SETI public: Low Luminosity Companions to White Dwarfs

From: LARRY KLAES (ljk4_at_msn.com)
Date: Thu Jun 02 2005 - 05:24:29 PDT

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    Paper: astro-ph/0506017
    Date: Wed, 1 Jun 2005 13:02:54 GMT (862kb)

    Title: Low Luminosity Companions to White Dwarfs

    Authors: J. Farihi, E.E. Becklin, B. Zuckerman
    Comments: 158 pages, 59 figures, 11 tables, accepted to ApJ Supplements
    \\
    This paper presents results of a near-infrared imaging survey for low mass
    stellar and substellar companions to white dwarfs. A wide field proper
    motion
    survey of 261 white dwarfs was capable of directly detecting companions at
    orbital separations between $\sim100$ and 5000 AU with masses as low as 0.05
    $M_{\odot}$, while a deep near field search of 86 white dwarfs was capable
    of
    directly detecting companions at separations between $\sim50$ and 1100 AU
    with
    masses as low as 0.02 $M_{\odot}$. Additionally, all white dwarf targets
    were
    examined for near-infrared excess emission, a technique capable of detecting
    companions at arbitrarily close separations down to masses of 0.05
    $M_{\odot}$.
    No brown dwarf candidates were detected, which implies a brown dwarf
    companion fraction of $<0.5$% for white dwarfs. In contrast, the stellar
    companion fraction of white dwarfs as measured by this survey is 22%,
    uncorrected for bias. Moreover, most of the known and suspected stellar
    companions to white dwarfs are low mass stars whose masses are only slightly
    greater than the masses of brown dwarfs. Twenty previously unknown stellar
    companions were detected, five of which are confirmed or likely white dwarfs
    themselves, while fifteen are confirmed or likely low mass stars.
    Similar to the distribution of cool field dwarfs as a function of spectral
    type, the number of cool unevolved dwarf companions peaks at mid-M type.
    Based
    on the present work, relative to this peak, field L dwarfs appear to be
    roughly
    2-3 times more abundant than companion L dwarfs. Additionally, there is no
    evidence that the initial companion masses have been altered by post main
    sequence binary interactions.

    \\ ( http://arXiv.org/abs/astro-ph/0506017 , 862kb)


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