A protoplanetary-disk model for the molecular gas discovered toward a T Tauri star GG Tau

Details A protoplanetary-disk model for the molecular gas discovered toward a T Tauri star GG Tau A protoplanetary-disk model for the molecular gas discovered toward a T Tauri star GG Tau

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasj...45l..27k&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 45, no. 2, p. L27-L32.

Astronomy and Astrophysics

Astronomy

10

Astronomical Models, Interstellar Gas, Molecular Gases, Planetary Evolution, Protoplanets, T Tauri Stars, Radiative Transfer, Star Formation

Scientific paper

The velocity profiles of the (C-12)O (J = 1-0) line emitted from protoplanetary gas disks are numerically calculated by taking account of line-radiative transfer, based on the Kyoto model. It was found that the calculated profiles fitted well to both the (C-12)O velocity profiles observed toward GG Tau by Kawabe et al. (1993) with the Nobeyama Millimeter Array and by Skrutskie et al. (1993) with the Nobeyama 45-m telescope. Assuming that the mass of GG Tau is 0.65 solar mass, a best-fit model of a protoplanetary disk with a radius of R(disk) = 900 AU, an inclination angle i = 67 deg, and a temperature variation T = 13(r/500 AU) exp 0.5 K was obtained.

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