the resulting total collapse rate is significantly lower than the value consistent with the input supernova rate. Supernova-driven turbulence inhibits star formation globally rather than triggering it. \\ ( http://arXiv.org/abs/astro-ph/0601005 , 980kb) From owner-public@setileague.org Wed Jan 4 07:55:02 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: * X-Spam-Status: No, score=1.3 required=5.5 tests=MSGID_FROM_MTA_HEADER, RCVD_IN_BL_SPAMCOP_NET autolearn=no version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k04Ft1kt006007 for ; Wed, 4 Jan 2006 07:55:02 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id KAA20277 for public-list; Wed, 4 Jan 2006 10:48:35 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f34.bay114.hotmail.com [65.54.169.44]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id KAA20273 for ; Wed, 4 Jan 2006 10:48:33 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 4 Jan 2006 07:48:01 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Wed, 04 Jan 2006 15:48:00 GMT X-Originating-IP: [24.39.94.195] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com In-Reply-To: <101AB72B-1564-4F6E-AA9A-B2065EF12836@cs.bham.ac.uk> From: "LARRY KLAES" To: W.H.Edmondson@cs.bham.ac.uk, public@setileague.org Subject: RE: SETI public: Pulsars as beacons for SETI Date: Wed, 04 Jan 2006 10:48:00 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 04 Jan 2006 15:48:01.0499 (UTC) FILETIME=[3E2A72B0:01C61146] Sender: owner-public@setileague.org Precedence: bulk Hi William, It's great to see someone doing actual SETI work! Best of luck and please keep us updated on your progress. Larry >From: William Edmondson >To: public@setileague.org >Subject: SETI public: Pulsars as beacons for SETI >Date: Thu, 29 Dec 2005 21:03:00 +0000 > >Hi folks > >You may recall many months back I posted a URL for a paper I'd had >published on a new search strategy. http://www.cs.bham.ac.uk/~whe/ >SETIPaper.pdf > >In February his year I visited Arecibo to gather some data, having being >awarded some time (see http://www.cs.bham.ac.uk/~whe/ AOproposal.pdf). We >eventually had ~30 hours of dedicated 'scope time. Pretty impressive. I >even got to drive the machine from my office back in UK for one >observation session! > >It's been a bit of a slog to get the data storage and processing hardware >organized (I don't work in a physics/astronomy department at the Uni in >Birmingham - and yes, although I DO work in a Computer Science department >we are the last people to need lots of storage etc....; it's a pretty >theoretical department and many of my colleagues work with pencil and >paper!). > >Shortly before Christmas the last two disks arrived from Arecibo and I now >have 3TB of data connected to a dual G5 Mac dedicated to SETI work. > >So now the hard work begins. I am, essentially, using some well-known >techniques from the world of pulsar search astronomy. I can recommend the >following (but it is expensive): > >Handbook of Pulsar Astronomy, by Duncan Lorimer and Michael Kramer. >Cambridge University Press. 2005. > >Duncan has been helpful with advice (my physics is a little rusty, having >completed my degree several decades ago and then moving on to other >fields). > >I am focussing at the moment on folding techniques, with some dispersion >correction as well (although the target stars are not that far away one >might envisage a small mark to space ratio in a pulsed transmission, which >implies the need for de-dispersion to preserve pulse shape....). I am >doing this because we have a target periodicity to search for, and folding >can significantly enhance S/N ratio. I'll probably try some FFT as well, >just in case there is a pulsar waiting to be discovered! > >I'll probably provide another update in a year's time. > >Happy searching in 2006. > >William Edmondson From owner-public@setileague.org Wed Jan 4 10:33:28 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: * X-Spam-Status: No, score=1.3 required=5.5 tests=MSGID_FROM_MTA_HEADER, RCVD_IN_BL_SPAMCOP_NET autolearn=no version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k04IXRS5006718 for ; Wed, 4 Jan 2006 10:33:28 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id NAA23735 for public-list; Wed, 4 Jan 2006 13:26:19 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f29.phx.gbl [65.54.169.39] (may be forged)) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id NAA23731; Wed, 4 Jan 2006 13:26:16 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 4 Jan 2006 10:25:44 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Wed, 04 Jan 2006 18:25:43 GMT X-Originating-IP: [24.39.94.195] 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: Can Minor Planets be Used to Assess Gravity in the Outer Solar System? Date: Wed, 04 Jan 2006 13:25:43 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 04 Jan 2006 18:25:44.0618 (UTC) FILETIME=[469FD0A0:01C6115C] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0504367 Date (v1): Sun, 17 Apr 2005 17:04:48 GMT (32kb) Date (revised v2): Sat, 1 Oct 2005 13:46:27 GMT (43kb) Date (revised v3): Mon, 2 Jan 2006 16:12:03 GMT (36kb) replaced with revised version Mon, 2 Jan 2006 16:12:03 GMT (36kb) Title: Can Minor Planets be Used to Assess Gravity in the Outer Solar System? Authors: Gary L. Page, David S. Dixon, John F. Wallin Comments: Accepted for publication in The Astrophysical Journal The twin Pioneer spacecraft have been tracked for over thirty years as they headed out of the solar system. After passing 20 AU from the Sun, both exhibited a systematic error in their trajectories that can be interpreted as a constant acceleration towards the Sun. This Pioneer Effect is most likely explained by spacecraft systematics, but there have been no convincing arguments that that is the case. The alternative is that the Pioneer Effect represents a real phenomenon and perhaps new physics. What is lacking is a means of measuring the effect, its variation, its potential anisotropies, and its region of influence. We show that minor planets provide an observational vehicle for investigating the gravitational field in the outer solar system, and that a sustained observation campaign against properly chosen minor planets could confirm or refute the existence of the Pioneer Effect. Additionally, even if the Pioneer Effect does not represent a new physical phenomenon, minor planets can be used to probe the gravitational field in the outer Solar System and since there are very few intermediate range tests of gravity at the multiple AU distance scale, this is a worthwhile endeavor in its own right. \\ ( http://arXiv.org/abs/astro-ph/0504367 , 36kb) From owner-public@setileague.org Wed Jan 4 12:13:55 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: ** X-Spam-Status: No, score=2.8 required=5.5 tests=AMATEUR_PORN, MSGID_FROM_MTA_HEADER,RCVD_IN_BL_SPAMCOP_NET autolearn=no version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k04KDtoO007120 for ; Wed, 4 Jan 2006 12:13:55 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id PAA26114 for public-list; Wed, 4 Jan 2006 15:10:57 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f26.bay114.hotmail.com [65.54.169.36]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id PAA26110; Wed, 4 Jan 2006 15:10:55 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 4 Jan 2006 12:10:19 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Wed, 04 Jan 2006 20:10:18 GMT X-Originating-IP: [24.39.94.195] 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: Amateur stargazers needed to help solve mystery / Pluto's frigid surprise Date: Wed, 04 Jan 2006 15:10:18 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 04 Jan 2006 20:10:19.0028 (UTC) FILETIME=[E276CD40:01C6116A] Sender: owner-public@setileague.org Precedence: bulk >From: "NewsAlert" >Reply-To: "Newsalert" >To: "Newsalert" >Subject: Amateur stargazers needed to help solve mystery / Pluto's frigid >surprise >Date: Wed, 4 Jan 2006 13:52:26 -0500 > > NEWSALERT: Wednesday, January 4, 2005 @ 1857 GMT > --------------------------------------------------------------------- > The latest news from Spaceflight Now > > >+++ ADVERTISEMENT +++ >Free technical seminar! Free analysis software! Join AGI at one of 10 >North American tour stops in January to learn about enhanced analysis >features and enterprise integration capabilities within the latest version >release of STK 7. Free registration at: http://www.agi.com/7Tour >+++ > > >WANTED: AMATEUR STARGAZERS TO HELP SOLVE MYSTERY >------------------------------------------------ >Ohio State University scientists have thought of a new way to solve an >astronomical mystery, and their plan relies on a well-connected network of >amateur stargazers and one very elusive subatomic particle. > > http://spaceflightnow.com/news/n0601/04mystery/ > > >PLUTO HAS BEEN FOUND COLDER THAN IT SHOULD BE >--------------------------------------------- >Mercury is boiling. Mars is freezing. The Earth is just right. When it >comes to the temperatures of the planets, it makes sense that they should >get colder the farther away they are from the Sun. But then there is >Pluto. It has been suspected that this remote world might be even colder >than it should be. Smithsonian scientists now have shown this to be true. > > http://spaceflightnow.com/news/n0601/03coldpluto/ > > >RESEARCHERS AWAIT TREASURE FROM STARDUST'S EPIC JOURNEY >------------------------------------------------------- >Donald Brownlee's heart skipped a beat six years ago when the launch of >the Stardust spacecraft didn't happen as planned. The University of >Washington astronomy professor has experienced many other tense times >since the historic mission blasted off a day late, and its return to Earth >on Jan. 15 will be just one more white-knuckle moment. > > > http://spaceflightnow.com/news/n0601/03stardust/ > > >----------------------------------------------------------------------- > > A DIGITAL RECORD OF SPACE HISTORY > > Visit the Astronomy Now Store for a full listing of space DVD discs. > New digital transfers offer the ultimate record > of the Apollo Moon landings. > > http://www.spaceflightnowstore.com > >----------------------------------------------------------------------- > > >AOL USERS >--------- >The links below make it easier for AOL users to reach our stories. > >AGI ADVERTISEMENT > >WANTED: AMATEUR >STARGAZERS TO HELP SOLVE MYSTERY > >PLUTO HAS BEEN >FOUND COLDER THAN IT SHOULD BE > >RESEARCHERS >AWAIT TREASURE FROM STARDUST'S EPIC JOURNEY > >SPACEFLIGHT NOW STORE > >--- From owner-public@setileague.org Wed Jan 4 16:00:25 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k0500Ogr008245 for ; Wed, 4 Jan 2006 16:00:24 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id SAA00965 for public-list; Wed, 4 Jan 2006 18:50:50 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav3.bay114.hotmail.com [65.54.169.75]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id SAA00960; Wed, 4 Jan 2006 18:50:48 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Wed, 4 Jan 2006 15:50:16 -0800 Message-ID: Received: from 71.123.22.200 by BAY114-DAV3.phx.gbl with DAV; Wed, 04 Jan 2006 23:50:16 +0000 X-Originating-IP: [71.123.22.200] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: Atmosphere, Interior, and Evolution of the Metal-Rich Transiting Planet HD 149026b Date: Wed, 4 Jan 2006 18:50:20 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_00A1_01C6115F.B6399470" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 x-mimeole: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Wed, 4 Jan 2006 18:50:20 -0500 X-OriginalArrivalTime: 04 Jan 2006 23:50:16.0906 (UTC) FILETIME=[9D032AA0:01C61189] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_00A1_01C6115F.B6399470 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable Paper: astro-ph/0507422 From: Jonathan J. Fortney [view email] Date (v1): Mon, 18 Jul 2005 21:49:23 GMT (134kb)=20 Date (revised v2): Tue, 3 Jan 2006 19:32:19 GMT (224kb) replaced with revised version Tue, 3 Jan 2006 19:32:19 GMT (224kb) Title: Atmosphere, Interior, and Evolution of the Metal-Rich Transiting = Planet=20 HD 149026b Authors: J. J. Fortney, D. Saumon, M. S. Marley, K. Lodders, R. S. = Freedman Comments: Accepted to the Astrophysical Journal. 18 pages, including 10=20 figures. New section on the atmosphere of planet HD 189733b. Enhanced=20 discussion of atmospheric Ti chemistry and core mass for HD 149026b We investigate the atmosphere and interior of the new transiting planet = HD 149026b, which appears to be very rich in heavy elements. We first = compute model atmospheres at metallicities ranging from solar to ten = times solar, and show how for cases with high metallicity or inefficient = redistribution of energy from the day side, the planet may develop a hot = stratosphere due to absorption of stellar flux by TiO and VO. The = spectra predicted by these models are very different than cooler = atmosphere models without stratospheres. The spectral effects are = potentially detectable with the Spitzer Space Telescope. In addition the = models with hot stratospheres lead to a large limb brightening, rather = than darkening. We compare the atmosphere of HD 149026b to other = well-known transiting planets, including the recently discovered HD = 189733b, which we show have planet-to-star flux ratios twice that of HD = 209458 and TrES-1. The methane abundance in the atmosphere of HD 189733b = is a sensitive indicator of atmospheric temperature and metallicity and = can be constrained with Spitzer IRAC observations. We then turn to = interior studies of HD 149026b and use a grid of self-consistent model = atmospheres and high-pressure equations of state for all components to = compute thermal evolution models of the planet. We estimate that the = mass of heavy elements within the planet is in the range of 60 to 93 = M_earth. Finally, we discuss trends in the radii of transiting planets = with metallicity in light of this new member of the class.=20 \\ ( = http://arXiv.org/abs/astro-ph/0507422 , 224kb) ------=_NextPart_000_00A1_01C6115F.B6399470 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
Paper: astro-ph/0507422

