SETI bioastro: Extrasolar planets and brown dwarfs around A-F type stars

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From: LARRY KLAES (ljk4_at_msn.com)
Date: Sat Sep 10 2005 - 03:19:40 UTC

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    Paper: astro-ph/0509111
    Date: Tue, 6 Sep 2005 06:37:57 GMT (94kb)

    Title: Extrasolar planets and brown dwarfs around A-F type stars. I.
    Performances of radial velocity measurements, first analyses of variations

    Authors: F. Galland, A. M. Lagrange, S. Udry, A. Chelli, F. Pepe, D. Queloz, J.
    L. Beuzit, M. Mayor

    Comments: final version, accepted for publication (A&A)
    \\
    We present the performances of a radial velocity measurement method that we
    developed for A-F type stars. These perfomances are evaluated through an
    extensive set of simulations, together with actual radial velocity observations
    of such stars using the ELODIE and HARPS spectrographs. We report the case of
    stars constant in radial velocity, the example of a binary detection on HD
    48097 (an A2V star, with vsini equal to 90 km/s) and a confirmation of the
    existence of a 3.9 MJup planet orbiting around HD 120136 (Tau Boo). The
    instability strip problem is also discussed. We show that with this method, it
    is in principle possible to detect planets and brown dwarfs around A-F type
    stars, thus allowing further study of the impact of stellar masses on planetary
    system formation over a wider range of stellar masses than is currently done.

    \\ ( http://arXiv.org/abs/astro-ph/0509111 , 94kb)

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    \\
    Paper: astro-ph/0509112
    Date: Tue, 6 Sep 2005 06:56:50 GMT (30kb)

    Title: Extrasolar planets and brown dwarfs around A-F type stars. II. A planet
    found with ELODIE around the F6V star HD 33564 showing a strong infrared
    excess

    Authors: F. Galland, A. M. Lagrange, S. Udry, A. Chelli, F. Pepe, J. L. Beuzit,
    M. Mayor

    Comments: final version, accepted for publication (A&A)
    \\
    We present here the detection of a planet orbiting around the F6V star HD
    33564. The radial velocity measurements, obtained with the ELODIE echelle
    spectrograph at the Haute-Provence Observatory, show a variation with a period
    of 388 days. Assuming a primary mass of 1.25 Mo, the best Keplerian fit to the
    data leads to a minimum mass of 9.1 MJup for the companion. We note that this
    is the most clear detection of a planet around a star showing a strong infrared
    excess.

    \\ ( http://arXiv.org/abs/astro-ph/0509112 , 30kb)

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