A Protoplanetary-Disk Model for the Molecular Gas Discovered toward a T Tauri Star GG Tau
Abstract
For a detailed analysis of the molecular gas discovered around GG Tau, we numerically calculated the velocity profiles of the (12) CO (J=1--0) line emitted from protoplanetary gas disks by taking account of line-radiative transfer, based on the Kyoto model. The calculated profiles were fitted to the profiles of (12) CO emission detected toward GG Tau by Kawabe et al. (1993, {Astrophys. J. Letters}, 404, L63) with the Nobeyama Millimeter Array (NMA) and by Skrutskie et al. (1993, {Astrophys. J.}, in press) with the Nobeyama 45-m telescope. We obtained a best-fit model of a protoplanetary disk having a radius of R_disk = 900 AU, an inclination angle of i = 67(deg) , and a temperature variation of T = 13 (r/500 AU)(-0.5) K, assuming that the mass of GG Tau is 0.65 MO . The new values of R_disk and T are larger than the results of R_disk =500 AU, i = 57 +/- 10(deg) , and T = 8 K (at 500 AU) by Kawabe et al. (1993) using NMA. The model fitting to the (12) CO data was quite good, except for a disagreement between our calculated flux and the observed flux of the blueshifted component by NMA, which can be explained by an asymmetry of the gas disk around GG Tau, as resolved by NMA.
- Publication:
-
Publications of the Astronomical Society of Japan
- Pub Date:
- April 1993
- Bibcode:
- 1993PASJ...45L..27K
- Keywords:
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- Astronomical Models;
- Interstellar Gas;
- Molecular Gases;
- Planetary Evolution;
- Protoplanets;
- T Tauri Stars;
- Radiative Transfer;
- Star Formation;
- Astrophysics;
- INTERSTELLAR: MOLECULES;
- PLANETS: FORMATION;
- RADIATIVE TRANSFER;
- STARS: FORMATION;
- STARS: INDIVIDUAL (GG TAURI)