Gas modelling in the disc of HD 163296
Creators
- Tilling, I.1
- Woitke, P.2, 3, 4
- Meeus, G.5
- Mora, A.
- Montesinos, B.6
- Rivière-Marichalar, P.6
- Eiroa, C.5
- Thi, W.-F.
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Isella, A.7
- Roberge, A.8
- Martin-Zaidi, C.
- Kamp, I.9
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Pinte, C.
- Sandell, G.10
- Vacca, W. D.10
- Ménard, F.
- Mendigutía, I.6
- Duchêne, G.11
- Dent, W. R. F.12
- Aresu, G.9
- Meijerink, R.13
- Spaans, M.9
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1.
University of Edinburgh
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2.
University of Vienna
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3.
UK Astronomy Technology Centre
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4.
University of St Andrews
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5.
Autonomous University of Madrid
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6.
Centro de Astrobiología
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7.
California Institute of Technology
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8.
Goddard Space Flight Center
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9.
University of Groningen
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10.
Ames Research Center
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11.
University of California, Berkeley
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12.
European Southern Observatory
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13.
Leiden University
Abstract
We present detailed model fits to observations of the disc around the Herbig Ae star HD 163296. This well-studied object has an age of ~4 Myr, with evidence of a circumstellar disc extending out to ~540 AU. We use the radiation thermo-chemical disc code ProDiMo to model the gas and dust in the circumstellar disc of HD 163296, and attempt to determine the disc properties by fitting to observational line and continuum data. These include new Herschel/PACS observations obtained as part of the open-time key program GASPS (GAS in Protoplanetary Systems), consisting of a detection of the [Oi] 63 μm line and upper limits for several other far infrared lines. We complement this with continuum data and ground-based observations of the ^(12)CO 3–2, 2–1 and ^(13)CO J = 1–0 line transitions, as well as an upper limit for the H_2 0–0 S(1) transition. We explore the effects of stellar ultraviolet variability and dust settling on the line emission, and on the derived disc properties. Our fitting efforts lead to derived gas/dust ratios in the range 9–100, depending on the assumptions made. We note that the line fluxes are sensitive in general to the degree of dust settling in the disc, with an increase in line flux for settled models. This is most pronounced in lines which are formed in the warm gas in the inner disc, but the low excitation molecular lines are also affected. This has serious implications for attempts to derive the disc gas mass from line observations. We derive fractional PAH abundances between 0.007 and 0.04 relative to ISM levels. Using a stellar and UV excess input spectrum based on a detailed analysis of observations, we find that the all observations are consistent with the previously assumed disc geometry.
Additional Information
© 2012 ESO. Received 18 March 2011. Accepted 2 November 2011. Published online 27 January 2012.Attached Files
Published - Tilling2012p17628Astron_Astrophys.pdf
Files
Tilling2012p17628Astron_Astrophys.pdf
Additional details
Identifiers
- Eprint ID
- 29972
- Resolver ID
- CaltechAUTHORS:20120404-090545717
Dates
- Created
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2012-04-04Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field