From: Jonathan J. Fortney [view=20 email]

Date (v1): Mon, 18 Jul 2005 21:49:23 GMT (134kb)
Date = (revised=20 v2): Tue, 3 Jan 2006 19:32:19 GMT (224kb)

replaced with revised = version=20 Tue, 3 Jan 2006 19:32:19 GMT (224kb)

Title: Atmosphere, Interior, = and=20 Evolution of the Metal-Rich Transiting Planet
HD = 149026b

Authors: J.=20 J. Fortney, D. Saumon, M. S. Marley, K. Lodders, R. S. = Freedman

Comments:=20 Accepted to the Astrophysical Journal. 18 pages, including 10 =
figures. New=20 section on the atmosphere of planet HD 189733b. Enhanced
discussion = of=20 atmospheric Ti chemistry and core mass for HD 149026b

We = investigate the=20 atmosphere and interior of the new transiting planet HD 149026b, which = appears=20 to be very rich in heavy elements. We first compute model atmospheres at = metallicities ranging from solar to ten times solar, and show how for = cases with=20 high metallicity or inefficient redistribution of energy from the day = side, the=20 planet may develop a hot stratosphere due to absorption of stellar flux = by TiO=20 and VO. The spectra predicted by these models are very different than = cooler=20 atmosphere models without stratospheres. The spectral effects are = potentially=20 detectable with the Spitzer Space Telescope. In addition the models with = hot=20 stratospheres lead to a large limb brightening, rather than darkening. = We=20 compare the atmosphere of HD 149026b to other well-known transiting = planets,=20 including the recently discovered HD 189733b, which we show have = planet-to-star=20 flux ratios twice that of HD 209458 and TrES-1. The methane abundance in = the=20 atmosphere of HD 189733b is a sensitive indicator of atmospheric = temperature and=20 metallicity and can be constrained with Spitzer IRAC observations. We = then turn=20 to interior studies of HD 149026b and use a grid of self-consistent = model=20 atmospheres and high-pressure equations of state for all components to = compute=20 thermal evolution models of the planet. We estimate that the mass of = heavy=20 elements within the planet is in the range of 60 to 93 M_earth. Finally, = we=20 discuss trends in the radii of transiting planets with metallicity in = light of=20 this new member of the class.

\\ ( http://arXiv.org/abs/astro-ph/0507422 , = 224kb)
 
