Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations

被引：144

作者：

de Gregorio-Monsalvo, I. ^{[1
,7
]}

Menard, F. ^{[2
,3
,4
]}

Dent, W. ^{[1
,11
]}

Pinte, C. ^{[4
]}

Lopez, C. ^{[1
,6
]}

Klaassen, P. ^{[5
]}

Hales, A. ^{[1
,6
]}

Cortes, P. ^{[1
,6
]}

Rawlings, M. G. ^{[6
]}

Tachihara, K. ^{[1
,10
]}

Testi, L. ^{[7
,8
]}

Takahashi, S. ^{[1
,9
]}

Chapillon, E. ^{[9
]}

Mathews, G. ^{[5
]}

Juhasz, A. ^{[5
]}

Akiyama, E. ^{[10
]}

Higuchi, A. E. ^{[1
,10
]}

Saito, M. ^{[1
,10
]}

Nyman, L. -A. ^{[1
,11
]}

Phillips, N. ^{[1
,11
]}

Rodon, J. ^{[11
]}

Corder, S. ^{[1
,6
]}

Van Kempen, T. ^{[1
,5
]}

机构：

[1] Joint ALMA Observ, Santiago, Chile

[2] Univ Chile, UMI FCA, CNRS, INSU France,UMI 3386, Santiago 8330072, Chile

[3] Univ Chile, Dept Astron, Santiago 8330072, Chile

[4] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France

[5] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[6] Natl Radio Astron Observ, Charlottesville, VA 22903 USA

[7] European So Observ, D-85748 Garching, Germany

[8] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy

[9] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan

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

[11] European So Observ, Santiago 7630000, Chile

来源：

ASTRONOMY & ASTROPHYSICS | 2013年 / 557卷

基金：

美国国家航空航天局;

关键词：

stars: kinematics and dynamics; stars: pre-main sequence; techniques: interferometric; protoplanetary disks; stars: individual: HD 163296; PROTOPLANETARY DISKS; RADIATIVE-TRANSFER; THERMAL STRUCTURE; HERBIG AE/BE; STARS; CO; HD-163296; EMISSION;

D O I：

10.1051/0004-6361/201321603

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. The aim of this work is to study the structure of the protoplanetary disk surrounding the Herbig Ae star HD 163296. Methods. We used high-resolution and high-sensitivity ALMA observations of the CO(3-2) emission line and the continuum at 850 mu m, as well as the three-dimensional Monte Carlo radiative transfer code, MCFOST, to model the data presented in this work. Results. The CO(3-2) emission unveils for the first time at submillimeter frequencies the vertical structure details of a gaseous disk in Keplerian rotation, showing the back and front sides of a flared disk. Continuum emission at 850 mu m reveals a compact dust disk with a 240 AU outer radius and a surface brightness profile that shows a very steep decline at radius larger than 125 AU. The gaseous disk is more than two times larger than the dust disk, with a similar critical radius but with a shallower radial profile. Radiative transfer models of the continuum data confirm the need for a sharp outer edge to the dust disk. The models for the CO(3-2) channel map require the disk to be slightly more geometrically thick than previous models suggested, and that the temperature at which CO gas becomes depleted (i.e., frozen out) from the outer regions of the disk midplane is T < 20 K, in agreement with previous studies.

引用

页数：7

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