L etter to the E ditor Herschel-PACS observation of the 10 Myr old T Tauri disk TW Hya ⋆ Constraining the disk gas mass

Content Provider	Semantic Scholar
Author	Thi, -F. Mathews, Geoffrey S. Ménard, François Woitke, Peter Meeus, Gwendolyn Riviere-Marichalar, Pablo Pinte, Christophe Howard, C. Douglas Roberge, Aki Sandell, G. Oran Pascucci, Ilaria Riaz, Bilal Grady, Carol A. Dent, William R. F. Kamp, I. I. Ntroduction Duchêne, Gaspard Augereau, J. Ch. Pantin, Eric J. Vandenbussche, Bart Tilling, I. Williams, Jonathan P. Eiroa, Carlos Barrado, David Alacid, J. M. Andrews, Shawn Ardila, David R. Aresu, Giambattista Brittain, Sean D. Ciardi, David R. Danchi, William C. Fedele, Davide Gregorio-Monsalvo, Itziar De Heras, Ana M. Huelamo, N. Krivov, Alexander V. Lebreton, J. Liseau, Réne Martin-Zaidi, C. Mendigutía, I. Montesinos, Benjamín Mora, Andrés Morales-Calderon, M. Nomura, Hideko Phillips, Neil Podio, Linda Poelman, Dieter R. Ramsay, Scott Rice, Ken Solano, E. Walker, Harry White, Glenn J. Wright, Gillian
Copyright Year	2010
Abstract	Planets are formed in disks around young stars. With an age of ∼ 10 Myr, TW Hya is one of the nearest T Tauri stars that is still s urrounded by a relatively massive disk. In addition a large number of molec u s has been found in the TW Hya disk, making TW Hya the perfec t test case in a large survey of disks withHerschel–PACS to directly study their gaseous component. We aim to constra i he gas and dust mass of the circumstellar disk around TW Hya. We observed the fine-structure lines of [O I] and [C II] as part of the Open-time large program GASPS. We complement this with continuum data and ground-based 12 CO 3–2 and13CO 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 [O I] line at 63 μm. The other lines that were observed, [O I] at 145 μm and [C II] at 157μm, are not detected. No extended emission has been found. Pre liminary modeling of the photometric and line data assuming [ 12CO]/[13CO]=69 suggests a dust mass for grains with radius < 1 mm of∼ 1.9× 10−4 M⊙ (total solid mass of 3× 10−3 M⊙) and a gas mass of (0.5–5) × 10−3 M⊙. The gas-to-dust mass may be lower than the standard interst ella value of 100.
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Alternate Webpage(s)	http://authors.library.caltech.edu/21150/1/Thi2010p11916Astron_Astrophys.pdf
Alternate Webpage(s)	http://uhra.herts.ac.uk/bitstream/handle/2299/7278/904546.pdf?sequence=1
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Language	English
Access Restriction	Open
Subject Keyword	Complement System Proteins Herschel graph KDM5D gene Mahdiyar Monte Carlo Photometry Physics and Astronomy Classification Scheme Sixty Nine Stars, Celestial Test case Triune continuum paradigm
Content Type	Text
Resource Type	Article