YNAO OpenIR  > 大样本恒星演化研究组
Herschel/HIFI observations of the circumstellar ammonia lines in IRC+10216
Schmidt, MR1; He JH(何金华)2; Szczerba, R1; Bujarrabal, V3; Alcolea, J4; Cernicharo, J5; Decin, L6,7; Justtanont, K8; Teyssier, D; Menten, KM; Neufeld, DA; Olofsson, H8; Planesas, P4; Marston, AP; Sobolev, AM; de Koter, A7; Schoier, FL8; Schmidt, MR (reprint author), N Copernicus Astron Ctr, Rabianska 8, PL-87100 Torun, Poland.
发表期刊ASTRONOMY & ASTROPHYSICS
2016-08
卷号592
DOI10.1051/0004-6361/201527290
产权排序第2完成单位
收录类别SCI ; EI
关键词Stars: Agb And post-Agb Circumstellar Matter Stars: Carbon Stars: Individual: irc+10216
摘要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).
项目资助者National Science Center [N 203 581040] ; NSFC research grant [11173056] ; Chinese Academy Of Sciences President's International Fellowship Initiative ; EU FP7-PEOPLE-IRSES programme in the framework of project POSTAG-BinGALAXIES [269193] ; Spanish MICINN ; MINECO [FIS2012-32096, AYA2009-07304, AYA2012-32032, CSD2009-00038] ; ERC [ERC-2013-SyG] ; NANOCOS-MOS [610256] ; European Research Council under the European Community's H program/ERC [646758] ; Swedish national space board ; NASA/JPL ; program CONSOLIDER INGENIO [CSD2009-00038] ; [2015VMA015]
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-6361
URL查看原文
WOS记录号WOS:000384722600037
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]INFRARED OBJECT IRC+10216 ; MASS-LOSS HISTORY ; CARBON-STAR ; WATER-VAPOR ; CW LEONIS ; INTERSTELLAR AMMONIA ; HYPERFINE-STRUCTURE ; OPTICAL-PROPERTIES ; INVERSION LINES ; COMOVING-FRAME
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/9843
专题大样本恒星演化研究组
中国科学院天体结构与演化重点实验室
通讯作者Schmidt, MR (reprint author), N Copernicus Astron Ctr, Rabianska 8, PL-87100 Torun, Poland.
作者单位1.N. Copernicus Astronomical Center, Rabiańska 8, 87-100 Toruń, Poland
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences, PO Box 110, Kunming, Yunnan Province, PR China
3.Observatorio Astronómico Nacional. Ap 112, 28803 Alcalá de Henares, Spain
4.Observatorio Astronómico Nacional (IGN), Alfonso XII N ◦ 3, 28014 Madrid, Spain(5)ICMM, CSIC, group of Molecular Astrophysics, C/Sor Juana Inés de la Cruz N3, 28049 Cantoblanco, Madrid, Spain
5.Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
6.Sterrenkundig Instituut Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 Amsterdam, The Netherlands
7.Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, 439 92 Onsala, Sweden
8.European Space Astronomy Centre, ESA, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain 10 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 11 Johns Hopkins Universtity, Baltimore, MD 21218, USA 12 Department of Astronomy, AlbaNova University Center, Stockholm University, 10691 Stockholm, Sweden 13 Ural Federal University, Astronomical Observatory, 620000 Ekaterinburg, Russian Federation
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Schmidt, MR,He JH,Szczerba, R,et al. Herschel/HIFI observations of the circumstellar ammonia lines in IRC+10216[J]. ASTRONOMY & ASTROPHYSICS,2016,592.
APA Schmidt, MR.,He JH.,Szczerba, R.,Bujarrabal, V.,Alcolea, J.,...&Schmidt, MR .(2016).Herschel/HIFI observations of the circumstellar ammonia lines in IRC+10216.ASTRONOMY & ASTROPHYSICS,592.
MLA Schmidt, MR,et al."Herschel/HIFI observations of the circumstellar ammonia lines in IRC+10216".ASTRONOMY & ASTROPHYSICS 592(2016).
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