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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20150129T103000
DTEND;TZID=Atlantic/Canary:20150129T113000
UID:iactalks-756
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/756
CREATED:2015-01-29T10:30:00+00:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Very Low Mass Stars, Brown Dwarfs and Gas Giant Exoplanets
DESCRIPTION:Very Low Mass Stars, Brown Dwarfs and Gas Giant Exoplanets\nDr.
  France Allard\n\nUnderstanding the atmospheric and evolutive properties o
 f very low mass stars, brown dwarfs, and gas giant exoplanets have been im
 portant challenges for modelers around the world since the discovery of th
 e first brown dwarfs in the Pleiades cluster (Rebolo et al. 1995) and in t
 he field (Nakajima et al. 1995). The early studies of brown dwarfs have pr
 ovided rich insights into atmospheric physics, with discoveries ranging fr
 om cloud formation (Tsuji et al. 1996), methane bands (Oppenheimer et al. 
 1995) and ammonia bands (Delorme et al. 2008), to the formation of wasi-mo
 lecular KI-H2 absorption (Allard et al. 2007), and to disequilibrium chemi
 stry (Yelle & Griffith 2001). New classical 1D models yield spectral e
 nergy distribution (SED) that match relatively well despite these complexi
 ties. These models have for instance explained the spectral transition fro
 m M to L, T and now Y brown dwarf spectral types (Allard et al. 2013). How
 ever, in presence of surface inhomogeneities revealed recently for a nearb
 y (2 pc) brown dwarf (Crossfield et al. 2014), the SED may well fit even e
 xactly, but the model parameters could be far from exact, e.g. with the ef
 fective temperature by several hundred kelvins too cool in the case of dus
 ty brown dwarfs and young gas giant exoplanets! I will review the progress
  achieved in reproducing the spectral properties of very low mass stars, b
 rown dwarfs and gas giant exoplanets, and review progress in modeling more
  accurately their atmospheres using Radiation HydroDynamical (RHD) simulat
 ions.
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