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[71.05] GM Auriagae's Circumstellar Disk: Multiwavelength Observations and Radiation Transfer Models

K. Wood (St Andrews), D. Koerner (Penn), B. Whitney (SSI), G. Schneider (Arizona), K. Stassun (Wisconsin), J. Bjorkman (Toledo)

We present models for the GM Auriga circumstellar disk based upon its spectral energy distribution and high-resolution HST imaging obtained with WFPC-2 (F555W) and NICMOS at 1.1 and 1.6 microns in its coronagraphic imaging mode. Our circumstellar geometry comprises a passively heated flared disk of mass M_d=0.06M_\odot, radius R_d=300AU, viewed at inclination i=45^\circ. Fitting the SED in the range 1 to 12 microns constrains the inner disk truncation radius to be R_in~4AU. Modeling additional SIRTF data in this regime will provide tighter constraints on the disk truncation radius. Our Monte Carlo radiative equilibrium code calculates accurate disk temperature structures and SEDs in only a few minutes on current Linux boxes. We will show model SEDs and disk temperature distributions for a range of different disk structures and inner disk truncation radii.

We acknowledge support from a UK/PPARC Advanced Fellowship, NASA's LTSA program, NSF Stellar Astronomy, and the Hubble Fellowship program. This work is based, in part, on observations with the NASA/ESA Hubble Space Telescope, obtained at the STScI, which is operated by the AURA, Inc. under NASA contract NAS5-26555 and supported by NASA grant NAG5-3042 to the NICMOS IDT.

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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.