SETI public: Discovery of a Planetary-Mass Brown Dwarf with a Circumstellar Disk

From: LARRY KLAES (ljk4_at_msn.com)
Date: Thu Dec 01 2005 - 06:36:13 PST

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    Paper: astro-ph/0511807
    Date: Tue, 29 Nov 2005 21:32:34 GMT (27kb)

    Title: Discovery of a Planetary-Mass Brown Dwarf with a Circumstellar Disk

    Authors: K. L. Luhman, Lucia Adame, Paola D'Alessio, Nuria Calvet, Lee
    Hartmann, S. T. Megeath, and G. G. Fazio

    Comments: 5 pages, accepted to Astrophysical Journal Letters
    \\
    Using the Hubble Space Telescope, the 4 m Blanco telescope at the Cerro
    Tololo Inter-American Observatory, and the Spitzer Space Telescope, we have
    performed deep imaging from 0.8 to 8 um of the southern subcluster in the
    Chamaeleon I star-forming region. In these data, we have discovered an
    object,
    Cha 110913-773444, whose colors and magnitudes are indicative of a very
    low-mass brown dwarf with a circumstellar disk. In a near-infrared spectrum
    of
    this source obtained with the Gemini Near-Infrared Spectrograph, the
    presence
    of strong steam absorption confirms its late-type nature (>=M9.5) while the
    shapes of the H- and K-band continua and the strengths of the Na I and K I
    lines demonstrate that it is a young, pre-main-sequence object rather than a
    field dwarf. A comparison of the bolometric luminosity of Cha 110913-773444
    to
    the luminosities predicted by the evolutionary models of Chabrier and
    Baraffe
    and Burrows and coworkers indicates a mass of 8+7/-3 M_Jup, placing it fully
    within the mass range observed for extrasolar planetary companions (M<=15
    M_Jup). The spectral energy distribution of this object exhibits
    mid-infrared
    excess emission at >5 um, which we have successfully modeled in terms of an
    irradiated viscous accretion disk with M'<=10e-12 M_sun/year. Cha
    110913-773444
    is now the least massive brown dwarf observed to have a circumstellar disk,
    and
    indeed is one of the least massive free-floating objects found to date.
    These
    results demonstrate that the raw materials for planet formation exist around
    free-floating planetary-mass bodies.

    \\ ( http://arXiv.org/abs/astro-ph/0511807 , 27kb)


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