------=_NextPart_000_00A1_01C6115F.B6399470-- From owner-public@setileague.org Thu Jan 5 07:54:33 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k05FsWFr017711 for ; Thu, 5 Jan 2006 07:54:33 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id KAA21772 for public-list; Thu, 5 Jan 2006 10:46:48 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f15.bay114.hotmail.com [65.54.169.25]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id KAA21766; Thu, 5 Jan 2006 10:46:45 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 5 Jan 2006 07:46:13 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Thu, 05 Jan 2006 15:46:13 GMT X-Originating-IP: [24.39.94.195] 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: 3 Papers on Hot Jupiters and Our Jupiter Date: Thu, 05 Jan 2006 10:46:13 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 05 Jan 2006 15:46:13.0998 (UTC) FILETIME=[2880D8E0:01C6120F] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0512632 Date: Thu, 29 Dec 2005 02:18:57 GMT (19kb) Title: On the Relation Between Hot Jupiters & the Roche Limit Authors: Eric B. Ford (UC Berkeley), Frederic A. Rasio (Northwestern) Comments: 10 pages, 3 figures, to appear in ApJL \\ Many of the known extrasolar planets are ``hot Jupiters,'' giant planets with orbital periods of just a few days. We use the observed distribution of hot Jupiters to constrain the location of its inner edge in the mass--period diagram. If we assume a slope corresponding to the classical Roche limit, then we find that the edge corresponds to a separation close to_twice_ the Roche limit, as expected if the planets started on highly eccentric orbits that were later circularized. In contrast, any migration scenario would predict an inner edge right at the Roche limit, which applies to planets approaching on nearly circular orbits. However, the current sample of hot Jupiters is not sufficient to provide a precise constraint simultaneously on both the location and slope of the inner edge. \\ ( http://arXiv.org/abs/astro-ph/0512632 , 19kb) Paper: astro-ph/0601001 Date: Mon, 2 Jan 2006 14:57:58 GMT (588kb) Title: Frequency of Hot Jupiters and Very Hot Jupiters from the OGLE-III Transit Surveys Toward the Galactic Bulge and Carina Authors: Andrew Gould (Ohio State), Susan Dorsher (Ohio State), B. Scott Gaudi (CfA), Andrzej Udalski (Warsaw University Observatory) Comments: 62 pages including 16 figures and 9 tables. Submitted to Acta Astronomica. Full resolution version at http://www.astronomy.ohio-state.edu/~gould/ogle_hot_jupiters.ps.gz \\ We derive the frequencies of hot Jupiters (HJs) with 3--5 day periods and very hot Jupiters (VHJs) with 1-3 day periods by comparing the planets actually detected in the OGLE-III survey with those predicted by our models. The models are constructed following Gould & Morgan (2003) by populating the line of sight with stars drawn from the Hipparcos catalog. Using these, we demonstrate that the number of stars with sensitivity to HJs and VHJs is only 4--16% of those in the OGLE-III fields satisfying the spectroscopic-followup limit of V_max<17.5. Hence, the frequencies we derive are much higher than a naive estimate would indicate. We find that at 90% confidence the fraction of stars with planets in the two period ranges is (1/310)(1^{+1.39}_{-0.59}) for HJs and (1/690)(1^{+1.10}_{-0.54}) for VHJs. The HJ rate is statistically indistinguishable from that found in radial velocity (RV) studies. However, we note that magnitude-limited RV samples are heavily biased toward metal-rich (hence, planet-bearing) stars, while transit surveys are not, and therefore we expect that more sensitive transit surveys should find a deficit of HJs as compared to RV surveys. The detection of 3 transiting VHJs, all with periods less than 2 days, is marginally consistent with the complete absence of such detections in RV surveys. The planets detected are consistent with being uniformly distributed between 1.00 and 1.25 Jovian radii, but there are too few in the sample to map this distribution in detail. \\ ( http://arXiv.org/abs/astro-ph/0601001 , 588kb) Paper: astro-ph/0601043 Date: Tue, 3 Jan 2006 12:34:14 GMT (63kb) Title: Jupiter's composition: sign of a (relatively) late formation in a chemically evolved protosolar disk Authors: Tristan Guillot (OCA), Ricardo Hueso Comments: 6 pages, 3 figures, in press in MNRAS. The definitive version is available at www.blackwellsynergy.com Proxy: ccsd ccsd-00016408 \\ It has been proposed that the enrichment in noble gases found by Galileo in Jupiter's atmosphere can be explained by their delivery inside cold planetesimals. We propose instead that this is a sign that the planet formed in a chemically evolved disk and that noble gases were acquired mostly in gaseous form during the planet's envelope capture phase. We show that the combined settling of grains to the disk midplane in the cold outer layers, the condensation of noble gases onto these grains at temperatures below 20-30K, and the evaporation from high disk altitudes effectively lead to a progressive, moderate enrichment of the disk. The fact that noble gases are vaporized from the grains in the hot inner disk regions (e.g. Jupiter formation region) is not a concern because a negative temperature gradient prevents convection from carrying the species into the evaporating region. We show that the ~2 times solar enrichment of Ar, Kr, Xe in Jupiter is hence naturally explained by a continuous growth of the planet governed by viscous diffusion in the protosolar disk in conjunction with an evaporation of the disk and its progressive enrichment on a million years timescale. \\ ( http://arXiv.org/abs/astro-ph/0601043 , 63kb) From owner-public@setileague.org Thu Jan 5 07:57:51 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k05FvoNF017755 for ; Thu, 5 Jan 2006 07:57:50 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id KAA21868 for public-list; Thu, 5 Jan 2006 10:50:55 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f34.bay114.hotmail.com [65.54.169.44]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id KAA21864; Thu, 5 Jan 2006 10:50:52 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 5 Jan 2006 07:50:20 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Thu, 05 Jan 2006 15:50:19 GMT X-Originating-IP: [24.39.94.195] 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: 6 Papers on Exoworlds and Circumstellar Disks Date: Thu, 05 Jan 2006 10:50:19 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 05 Jan 2006 15:50:20.0710 (UTC) FILETIME=[BB8E1C60:01C6120F] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0512634 Date: Thu, 29 Dec 2005 02:19:45 GMT (100kb) Title: Improving the Efficiency of Markov Chain Monte Carlo for Analyzing the Orbits of Extrasolar Planets Authors: Eric B. Ford (UC Berkeley, Princeton) Comments: 46 pages, 5 figures, 2 tables, ApJ in press \\ Precise radial velocity measurements have led to the discovery of ~170 extrasolar planetary systems. Understanding the uncertainties in the orbital solutions will become increasingly important as the discovery space for extrasolar planets shifts to planets with smaller masses and longer orbital periods. The method of Markov chain Monte Carlo (MCMC) provides a rigorous method for quantifying the uncertainties in orbital parameters in a Bayesian framework (Ford 2005a). The main practical challenge for the general application of MCMC is the need to construct Markov chains which quickly converge. The rate of convergence is very sensitive to the choice of the candidate transition probability distribution function (CTPDF). Here we explain one simple method for generating alternative CTPDFs which can significantly speed convergence by one to three orders of magnitude. We have numerically tested dozens of CTPDFs with simulated radial velocity data sets to identify those which perform well for different types of orbits and suggest a set of CTPDFs for general application. Additionally, we introduce other refinements to the MCMC algorithm for radial velocity planets, including an improved treatment of the uncertainties in the radial velocity observations, an algorithm for automatically choosing step sizes, an algorithm for automatically determining reasonable stopping times, and the use of importance sampling for including the dynamical evolution of multiple planet systems. Together, these improvements make it practical to apply MCMC to multiple planet systems. We demonstrate the improvements in efficiency by analyzing a variety of extrasolar planetary systems. \\ ( http://arXiv.org/abs/astro-ph/0512634 , 100kb) Paper: astro-ph/0512635 Date: Thu, 29 Dec 2005 02:20:11 GMT (23kb) Title: What do Multiple Planet Systems Teach us about Planet Formation? Authors: Eric B. Ford Comments: 12 pages, to appear in Frank N. Bash Symposium 2005: New Horizons in Astronomy \\ For centuries, our knowledge of planetary systems and ideas about planet formation were based on a single example, our solar system. During the last thirteen years, the discovery of ~170 planetary systems has ushered in a new era for astronomy. I review the surprising properties of extrasolar planetary systems and discuss how they are reshaping theories of planet formation. I focus on how multiple planet systems constrain the mechanisms proposed to explain the large eccentricities typical of extrasolar planets. I suggest that strong planet-planet scattering is common and most planetary systems underwent a phase of large eccentricities. I propose that a planetary system's final eccentricities may be strongly influenced by how much mass remains in a planetesimal disk after the last strong planet-planet scattering event. \\ ( http://arXiv.org/abs/astro-ph/0512635 , 23kb) Paper: astro-ph/0601013 Date: Sun, 1 Jan 2006 10:33:27 GMT (49kb) Title: Dust Size Growth and Settling in a Protoplanetary Disk Authors: Hideko Nomura and Yoshitsugu Nakagawa (Kobe University) Comments: 27 pages, 8 figures, accepted for publication in the ApJ \\ We have studied dust evolution in a quiescent or turbulent protoplanetary disk by numerically solving coagulation equation for settling dust particles, using the minimum mass solar nebular model. As a result, if we assume an ideally quiescent disk, the dust particles settle toward the disk midplane to form a gravitationally unstable layer within 2x10^3 - 4x10^4 yr at 1 - 30 AU, which is in good agreement with an analytic calculation by Nakagawa, Sekiya, & Hayashi (1986) although they did not take into account the particle size distribution explicitly. In an opposite extreme case of a globally turbulent disk, on the other hand, the dust particles fluctuate owing to turbulent motion of the gas and most particles become large enough to move inward very rapidly within 70 - 3x10^4 yr at 1 - 30 AU, depending on the strength of turbulence. Our result suggests that global turbulent motion should cease for the planetesimal formation in protoplanetary disks. \\ ( http://arXiv.org/abs/astro-ph/0601013 , 49kb) Paper: astro-ph/0601024 Date: Mon, 2 Jan 2006 11:30:14 GMT (59kb) Title: High resolution spectroscopy of stars with transiting planets. The cases of OGLE-TR-10, 56, 111, 113, and TrES-1 Authors: N.C Santos, F. Pont, C. Melo, G. Israelian, F. Bouchy, M. Mayor, C. Moutou, D. Queloz, S. Udry, T. Guillot Comments: Accepted for Publication in Astronomy & Astrophysics \\ Context: During the past years photometric surveys, later complemented by follow-up radial-velocity measurements, have revealed the presence of several new extra-solar transiting planets, in very short period orbits. Many of the host stars are extremely faint (V$\sim$16), making high-precision spectroscopic measurements challenging. Aims: We have used the UVES spectrograph (VLT-UT2 telescope) to obtain high resolution spectra of 5 stars hosting transiting planets, namely for OGLE-TR-10, 56, 111, 113 and TrES-1. The immediate objective is to derive accurate stellar parameters and chemical abundances. Methods: The stellar parameters were derived from an LTE analysis of a set of FeI and FeII lines. Results: Complementing the spectroscopic information with photometric transit curves and radial-velocity data from the literature, we have then refined the stellar and planetary radii and masses. The obtained data were also used to study and discuss the relation between the stellar metallicity and orbital period of the planets. \\ ( http://arXiv.org/abs/astro-ph/0601024 , 59kb) Paper: astro-ph/0601028 Date: Mon, 2 Jan 2006 16:17:47 GMT (84kb) Title: Linear and Bayesian Planet Detection Algorithms for the Terrestrial Planet Finder Authors: N. Jeremy Kasdin, Isabelle Braems \\ Current plans call for the first Terrestrial Planet Finder mission, TPF-C, to be a monolithic space telescope with a coronagraph for achieving high contrast. The coronagraph removes the diffracted starlight allowing the nearby planet to be detected. In this paper, we present a model of the planet measurement and noise statistics. We utilize this model to develop two planet detection algorithms, one based on matched filtering of the PSF and one using Bayesian techniques. These models are used to formulate integration time estimates for a planet detection with desired small probabilities of false alarms and missed detections. \\ ( http://arXiv.org/abs/astro-ph/0601028 , 84kb) Paper: astro-ph/0601033 Date: Mon, 2 Jan 2006 21:00:08 GMT (148kb) Title: Massive Protoplanetary Disks in the Trapezium Region Authors: J.A. Eisner, John M. Carpenter Comments: 27 pages, including 7 figures. Accepted by ApJ \\ (abridged) We determine the disk mass distribution around 336 stars in the young Orion Nebula cluster by imaging a 2.5' x 2.5' region in 3 mm continuum emission with the Owens Valley Millimeter Array. For this sample of 336 stars, we observe 3 mm emission above the 3-sigma noise level toward ten sources, six of which have also been detected optically in silhouette against the bright nebular background. In addition, we detect 20 objects that do not correspond to known near-IR cluster members. Comparisons of our measured fluxes with longer wavelength observations enable rough separation of dust emission from thermal free-free emission, and we find substantial dust emission toward most objects. For the ten objects detected at both 3 mm and near-IR wavelengths, eight exhibit substantial dust emission. Excluding the high-mass stars and assuming a gas-to-dust ratio of 100, we estimate circumstellar masses ranging from 0.13 to 0.39 Msun. For the cluster members not detected at 3 mm, images of individual objects are stacked to constrain the mean 3 mm flux of the ensemble. The average flux is detected at the 3-sigma confidence level, and implies an average disk mass of 0.005 Msun, comparable to the minimum mass solar nebula. The percentage of stars in Orion surrounded by disks more massive than ~0.1 Msun is consistent with the disk mass distribution in Taurus, and we argue that massive disks in Orion do not appear to be truncated through close encounters with high-mass stars. Comparison of the average disk mass and number of massive dusty structures in Orion with similar surveys of the NGC 2024 and IC 348 clusters constrains the evolutionary timescales of massive circumstellar disks in clustered environments. \\ ( http://arXiv.org/abs/astro-ph/0601033 , 148kb) From owner-public@setileague.org Thu Jan 5 08:25:39 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k05GPdqH017898 for ; Thu, 5 Jan 2006 08:25:39 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id LAA22640 for public-list; Thu, 5 Jan 2006 11:20:12 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f39.bay114.hotmail.com [65.54.169.49]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id LAA22636; Thu, 5 Jan 2006 11:20:09 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 5 Jan 2006 08:19:38 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Thu, 05 Jan 2006 16:19:37 GMT X-Originating-IP: [24.39.94.195] 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: Physical Interpretations of Rotating Radio Transients Date: Thu, 05 Jan 2006 11:19:37 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 05 Jan 2006 16:19:38.0664 (UTC) FILETIME=[D3609A80:01C61213] Sender: owner-public@setileague.org Precedence: bulk Paper: astro-ph/0601063 Date: Wed, 4 Jan 2006 00:54:41 GMT (8kb) Title: Physical Interpretations of Rotating Radio Transients Authors: Bing Zhang (UNLV), Janusz Gil (Zielona Gora Univ) and Jaroslow Dyks (Nicolaus Copernicus Center) Comments: 3 pages, submitted to ApJL \\ Nearly a dozen of Rotating RAdio Transients (RRATs) have been discovered recently. These objects share similar spin parameters with normal radio pulsars but distinguish themselves from normal pulsars by being quiescent most of the time and only becoming radio bright occasionally. We discuss two possible interpretations to the phenomenon. The first model suggests that these objects are pulsars slightly below the radio emission ``death line'', and become active occasionally when the conditions for pair production and coherent emission are satisfied. The second model invokes a radio emission direction reversal in normal pulsars, as has been introduced to interpret the peculiar mode changing phenomenon in PSR B1822-09. In this picture, our line of sight misses the main radio emission beam of RRATs but happens to sweep the emission beam when the radio emission direction is reversed. RRATs are therefore the other half of the normal ``nulling'' pulsars. We suggest that X-ray observations can provide clues to differentiate these two possibilities. \\ ( http://arXiv.org/abs/astro-ph/0601063 , 8kb) From owner-public@setileague.org Thu Jan 5 10:32:14 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.3 required=5.5 tests=MSGID_FROM_MTA_HEADER, PLING_QUERY autolearn=no version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k05IWC3x018759 for ; Thu, 5 Jan 2006 10:32:13 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id NAA25423 for public-list; Thu, 5 Jan 2006 13:19:45 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f2.bay114.hotmail.com [65.54.169.12]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id NAA25419; Thu, 5 Jan 2006 13:19:42 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 5 Jan 2006 10:19:10 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Thu, 05 Jan 2006 18:19:09 GMT X-Originating-IP: [24.39.94.195] 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: Earth to Mars in 3 hours? Eleven light years in just 80 days?! Date: Thu, 05 Jan 2006 13:19:09 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 05 Jan 2006 18:19:10.0350 (UTC) FILETIME=[86090AE0:01C61224] Sender: owner-public@setileague.org Precedence: bulk The news item - a quote: "The theoretical engine works by creating an intense magnetic field that, according to ideas first developed by the late scientist Burkhard Heim in the 1950s, would produce a gravitational field and result in thrust for a spacecraft. "Also, if a large enough magnetic field was created, the craft would slip into a different dimension, where the speed of light is faster, allowing incredible speeds to be reached. Switching off the magnetic field would result in the engine reappearing in our current dimension." http://news.scotsman.com/scitech.cfm?id=16902006 The actual paper: http://www.uibk.ac.at/c/cb/cb26/heim/theorie_raumfahrt/hqtforspacepropphysicsaip2005.pdf Is it for real? Is it a load of hokum? Does this mean we will have the USS Enterprise far sooner than once thought? Will ETI with interstellar warships star arriving soon? I report - you decide. From owner-public@setileague.org Thu Jan 5 15:52:05 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k05Nq5N9020585 for ; Thu, 5 Jan 2006 15:52:05 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id SAA02982 for public-list; Thu, 5 Jan 2006 18:47:42 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav1.bay114.hotmail.com [65.54.169.73]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id SAA02978; Thu, 5 Jan 2006 18:47:39 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Thu, 5 Jan 2006 15:47:08 -0800 Message-ID: Received: from 129.44.237.167 by BAY114-DAV1.phx.gbl with DAV; Thu, 05 Jan 2006 23:47:07 +0000 X-Originating-IP: [129.44.237.167] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: Half a Dozen Stars Born in Milky Way Every Year Date: Thu, 5 Jan 2006 18:47:13 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_008B_01C61228.7161E270" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MIMEOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Thu, 5 Jan 2006 18:47:13 -0500 X-OriginalArrivalTime: 05 Jan 2006 23:47:08.0640 (UTC) FILETIME=[5735CE00:01C61252] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_008B_01C61228.7161E270 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable Science/Astronomy: * Half a Dozen Stars Born in Milky Way Every Year=20 http://www.space.com/scienceastronomy/060104_star_birth.html= Astronomers have the best evidence yet pinning down how just many stars = form in our galaxy every year: about half a dozen. * Reacting to Disaster=20 http://www.space.com/searchforlife/seti_vakoch_react_060105.html The scenario is familiar from Hollywood blockbusters like Armageddon and = Deep Impact. A massive asteroid-perhaps ten miles in diameter-is headed = straight for Earth. An all-out effort to deflect it is mounted. If the = mission succeeds, civilization as we know it will continue.=20 ------=_NextPart_000_008B_01C61228.7161E270 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
Science/Astronomy:

