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Herschel/HIFI observations of the circumstellar ammonia lines in IRC+10216

M. R. Schmidt ; J. H. He ; R. Szczerba ; V. Bujarrabal ; J. Alcolea ; J. Cernicharo ; L. Decin ; Kay Justtanont (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; D. Teyssier ; K. M. Menten ; D. A. Neufeld ; Hans Olofsson (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; P. Planesas ; A. P. Marston ; A. M. Sobolev ; A. de Koter ; Fredrik L. Schöier (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium)
Astronomy and Astrophysics (0004-6361). Vol. 592 (2016),
[Artikel, refereegranskad vetenskaplig]

Context. A discrepancy exists between the abundance of ammonia (NH3) derived previously for the circumstellar envelope (CSE) of IRC+10216 from far-IR submillimeter rotational lines and that inferred from radio inversion or mid-infrared (MIR) absorption transitions. Aims. To address the discrepancy described above, new high-resolution far-infrared (FIR) observations of both ortho-and para-NH3 transitions toward IRC+10216 were obtained with Herschel, with the goal of determining the ammonia abundance and constraining the distribution of NH3 in the envelope of IRC+10216. Methods. We used the Heterodyne Instrument for the Far Infrared (HIFI) on board Herschel to observe all rotational transitions up to the J = 3 level (three ortho-and six para-NH3 lines). We conducted non-LTE multilevel radiative transfer modelling, including the effects of near-infrared (NIR) radiative pumping through vibrational transitions. The computed emission line profiles are compared with the new HIFI data, the radio inversion transitions, and the MIR absorption lines in the nu(2) band taken from the literature. Results. We found that NIR pumping is of key importance for understanding the excitation of rotational levels of NH3. The derived NH3 abundances relative to molecular hydrogen were (2.8 +/- 0.5) x 10(-8) for ortho-NH3 and (3.2(-0.6)(+0.7)) x 10(-8) for para-NH3, consistent with an ortho/para ratio of 1. These values are in a rough agreement with abundances derived from the inversion transitions, as well as with the total abundance of NH3 inferred from the MIR absorption lines. To explain the observed rotational transitions, ammonia must be formed near to the central star at a radius close to the end of the wind acceleration region, but no larger than about 20 stellar radii (1 sigma confidence level).

Nyckelord: stars: AGB and post-AGB, circumstellar matter, stars: carbon, stars: individual: IRC+10216

Denna post skapades 2016-11-25. Senast ändrad 2017-01-25.
CPL Pubid: 245633


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