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Herschel-PACS observation of the 10 Myr old T Tauri disk TW Hya Constraining the disk gas mass

W. F. Thi ; G. Mathews ; F. Menard ; P. Woitke ; G. Meeus ; P. Riviere-Marichalar ; C. Pinte ; C. D. Howard ; A. Roberge ; G. Sandell ; I. Pascucci ; B. Riaz ; C. A. Grady ; W. R. F. Dent ; I. Kamp ; G. Duchene ; J. C. Augereau ; E. Pantin ; B. Vandenbussche ; I. Tilling ; J. P. Williams ; C. Eiroa ; D. Barrado ; J. M. Alacid ; S. Andrews ; D. R. Ardila ; G. Aresu ; S. Brittain ; D. R. Ciardi ; W. Danchi ; D. Fedele ; I. de Gregorio-Monsalvo ; A. Heras ; N. Huelamo ; A. Krivov ; J. Lebreton ; René Liseau (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; C. Martin-Zaidi ; I. Mendigutia ; B. Montesinos ; A. Mora ; M. Morales-Calderon ; H. Nomura ; N. Phillips ; L. Podio ; D. R. Poelman ; S. Ramsay ; K. Rice ; E. Solano ; H. Walker ; G. J. White ; G. Wright
Astronomy & Astrophysics (0004-6361). Vol. 518 (2010), Article Number: L125,
[Artikel, refereegranskad vetenskaplig]

Planets are formed in disks around young stars. With an age of similar to 10 Myr, TW Hya is one of the nearest T Tauri stars that is still surrounded by a relatively massive disk. In addition a large number of molecules has been found in the TW Hya disk, making TW Hya the perfect test case in a large survey of disks with Herschel-PACS to directly study their gaseous component. We aim to constrain the gas and dust mass of the circumstellar disk around TW Hya. We observed the fine-structure lines of [OI] and [CII] as part of the open-time large program GASPS. We complement this with continuum data and ground-based (12) CO 3-2 and (CO)-C-13 3-2 observations. We simultaneously model the continuum and the line fluxes with the 3D Monte-Carlo code MCFOST and the thermo-chemical code ProDiMo to derive the gas and dust masses. We detect the [OI] line at 63 mu m. The other lines that were observed, [OI] at 145 mu m and [CII] at 157 mu m, are not detected. No extended emission has been found. Preliminary modeling of the photometric and line data assuming [(CO)-C-12]/[(CO)-C-13] = 69 suggests a dust mass for grains with radius < 1 mm of similar to 1.9 x 10(-4) M-circle dot (total solid mass of 3 x 10(-3) M-circle dot) and a gas mass of (0.5-5) x 10(-3) M-circle dot. The gas-to-dust mass may be lower than the standard interstellar value of 100.

Nyckelord: circumstellar disks, main-sequence stars, protoplanetary disks, young stars, x-ray, hydrae, emission, spectra, models, array

Denna post skapades 2010-12-08. Senast ändrad 2011-03-21.
CPL Pubid: 130325


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