* Half a Dozen Stars Born in Milky Way = Every Year=20

* Reacting to Disaster

http://www.space.com/searchforlife/seti_vakoch_react_060105.htm= l

The=20 scenario is familiar from Hollywood blockbusters like Armageddon and = Deep=20 Impact. A massive asteroid-perhaps ten miles in diameter-is headed = straight for=20 Earth. An all-out effort to deflect it is mounted. If the mission = succeeds,=20 civilization as we know it will continue.
 
------=_NextPart_000_008B_01C61228.7161E270-- From owner-public@setileague.org Fri Jan 6 11:37:02 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k06Jb2cP026603 for ; Fri, 6 Jan 2006 11:37:02 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id OAA29973 for public-list; Fri, 6 Jan 2006 14:31:20 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f11.bay114.hotmail.com [65.54.169.21]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id OAA29969; Fri, 6 Jan 2006 14:31:18 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 6 Jan 2006 11:30:46 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Fri, 06 Jan 2006 19:30:45 GMT X-Originating-IP: [24.39.94.195] 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: MESSENGER Sets Record for Space Laser Communication Date: Fri, 06 Jan 2006 14:30:45 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 06 Jan 2006 19:30:46.0119 (UTC) FILETIME=[B0ED1F70:01C612F7] Sender: owner-public@setileague.org Precedence: bulk Record Set for Space Laser Communication http://www.space.com/missionlaunches/060104_laser_comm.html In a cosmic version of laser tag, NASA's MESSENGER spacecraft and an Earth-based observatory successfully exchanged laser pulses with each other while millions of miles apart. From owner-public@setileague.org Fri Jan 6 12:18:48 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k06KIlYg026895 for ; Fri, 6 Jan 2006 12:18:48 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id PAA01015 for public-list; Fri, 6 Jan 2006 15:13:14 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-f21.bay114.hotmail.com [65.54.169.31]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id PAA01011; Fri, 6 Jan 2006 15:13:11 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 6 Jan 2006 12:12:40 -0800 Message-ID: Received: from 65.54.169.200 by by114fd.bay114.hotmail.msn.com with HTTP; Fri, 06 Jan 2006 20:12:39 GMT X-Originating-IP: [24.39.94.195] 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: ID in the CMB? Date: Fri, 06 Jan 2006 15:12:39 -0500 Mime-Version: 1.0 Content-Type: text/plain; format=flowed X-OriginalArrivalTime: 06 Jan 2006 20:12:40.0556 (UTC) FILETIME=[8BA5C2C0:01C612FD] Sender: owner-public@setileague.org Precedence: bulk This is from the latest Sky & Telescope News Bulletin, of all places. LOOKING FOR A CREATOR'S CALLING CARD If our universe was purposefully created -- perhaps by a deity or an advanced civilization in another universe -- could the creator have left a calling card in the microwave background? The idea is not as crazy as it seems. Cosmologists such as Andre Linde (Stanford University) and Alan Guth (MIT) have speculated that an advanced civilization could, in principle, cook up a new universe in a lab by concentrating huge quantities of energy into a tiny volume of space.... In a paper posted on astro-ph, physicists Stephen Hsu (University of Oregon) and Anthony Zee (University of California, Santa Barbara) come up with an alternative idea: astronomers could look for an artificial message from the creator in the cosmic microwave background (CMB) -- the afterglow of the Big Bang.... http://SkyandTelescope.com/news/article_1647_1.asp From owner-public@setileague.org Fri Jan 6 15:40:58 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=none autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k06NewW9027906 for ; Fri, 6 Jan 2006 15:40:58 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id SAA05566 for public-list; Fri, 6 Jan 2006 18:36:07 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from web81703.mail.mud.yahoo.com (web81703.mail.mud.yahoo.com [68.142.199.167]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with SMTP id SAA05552 for ; Fri, 6 Jan 2006 18:36:03 -0500 (EST) Received: (qmail 99751 invoked by uid 60001); 6 Jan 2006 23:35:32 -0000 DomainKey-Signature: a=rsa-sha1; q=dns; c=nofws; s=s1024; d=sbcglobal.net; h=Message-ID:Received:Date:From:Subject:To:Cc:In-Reply-To:MIME-Version:Content-Type:Content-Transfer-Encoding; b=zOZjLUPlovdvTlJJrvXyGMXlqfXzPMbBkEUpS9k8H0Ev8qQJcRwcSrhdTSzHnGz2/kBtmUOuRQCIOK5xPPmIKygXloK1c9Wmny+P3K+3glybFpI6j8ZiKndV0vgMwDeAmh4CJyypIY+yQbMHqa6dv/ov5Yv0jntwCTxnM+YACpg= ; Message-ID: <20060106233532.99749.qmail@web81703.mail.mud.yahoo.com> Received: from [69.183.163.246] by web81703.mail.mud.yahoo.com via HTTP; Fri, 06 Jan 2006 15:35:32 PST Date: Fri, 6 Jan 2006 15:35:32 -0800 (PST) From: David Ocame Subject: Re: SETI public: ID in the CMB? To: public@setileague.org Cc: bioastro@setileague.org In-Reply-To: MIME-Version: 1.0 Content-Type: text/plain; charset=iso-8859-1 Content-Transfer-Encoding: 8bit Sender: owner-public@setileague.org Precedence: bulk Actually, this is not a new idea. As far as I can tell, James N. Gardner first put forth this hypothesis in his book, "Biocosm", first published in 2003 by Inner Ocean Publishing. Now, I am not keen on the idea of mixing intelligent design in the same sentence with science. I don't think Gardner meant for this to happen either. Gardner said that it is the purpose of life in a universe to produce "baby universes" in much the same way as Hsu and Zee suggest. In this way, information would be transmitted from the parent to the offspring universe(s)by virtue of the "cooking" conditions (recipe). But, the first steps before that could happen involved life becoming co-terminus with all the cosmos. In light of all the problems that intelligent design philosophy has been causing of late, it might be a good idea to take another look at these writings. Dave Ocame --- LARRY KLAES wrote: > This is from the latest Sky & Telescope News > Bulletin, of all places. > > LOOKING FOR A CREATOR'S CALLING CARD > > If our universe was purposefully created -- perhaps > by a deity or an > advanced civilization in another universe -- could > the creator have left a > calling card in the microwave background? > > The idea is not as crazy as it seems. Cosmologists > such as Andre Linde > (Stanford University) and Alan Guth (MIT) have > speculated that an advanced > civilization could, in principle, cook up a new > universe in a lab by > concentrating huge quantities of energy into a tiny > volume of space.... > > In a paper posted on astro-ph, physicists Stephen > Hsu (University of > Oregon) and Anthony Zee (University of California, > Santa Barbara) come up > with an alternative idea: astronomers could look for > an artificial message > from the creator in the cosmic microwave background > (CMB) -- the afterglow > of the Big Bang.... > > http://SkyandTelescope.com/news/article_1647_1.asp > > > *********************************** *********************************** Dave Ocame, N1YVV Awards Chair The SETILeague, Inc www.setileague.org Stony Creek Observatory FN31og -72.834 longitude 41.272 latitude Member: The SETILeague, Inc. and, The Society for Amateur Radio Astronomy (SARA) and, The Planetary Society ****I'm not dead, yet!**** From owner-public@setileague.org Fri Jan 6 18:38:30 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k072cTlJ028854 for ; Fri, 6 Jan 2006 18:38:30 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id VAA09551 for public-list; Fri, 6 Jan 2006 21:34:46 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav11.bay114.hotmail.com [65.54.169.83]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id VAA09547; Fri, 6 Jan 2006 21:34:44 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 6 Jan 2006 18:34:12 -0800 Message-ID: Received: from 71.123.28.57 by BAY114-DAV11.phx.gbl with DAV; Sat, 07 Jan 2006 02:34:12 +0000 X-Originating-IP: [71.123.28.57] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: And the Miguel Alcubierre Warp Drive of 1994 Date: Fri, 6 Jan 2006 21:34:11 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_0071_01C61308.EEA9A840" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Fri, 6 Jan 2006 21:34:11 -0500 X-OriginalArrivalTime: 07 Jan 2006 02:34:12.0871 (UTC) FILETIME=[D887D170:01C61332] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_0071_01C61308.EEA9A840 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable A physicist named Miguel Alcubierre came up with his own Warp Drive = concept in 1994: http://en.wikipedia.org/wiki/Alcubierre_drive The paper: http://www.arxiv.org/abs/gr-qc/0009013 http://news.bbc.co.uk/1/hi/sci/tech/364496.stm ------=_NextPart_000_0071_01C61308.EEA9A840 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
A physicist named Miguel Alcubierre came up with his own Warp Drive = concept=20 in 1994:

