Imaging the disk around TW Hydrae with the submillimeter array

被引：162

作者：

Qi, CH

Ho, PTP

Wilner, DJ

Takakuwa, S

Hirano, N

Ohashi, N

Bourke, TL

Zhang, QH

Blake, GA

Hogerheijde, M

Saito, M

Choi, MH

Yang, J

机构：

[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[2] Harvard Smithsonian Ctr Astrophys, Sunmillimeter Array Project, Hilo, HI 96720 USA

[3] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan

[4] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA

[5] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA

[6] Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands

[7] Natl Astron Observ Japan, Tokyo 1818588, Japan

[8] Korea Astron Observ, Taeduk Radio Astron Observ, Taejon 305348, South Korea

[9] Chinese Acad Sci, Purple Mt Observ, Nanjing 21008, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2004年 / 616卷 / 01期

关键词：

circumstellar matter; ISM : molecules; planetary systems : protoplanetary disks; radio lines : stars; stars : individual (TW Hydrae);

D O I：

10.1086/421063

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present similar to2"-4" aperture synthesis observations of the circumstellar disk surrounding the nearby young star TW Hya in the CO J = 2-1 and J = 3-2 lines and associated dust continuum obtained with the partially completed Submillimeter Array. The extent and peak flux of the 230 and 345 GHz dust emission follow closely the predictions of the irradiated accretion disk model of Calvet et al. The resolved molecular line emission extends to a radius of at least 200 AU, the full extent of the disk visible in scattered light, and shows a clear pattern of Keplerian rotation. Comparison of the images with two-dimensional Monte Carlo models constrains the disk inclination angle to 7degrees +/- 1degrees. The CO emission is optically thick in both lines, and the kinetic temperature in the line formation region is similar to20 K. Substantial CO depletion, by an order of magnitude or more from canonical dark cloud values, is required to explain the characteristics of the line emission.

引用

页码：L11 / L14

页数：4