Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.106b&link_type=abstract
The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole
Other
Scientific paper
The Herschel Space Observatory has opened the sky for studies of warm and dense gas. Rotational lines of CO with Jup ≳ 14 have been detected towards envelopes of young stellar objects and protoplanetary disks indicating a considerable amount of gas with temperature over several 100 K The low-mass young stellar object HH46 (van Kempen et al. 2010) for example has been detected in CO up to Jup = 31. Their analysis indicates an origin of the radiation in outflow wall, irradiated and heated by protostellar far UV (FUV) radiation. Another example is the protoplanetary disk around HD100546 (Sturm et al. 2010) where CO levels of up to 2500 K are excited. What is the amount of warm gas in these sources? Can we explain the amount of warm gas by heating through protostellar FUV radiation or are the additional sources of heating needed, like shocks? How are the CO lines excited? What are the essential parameters that control the abundance and excitation of CO. How does CO relate to other important molecular and atomic coolants? We attempt to answer these questions with a new and detailed chemistry and radiative transfer called Chem&trans (Bruderer et al., in prep). The 2D model is based on the work of Bruderer et al. 2009, 2010 and solves self-consistently for the chemistry, dust and line radiative transfer and the thermal balance to obtain the gas temperature. The new model is modular and can be applied on a wide range of objects from protoplanetary disks to envelopes of young stellar objects. We discuss the new model and show first results derived with the code.
Bruderer Simon
Doty Steven D.
van Dishoeck Ewine F.
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