http://en.wikipedia.org/wiki/Alcubierre_drive

= The=20 paper:

http://www.arxiv.org/abs/gr-qc/0009013

http://news.bbc.co.uk/1/hi/sci/tech/364496.stm
------=_NextPart_000_0071_01C61308.EEA9A840-- From owner-public@setileague.org Fri Jan 6 20:04:44 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k0744iZX030000 for ; Fri, 6 Jan 2006 20:04:44 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id WAA11674 for public-list; Fri, 6 Jan 2006 22:59:38 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav2.bay114.hotmail.com [65.54.169.74]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id WAA11670; Fri, 6 Jan 2006 22:59:35 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 6 Jan 2006 19:59:04 -0800 Message-ID: Received: from 71.123.28.57 by BAY114-DAV2.phx.gbl with DAV; Sat, 07 Jan 2006 03:59:03 +0000 X-Originating-IP: [71.123.28.57] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: 2 papers Date: Fri, 6 Jan 2006 22:59:02 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_020A_01C61314.C93A6980" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Fri, 6 Jan 2006 22:59:02 -0500 X-OriginalArrivalTime: 07 Jan 2006 03:59:04.0228 (UTC) FILETIME=[B3373E40:01C6133E] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_020A_01C61314.C93A6980 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable Paper: astro-ph/0601092=20 Date: Wed, 4 Jan 2006 23:56:24 GMT (66kb)=20 Title: Resolving the Surfaces of Extrasolar Planets With Secondary = Eclipse=20 Light Curves Authors: Peter K. G. Williams, David Charbonneau, Curtis S. Cooper, Adam = P.=20 Showman, Jonathan J. Fortney Comments: AASTeX 5.2, 22 pages, 5 figures, submitted to ApJ=20 \\=20 We present a method that employs the secondary eclipse light curves of=20 transiting extrasolar planets to probe the spatial variation of their = thermal=20 emission. This technique permits an observer to resolve the surface of = the=20 planet without needing to isolate its light from that of the central = star. We=20 evaluate the feasibility of this technique for the HD 209458 system by = first=20 modeling the secondary eclipse light curves that would result from = several=20 representations of the planetary emission and then simulating the noise=20 properties of observations of this signal with the Spitzer Space = Telescope=20 Infrared Array Camera (IRAC). We consider two representations of the = planetary=20 thermal emission: a simple parameterized model, and the results of a = dynamical=20 simulation of the planetary atmosphere previously published by Cooper &=20 Showman. We find that observations of the secondary eclipse light curve = are=20 most sensitive to the longitudinal contrast in the emission of the = planetary=20 hemisphere visible near opposition. We quantify this signal with a = parameter,=20 the "uniform time offset," which measures the time delay between the = observed=20 secondary eclipse and that of a simulated, uniformly-emitting planet. We = compare the predicted amplitude of this parameter for HD 209458b with = the=20 precision with which IRAC could measure it. We find that IRAC = observations at=20 3.6 um of a single secondary eclipse should permit sufficient precision = to test=20 the Cooper & Showman model of the planetary atmosphere. We quantify the=20 signal-to-noise ratio for this offset in the remaining IRAC bands and = find that=20 a modest improvement in photometric precision should permit similarly = robust=20 detections. \\ ( http://arXiv.org/abs/astro-ph/0601092 , 66kb) Paper: astro-ph/0601059=20 Date: Tue, 3 Jan 2006 23:14:48 GMT (403kb)=20 Title: Suppressing Speckle Noise for Simultaneous Differential = Extrasolar=20 Planet Imaging (SDI) at the VLT and MMT Authors: Beth A. Biller, Laird M. Close, Rainer Lenzen, Wolfgang = Brandner,=20 Donald McCarthy, Eric Nielsen, Stephan Kellner, and Markus Hartung Comments: 5 pages, 3 figures, 1 table. Presented at IAU Colloquium 200, = Direct=20 Imaging of Exoplanets: Science and Techniques=20 \\=20 We discuss the instrumental and data reduction techniques used to = suppress=20 speckle noise with the Simultaneous Differential Imager (SDI) = implemented at=20 the VLT and the MMT. SDI uses a double Wollaston prism and a quad filter = to=20 take 4 identical images simultaneously at 3 wavelengths surrounding the = 1.62 um=20 methane bandhead found in the spectrum of cool brown dwarfs and gas = giants. By=20 performing a difference of images in these filters, speckle noise from = the=20 primary can be significantly attenuated, resulting in photon noise = limited data=20 past 0.5''. Non-trivial data reduction tools are necessary to pipeline = the=20 simultaneous differential imaging. Here we discuss a custom algorithm=20 implemented in IDL to perform this reduction. The script performs basic = data=20 reduction tasks but also precisely aligns images taken in each of the = filters=20 using a custom shift and subtract routine. In our survey of nearby young = stars=20 at the VLT and MMT (see Biller et al., this conference), we achieved H = band=20 contrasts >25000 (5 sigma Delta F1(1.575 um) > 10.0 mag, Delta H > 11.5 = mag for=20 a T6 spectral type object) at a separation of 0.5" from the primary = star. We=20 believe that our SDI images are among the highest contrast astronomical = images=20 ever made from ground or space for methane rich companions. \\ ( http://arXiv.org/abs/astro-ph/0601059 , 403kb) ------=_NextPart_000_020A_01C61314.C93A6980 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
Paper: = astro-ph/0601092=20
Date: Wed, 4 Jan 2006 23:56:24 GMT (66kb)=20

Title: Resolving the Surfaces of Extrasolar Planets With Secondary = Eclipse=20
Light Curves

Authors: Peter K. G. Williams, David Charbonneau, Curtis S. Cooper, = Adam P.=20
Showman, Jonathan J. Fortney

Comments: AASTeX 5.2, 22 pages, 5 figures, submitted to ApJ
\\ =
We=20 present a method that employs the secondary eclipse light curves of=20
transiting extrasolar planets to probe the spatial variation of = their=20 thermal
emission. This technique permits an observer to resolve the = surface=20 of the
planet without needing to isolate its light from that of the = central=20 star. We
evaluate the feasibility of this technique for the HD = 209458 system=20 by first
modeling the secondary eclipse light curves that would = result from=20 several
representations of the planetary emission and then = simulating the=20 noise
properties of observations of this signal with the Spitzer = Space=20 Telescope
Infrared Array Camera (IRAC). We consider two = representations of=20 the planetary
thermal emission: a simple parameterized model, and = the=20 results of a dynamical
simulation of the planetary atmosphere = previously=20 published by Cooper &
Showman. We find that observations of the=20 secondary eclipse light curve are
most sensitive to the longitudinal = contrast in the emission of the planetary
hemisphere visible near=20 opposition. We quantify this signal with a parameter,
the "uniform = time=20 offset," which measures the time delay between the observed =
secondary=20 eclipse and that of a simulated, uniformly-emitting planet. We =
compare the=20 predicted amplitude of this parameter for HD 209458b with the =
precision with=20 which IRAC could measure it. We find that IRAC observations at
3.6 = um of a=20 single secondary eclipse should permit sufficient precision to test =
the=20 Cooper & Showman model of the planetary atmosphere. We quantify the=20
signal-to-noise ratio for this offset in the remaining IRAC bands = and find=20 that
a modest improvement in photometric precision should permit = similarly=20 robust
detections.

