Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...357l...9c&link_type=abstract
Astronomy and Astrophysics, v.357, p.L9-L12 (2000)
Astronomy and Astrophysics
Astrophysics
64
Scientific paper
We model the H2CO and H213CO line emission observed towards the solar-type protostar IRAS16293-2422. Based upon previous analysis of the physical structure of the envelope surrounding IRAS16293-2422, we develop a model in which the H2CO lines are emitted by two components: a cold H_2CO-poor outer envelope and a warm H_2CO-rich core. We find that the model reproduces successfully all the available H2CO and H213CO data for a H2CO abundance equal to (1.1 +/- 0.3) x 10-9 in the outer and (1.1 +/- 0.4) x 10-7 in the inner regions of the envelope respectively. We interpret this increase of the H2CO abundance as due to the evaporation of the grain mantles when the dust temperature exceeds 100 K at about 150 AU from the center, forming a hot core like region. Assuming that all mantle constituents evaporate and are detected in the gas phase, we derive that the H_2CO-ice abundance is about 3% of the H_2O-ice abundance. This is the first measurement of the H2CO abundance in grain mantles around a low-mass protostar.
Castets Alain
Caux Emmanuel
Ceccarelli Cecilia
Loinard Laurent
Tielens Alexander G. G. M.
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