\\ ( http://arXiv.org/abs/astro-ph/0601092 ,=20 66kb)

 
Paper: astro-ph/0601059 =
Date: Tue,=20 3 Jan 2006 23:14:48 GMT (403kb)

Title: Suppressing Speckle Noise for Simultaneous = Differential Extrasolar
Planet Imaging (SDI) at the VLT and MMT

Authors: Beth A. Biller, Laird M. Close, Rainer = Lenzen,=20 Wolfgang Brandner,
Donald McCarthy, Eric Nielsen, Stephan Kellner, = and=20 Markus Hartung

Comments: 5 pages, 3 figures, 1 table. Presented = at IAU=20 Colloquium 200, Direct
Imaging of Exoplanets: Science and Techniques =
\\=20
We discuss the instrumental and data reduction techniques used to = suppress=20
speckle noise with the Simultaneous Differential Imager (SDI) = implemented at=20
the VLT and the MMT. SDI uses a double Wollaston prism and a quad = filter to=20
take 4 identical images simultaneously at 3 wavelengths surrounding = the 1.62=20 um
methane bandhead found in the spectrum of cool brown dwarfs and = gas=20 giants. By
performing a difference of images in these filters, = speckle noise=20 from the
primary can be significantly attenuated, resulting in = photon noise=20 limited data
past 0.5''. Non-trivial data reduction tools are = necessary to=20 pipeline the
simultaneous differential imaging. Here we discuss a = custom=20 algorithm
implemented in IDL to perform this reduction. The script = performs=20 basic data
reduction tasks but also precisely aligns images taken in = each of=20 the filters
using a custom shift and subtract routine. In our survey = of=20 nearby young stars
at the VLT and MMT (see Biller et al., this = conference),=20 we achieved H band
contrasts >25000 (5 sigma Delta F1(1.575 um) = > 10.0=20 mag, Delta H > 11.5 mag for
a T6 spectral type object) at a = separation of=20 0.5" from the primary star. We
believe that our SDI images are among = the=20 highest contrast astronomical images
ever made from ground or space = for=20 methane rich companions.

\\ ( http://arXiv.org/abs/astro-ph/0601059 , = 403kb)

------=_NextPart_000_020A_01C61314.C93A6980-- From owner-public@setileague.org Fri Jan 6 20:23:46 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k074NjpS030082 for ; Fri, 6 Jan 2006 20:23:45 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id XAA12165 for public-list; Fri, 6 Jan 2006 23:21:04 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav1.bay114.hotmail.com [65.54.169.73]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id XAA12159; Fri, 6 Jan 2006 23:21:01 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Fri, 6 Jan 2006 20:20:30 -0800 Message-ID: Received: from 71.123.28.57 by BAY114-DAV1.phx.gbl with DAV; Sat, 07 Jan 2006 04:20:29 +0000 X-Originating-IP: [71.123.28.57] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: High-Resolution Simulations of a Moon-Forming Impact and Post-Impact Evolution Date: Fri, 6 Jan 2006 23:20:28 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_0228_01C61317.C7F55F00" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Fri, 6 Jan 2006 23:20:28 -0500 X-OriginalArrivalTime: 07 Jan 2006 04:20:30.0204 (UTC) FILETIME=[B1B79BC0:01C61341] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_0228_01C61317.C7F55F00 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable Paper: astro-ph/0601094=20 Date: Thu, 5 Jan 2006 03:34:52 GMT (296kb)=20 Title: High-Resolution Simulations of a Moon-Forming Impact and = Post-Impact=20 Evolution Authors: Keiichi Wada (1), Eiichiro Kokubo (1) and Junichiro Makino (2) = ((1)=20 National Astronomical Observatory of Japan, (2) University of Tokyo) Comments: ApJ 638, Feb. 20 in press=20 \\=20 In order to examine the ``giant impact hypothesis'' for the Moon = formation,=20 we run the first grid-based, high-resolution hydrodynamic simulations = for an=20 impact between proto-Earth and a proto-planet. The spatial resolution = for the=20 impact-generated disk is greatly improved from previous particle-based=20 simulations. This allows us to explore fine structures of a = circumterrestrial=20 debris disk and its long-term evolution. We find that in order to form a = debris=20 disk from which a lunar-sized satellite can be accumulated, the impact = must=20 result in a disk of mostly liquid or solid debris, where pressure is not = effective, well before the accumulation process starts. If the debris is = dominated by vapor gas, strong spiral shocks are generated, and = therefore the=20 circumterrestrial disk cannot survive more than several days. This = suggests=20 that there could be an appropriate mass range for terrestrial planets to = harbor=20 a large moon as a result of giant impacts, since vaporization during an = impact=20 depends on the impact energy. \\ ( http://arXiv.org/abs/astro-ph/0601094 , 296kb) ------=_NextPart_000_0228_01C61317.C7F55F00 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
Paper: = astro-ph/0601094=20
Date: Thu, 5 Jan 2006 03:34:52 GMT (296kb)=20

Title: High-Resolution Simulations of a Moon-Forming Impact and = Post-Impact=20
Evolution

Authors: Keiichi Wada (1), Eiichiro Kokubo (1) and Junichiro Makino = (2) ((1)=20
National Astronomical Observatory of Japan, (2) University of = Tokyo)

Comments: ApJ 638, Feb. 20 in press
\\
In order to examine = the=20 ``giant impact hypothesis'' for the Moon formation,
we run the first = grid-based, high-resolution hydrodynamic simulations for an
impact = between=20 proto-Earth and a proto-planet. The spatial resolution for the=20
impact-generated disk is greatly improved from previous = particle-based=20
simulations. This allows us to explore fine structures of a=20 circumterrestrial
debris disk and its long-term evolution. We find = that in=20 order to form a debris
disk from which a lunar-sized satellite can = be=20 accumulated, the impact must
result in a disk of mostly liquid or = solid=20 debris, where pressure is not
effective, well before the = accumulation=20 process starts. If the debris is
dominated by vapor gas, strong = spiral=20 shocks are generated, and therefore the
circumterrestrial disk = cannot=20 survive more than several days. This suggests
that there could be an = appropriate mass range for terrestrial planets to harbor
a large = moon as a=20 result of giant impacts, since vaporization during an impact
depends = on the=20 impact energy.

\\ ( http://arXiv.org/abs/astro-ph/0601094 , 296kb)

------=_NextPart_000_0228_01C61317.C7F55F00-- From owner-public@setileague.org Sat Jan 7 09:52:57 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k07Hquh9014602 for ; Sat, 7 Jan 2006 09:52:56 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id MAA29585 for public-list; Sat, 7 Jan 2006 12:49:18 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav4.bay114.hotmail.com [65.54.169.76]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id MAA29579; Sat, 7 Jan 2006 12:49:15 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Sat, 7 Jan 2006 09:48:43 -0800 Message-ID: Received: from 129.44.209.129 by BAY114-DAV4.phx.gbl with DAV; Sat, 07 Jan 2006 17:48:42 +0000 X-Originating-IP: [129.44.209.129] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: 2 papers on space cloud contents Date: Sat, 7 Jan 2006 12:48:34 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_0049_01C61388.ABFA5EB0" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Sat, 7 Jan 2006 12:48:34 -0500 X-OriginalArrivalTime: 07 Jan 2006 17:48:43.0662 (UTC) FILETIME=[9A1212E0:01C613B2] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_0049_01C61388.ABFA5EB0 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable Paper: astro-ph/0601077=20 Date: Wed, 4 Jan 2006 19:22:27 GMT (361kb)=20 Title: Hubble Space Telescope NICMOS Polarization Measurements of OMC-1 Authors: Janet P. Simpson (1 and 2), Sean W. J. Colgan (1), Edwin F. = Erickson=20 (1), Michael G. Burton (3), and A. S. B. Schultz (2) ((1) NASA Ames = Research=20 Center, (2) SETI Institute, (3) University of New South Wales) Comments: 41 pages, 8 figures, 4 tables, to appear in The Astrophysical = Journal=20 \\=20 We present 2micron polarization measurements of positions in the BN = region of=20 the Orion Molecular Cloud (OMC-1) made with NICMOS Camera 2 (0.2'' = resolution)=20 on HST. Our results are as follows: BN is sim 29% polarized by dichroic=20 absorption and appears to be the illuminating source for most of the = nebulosity=20 to its north and up to sim 5'' to its south. Although the stars are = probably=20 all polarized by dichroic absorption, there are a number of compact, but = non-point-source, objects that could be polarized by a combination of = both=20 dichroic absorption and local scattering of star light. We identify = several=20 candidate YSOs, including an approximately edge-on bipolar YSO 8.7'' = east of=20 BN, and a deeply-embedded variable star. Additional strongly polarized = sources=20 are IRc2-B, IRc2-D, and IRc7, all of which are obviously self-luminous = at=20 mid-infrared wavelengths and may be YSOs. None of these is a reflection = nebula=20 illuminated by a star located near radio source I, as was previously = suggested.=20 Other IRc sources are clearly reflection nebulae: IRc3 appears to be=20 illuminated by IRc2-B or a combination of the IRc2 sources, and IRc4 and = IRc5=20 appear to be illuminated by an unseen star in the vicinity of radio = source I,=20 or by Star n or IRc2-A. Trends in the magnetic field direction are = inferred=20 from the polarization of the 26 stars that are bright enough to be seen = as=20 NICMOS point sources. The most polarized star has a polarization = position angle=20 different from its neighbors by sim 40^o, but in agreement with the = grain=20 alignment inferred from millimeter polarization measurements of the cold = dust=20 cloud in the southern part of OMC-1. \\ ( http://arXiv.org/abs/astro-ph/0601077 , 361kb) Paper: astro-ph/0601078=20 Date: Wed, 4 Jan 2006 13:43:02 GMT (659kb)=20 Title: Ammonia in Infrared Dark Clouds Authors: Thushara Pillai (1), Friedrich Wyrowski (1), Sean J. Carey (2), = Karl=20 M. Menten (1) ((1)Max-Planck-Institut fuer Radioastronomie, Bonn = (2)Spitzer=20 Science Center, California Institute of Technology) Comments: 17 pages, 11 figures, in press in Astronomy & Astrophysics=20 \\=20 Infrared Dark Clouds appear to be the long sought population of cold and = dense aggregations with the potential of harbouring the earliest stages = of=20 massive star formation. Up to now there has been no systematic study on = the=20 temperature distribution, velocity fields, chemical and physical state = toward=20 this new cloud population. Knowing these properties is crucial for=20 understanding the presence, absence and the very potential of star = formation.=20 The present paper aims at addressing these questions. We analyse = temperature=20 structures and velocity fields and gain information on their chemical=20 evolution. The gas emission is remarkably coextensive with the = extinction seen=20 at infrared wavelengths and with the submillimeter dust emission. Our = results=20 show that IRDCs are on average cold (T < 20 K) and have variations among = the=20 different cores. IRDC cores are in virial equilibrium, are massive (M > = 100=20 M_sun), highly turbulent (1 -- 3 km/s) and exhibit significant velocity=20 structure (variations around 1 -- 2 km/s over the cloud). We find an = increasing=20 trend in temperature from IRDCs with high ammonia column density to high = mass=20 protostellar objects and hot core/Ultracompact Hii regions stages of = early warm=20 high-mass star formation while linewidths of IRDCs are smaller. On the = basis of=20 this sample, we infer that while active star formation is not yet = pervasive in=20 most IRDCs, local condensations might collapse in the future or have = already=20 begun forming stars. \\ ( http://arXiv.org/abs/astro-ph/0601078 , 659kb) ------=_NextPart_000_0049_01C61388.ABFA5EB0 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
Paper: = astro-ph/0601077=20
Date: Wed, 4 Jan 2006 19:22:27 GMT (361kb)=20

Title: Hubble Space Telescope NICMOS Polarization Measurements of = OMC-1

Authors: Janet P. Simpson (1 and 2), Sean W. J. Colgan (1), Edwin F. = Erickson=20
(1), Michael G. Burton (3), and A. S. B. Schultz (2) ((1) NASA Ames = Research=20
Center, (2) SETI Institute, (3) University of New South Wales)

Comments: 41 pages, 8 figures, 4 tables, to appear in The = Astrophysical=20 Journal
\\
We present 2micron polarization measurements of = positions in=20 the BN region of
the Orion Molecular Cloud (OMC-1) made with NICMOS = Camera 2=20 (0.2'' resolution)
on HST. Our results are as follows: BN is sim 29% = polarized by dichroic
absorption and appears to be the illuminating = source=20 for most of the nebulosity
to its north and up to sim 5'' to its = south.=20 Although the stars are probably
all polarized by dichroic = absorption, there=20 are a number of compact, but
non-point-source, objects that could be = polarized by a combination of both
dichroic absorption and local = scattering=20 of star light. We identify several
candidate YSOs, including an=20 approximately edge-on bipolar YSO 8.7'' east of
BN, and a = deeply-embedded=20 variable star. Additional strongly polarized sources
are IRc2-B, = IRc2-D, and=20 IRc7, all of which are obviously self-luminous at
mid-infrared = wavelengths=20 and may be YSOs. None of these is a reflection nebula
illuminated by = a star=20 located near radio source I, as was previously suggested.
Other IRc = sources=20 are clearly reflection nebulae: IRc3 appears to be
illuminated by = IRc2-B or=20 a combination of the IRc2 sources, and IRc4 and IRc5
appear to be=20 illuminated by an unseen star in the vicinity of radio source I,
or = by Star=20 n or IRc2-A. Trends in the magnetic field direction are inferred =
from the=20 polarization of the 26 stars that are bright enough to be seen as =
NICMOS=20 point sources. The most polarized star has a polarization position angle =
different from its neighbors by sim 40^o, but in agreement with the = grain=20
alignment inferred from millimeter polarization measurements of the = cold=20 dust
cloud in the southern part of OMC-1.

\\ ( http://arXiv.org/abs/astro-ph/0601077 , 361kb)

Paper: = astro-ph/0601078=20
Date: Wed, 4 Jan 2006 13:43:02 GMT (659kb)=20

Title: Ammonia in Infrared Dark Clouds

Authors: Thushara Pillai (1), Friedrich Wyrowski (1), Sean J. Carey = (2), Karl=20
M. Menten (1) ((1)Max-Planck-Institut fuer Radioastronomie, Bonn = (2)Spitzer=20
Science Center, California Institute of Technology)

Comments: 17 pages, 11 figures, in press in Astronomy & = Astrophysics=20
\\
Infrared Dark Clouds appear to be the long sought population = of cold=20 and
dense aggregations with the potential of harbouring the earliest = stages=20 of
massive star formation. Up to now there has been no systematic = study on=20 the
temperature distribution, velocity fields, chemical and physical = state=20 toward
this new cloud population. Knowing these properties is = crucial for=20
understanding the presence, absence and the very potential of star=20 formation.
The present paper aims at addressing these questions. We = analyse=20 temperature
structures and velocity fields and gain information on = their=20 chemical
evolution. The gas emission is remarkably coextensive with = the=20 extinction seen
at infrared wavelengths and with the submillimeter = dust=20 emission. Our results
show that IRDCs are on average cold (T < 20 = K) and=20 have variations among the
different cores. IRDC cores are in virial=20 equilibrium, are massive (M > 100
M_sun), highly turbulent (1 -- = 3 km/s)=20 and exhibit significant velocity
structure (variations around 1 -- 2 = km/s=20 over the cloud). We find an increasing
trend in temperature from = IRDCs with=20 high ammonia column density to high mass
protostellar objects and = hot=20 core/Ultracompact Hii regions stages of early warm
high-mass star = formation=20 while linewidths of IRDCs are smaller. On the basis of
this sample, = we infer=20 that while active star formation is not yet pervasive in
most IRDCs, = local=20 condensations might collapse in the future or have already
begun = forming=20 stars.

\\ ( http://arXiv.org/abs/astro-ph/0601078 , 659kb)

------=_NextPart_000_0049_01C61388.ABFA5EB0-- From owner-public@setileague.org Sat Jan 7 12:23:00 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k07KN0JG015330 for ; Sat, 7 Jan 2006 12:23:00 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id PAA03137 for public-list; Sat, 7 Jan 2006 15:20:13 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav15.bay114.hotmail.com [65.54.169.87]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id PAA03133; Sat, 7 Jan 2006 15:20:10 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Sat, 7 Jan 2006 12:19:38 -0800 Message-ID: Received: from 129.44.209.129 by BAY114-DAV15.phx.gbl with DAV; Sat, 07 Jan 2006 20:19:38 +0000 X-Originating-IP: [129.44.209.129] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: Stardust@Home Date: Sat, 7 Jan 2006 15:19:37 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_00C3_01C6139D.C5B6E9D0" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Sat, 7 Jan 2006 15:19:37 -0500 X-OriginalArrivalTime: 07 Jan 2006 20:19:38.0797 (UTC) FILETIME=[AF5A05D0:01C613C7] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_00C3_01C6139D.C5B6E9D0 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable A distributed search by volunteers for interstellar dust in the Stardust = interstellar dust collector.=20 In January 2004, the Stardust spacecraft flew through the coma of comet = Wild2 and captured thousands of cometary dust grains in special aerogel = collectors. Two years later, in January 2006, Stardust will return these = dust grains --- the first sample return from a solid solar-system body = beyond the Moon --- to Earth. But Stardust carries an equally important = payload on the opposite side of the cometary collector: the first = samples of contemporary interstellar dust ever collected. As well as = being the first mission to return samples from a comet, Stardust is the = first sample return mission from the Galaxy. But finding the incredibly = tiny interstellar dust impacts in the Stardust Interstellar Dust = Collector (SIDC) will be extremely difficult. We are seeking volunteers to help us to search for these tiny samples of = matter from the galaxy. Volunteers are critical to the success of this = project. Please help us find the first samples of contemporary Stardust = ever collected. http://stardustathome.ssl.berkeley.edu/index.html ------=_NextPart_000_00C3_01C6139D.C5B6E9D0 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
A distributed = search by=20 volunteers for interstellar dust in the Stardust interstellar dust = collector.=20

In January 2004, the Stardust spacecraft flew through the coma of = comet Wild2=20 and captured thousands of cometary dust grains in special aerogel = collectors.=20 Two years later, in January 2006, Stardust will return these dust grains = --- the=20 first sample return from a solid solar-system body beyond the Moon --- = to Earth.=20 But Stardust carries an equally important payload on the opposite side = of the=20 cometary collector: the first samples of contemporary interstellar dust = ever=20 collected. As well as being the first mission to return samples from a = comet,=20 Stardust is the first sample return mission from the Galaxy. But finding = the=20 incredibly tiny interstellar dust impacts in the Stardust Interstellar = Dust=20 Collector (SIDC) will be extremely difficult.

We are seeking volunteers to help us to search for these tiny samples = of=20 matter from the galaxy. Volunteers are critical to the success of this = project.=20 Please help us find the first samples of contemporary Stardust ever=20 collected.

http://stardustathome.ssl.berkeley.edu/index.html

------=_NextPart_000_00C3_01C6139D.C5B6E9D0-- From owner-public@setileague.org Sat Jan 7 12:32:38 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k07KWb2G015401 for ; Sat, 7 Jan 2006 12:32:37 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id PAA03399 for public-list; Sat, 7 Jan 2006 15:30:53 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav3.bay114.hotmail.com [65.54.169.75]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id PAA03395; Sat, 7 Jan 2006 15:30:51 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Sat, 7 Jan 2006 12:30:20 -0800 Message-ID: Received: from 129.44.209.129 by BAY114-DAV3.phx.gbl with DAV; Sat, 07 Jan 2006 20:30:19 +0000 X-Originating-IP: [129.44.209.129] X-Originating-Email: [ljk4@msn.com] X-Sender: ljk4@msn.com From: "LARRY KLAES" To: "setipublic" Cc: "BioAstro" Subject: SETI public: Active Assessment of Active SETI Date: Sat, 7 Jan 2006 15:30:18 -0500 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_00DE_01C6139F.43B23C80" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: MSN 9 X-MimeOLE: Produced By MSN MimeOLE V9.10.0011.1703 Seal-Send-Time: Sat, 7 Jan 2006 15:30:18 -0500 X-OriginalArrivalTime: 07 Jan 2006 20:30:20.0235 (UTC) FILETIME=[2DADB1B0:01C613C9] Sender: owner-public@setileague.org Precedence: bulk This is a multi-part message in MIME format. ------=_NextPart_000_00DE_01C6139F.43B23C80 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable Active Assessment of Active SETI=20 by H. Paul Shuch, Ph.D.=20 Almost since its inception nearly half a century ago, SETI science has = seen its supporters wage a running battle over the question of = transmissions from Earth. Deliberate transmission of signals into space, = sometimes called Active SETI, is justified by its proponents on the = grounds of reciprocity. That is, some argue, we cannot in good = conscience search for signals which we would hope other civilizations = might choose to beam our way, if we ourselves are not willing to = transmit such signals from Earth. The counter-argument involves the = safety, and some would say the very survival, of our planet.=20 Critics to Active SETI point out the dangers of shouting in the jungle. = Radio amateurs in support of Active SETI counter that (1) the cat is = already out of the bag, as we have been inadvertently transmitting to = the stars for a century or so, and (2) if everybody's listening and = nobody calls CQ, the bands will appear dead to all concerned. http://www.setileague.org/editor/sanmarin.htm ------=_NextPart_000_00DE_01C6139F.43B23C80 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
Active = Assessment of Active=20 SETI=20

by H. Paul Shuch, Ph.D.

Almost since its inception nearly half a century ago, SETI science = has seen=20 its supporters wage a running battle over the question of transmissions = from=20 Earth. Deliberate transmission of signals into space, sometimes called = Active=20 SETI, is justified by its proponents on the grounds of reciprocity. That = is,=20 some argue, we cannot in good conscience search for signals which we = would hope=20 other civilizations might choose to beam our way, if we ourselves are = not=20 willing to transmit such signals from Earth. The counter-argument = involves the=20 safety, and some would say the very survival, of our planet.

Critics to Active SETI point out the dangers of shouting in the = jungle. Radio=20 amateurs in support of Active SETI counter that (1) the cat is already = out of=20 the bag, as we have been inadvertently transmitting to the stars for a = century=20 or so, and (2) if everybody's listening and nobody calls CQ, the bands = will=20 appear dead to all concerned.

http://www.setileague.org/editor/sanmarin.htm

------=_NextPart_000_00DE_01C6139F.43B23C80-- From owner-public@setileague.org Sun Jan 8 07:28:34 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k08FSXak020247 for ; Sun, 8 Jan 2006 07:28:34 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id KAA27708 for public-list; Sun, 8 Jan 2006 10:23:49 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from aolrelay01.ipowerweb.com (office207-174.ipowerweb.com [66.235.207.174] (may be forged)) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with SMTP id KAA27701 for ; Sun, 8 Jan 2006 10:23:45 -0500 (EST) Received: (qmail 66704 invoked by uid 0); 9 Jan 2006 07:21:43 -0000 Received: from 66.235.220.224 by aolrelay01.ipowerweb.com (envelope-from , uid 1002) with qmail-scanner-1.25st (clamdscan: 0.87.1/1162. spamassassin: 3.1.0. perlscan: 1.25st. Clear:RC:0(66.235.220.224):SA:0(0.0/5.0):. Processed in 3.302944 secs); 09 Jan 2006 07:21:43 -0000 Received: from unknown (HELO host224.ipowerweb.com) (66.235.220.224) by aolrelay01.ipowerweb.com with SMTP; 9 Jan 2006 07:21:40 -0000 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 1EvcNn-0003HN-UL; Sun, 08 Jan 2006 07:23:00 -0800 Message-ID: <001601c61467$6f695980$887ba8c0@Zeke> From: "James Brown" To: "LARRY KLAES" , "setipublic" Cc: "BioAstro" References: Subject: Re: SETI public: Stardust@Home Date: Sun, 8 Jan 2006 07:23:08 -0800 MIME-Version: 1.0 Content-Type: multipart/alternative; boundary="----=_NextPart_000_0013_01C61424.5FB31D70" X-Priority: 3 X-MSMail-Priority: Normal X-Mailer: Microsoft Outlook Express 6.00.2800.1506 X-MimeOLE: Produced By Microsoft MimeOLE V6.00.2800.1506 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 - 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_0013_01C61424.5FB31D70 Content-Type: text/plain; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable Larry - The URL at the bottom of the page doesn't seem to work. Do you = have a different one? ----- Original Message -----=20 From: LARRY KLAES=20 To: setipublic=20 Cc: BioAstro=20 Sent: Saturday, January 07, 2006 12:19 PM Subject: SETI public: Stardust@Home A distributed search by volunteers for interstellar dust in the = Stardust interstellar dust collector.=20 In January 2004, the Stardust spacecraft flew through the coma of = comet Wild2 and captured thousands of cometary dust grains in special = aerogel collectors. Two years later, in January 2006, Stardust will = return these dust grains --- the first sample return from a solid = solar-system body beyond the Moon --- to Earth. But Stardust carries an = equally important payload on the opposite side of the cometary = collector: the first samples of contemporary interstellar dust ever = collected. As well as being the first mission to return samples from a = comet, Stardust is the first sample return mission from the Galaxy. But = finding the incredibly tiny interstellar dust impacts in the Stardust = Interstellar Dust Collector (SIDC) will be extremely difficult. We are seeking volunteers to help us to search for these tiny samples = of matter from the galaxy. Volunteers are critical to the success of = this project. Please help us find the first samples of contemporary = Stardust ever collected. http://stardustathome.ssl.berkeley.edu/index.html ------=_NextPart_000_0013_01C61424.5FB31D70 Content-Type: text/html; charset="iso-8859-1" Content-Transfer-Encoding: quoted-printable
Larry - The URL at the bottom of the page = doesn't seem to=20 work.  Do you have a different one?
----- Original Message -----
From:=20 LARRY KLAES =
Sent: Saturday, January 07, = 2006 12:19=20 PM
Subject: SETI public: Stardust@Home

A = distributed search by=20 volunteers for interstellar dust in the Stardust interstellar dust = collector.=20

In January 2004, the Stardust spacecraft flew through the coma of = comet=20 Wild2 and captured thousands of cometary dust grains in special = aerogel=20 collectors. Two years later, in January 2006, Stardust will return = these dust=20 grains --- the first sample return from a solid solar-system body = beyond the=20 Moon --- to Earth. But Stardust carries an equally important payload = on the=20 opposite side of the cometary collector: the first samples of = contemporary=20 interstellar dust ever collected. As well as being the first mission = to return=20 samples from a comet, Stardust is the first sample return mission from = the=20 Galaxy. But finding the incredibly tiny interstellar dust impacts in = the=20 Stardust Interstellar Dust Collector (SIDC) will be extremely = difficult.

We are seeking volunteers to help us to search for these tiny = samples of=20 matter from the galaxy. Volunteers are critical to the success of this = project. Please help us find the first samples of contemporary = Stardust ever=20 collected.

http://stardustathome.ssl.berkeley.edu/index.html

------=_NextPart_000_0013_01C61424.5FB31D70-- From owner-public@setileague.org Sun Jan 8 08:43:56 2006 X-Spam-Checker-Version: SpamAssassin 3.1.0 (2005-09-13) on Sentry.net X-Spam-Level: X-Spam-Status: No, score=0.0 required=5.5 tests=HTML_MESSAGE, MSGID_FROM_MTA_HEADER autolearn=failed version=3.1.0 Received: from seti1.setileague.org (seti1.setileague.org [204.176.91.10]) by Sentry.net (8.13.3/8.13.3) with ESMTP id k08GhtTR020559 for ; Sun, 8 Jan 2006 08:43:56 -0800 Received: (from majordom@localhost) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) id LAA29417 for public-list; Sun, 8 Jan 2006 11:40:36 -0500 (EST) X-Authentication-Warning: seti1.setileague.org: majordom set sender to owner-public@seti1.setileague.org using -f Received: from hotmail.com (bay114-dav6.bay114.hotmail.com [65.54.169.78]) by seti1.setileague.org (8.9.3 (PHNE_24419+JAGae58098)/8.9.3) with ESMTP id LAA29413; Sun, 8 Jan 2006 11:40:34 -0500 (EST) Received: from mail pickup service by hotmail.com with Microsoft SMTPSVC; Sun, 8 Jan 2006 08:40:02 -0800 Message-ID: Received: from 129.44.214.10 by BAY114-DAV6.phx.gbl with DAV; Sun, 08 Jan 2006 16:40:02 +0000 X-Originating-IP: [129.44.214.10] X-Originating-Email: [ljk4@msn.com] X