Analysis of the first overtone bands of isotopologues of CO and SiO in stellar spectra
Analysis of the first overtone bands of isotopologues of CO and SiO in stellar spectra
复制标题
恒星光谱中CO和SiO同位素体的第一泛音带分析
DOI：
10.1051/0004-6361/201936811
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发表时间：
2019
影响因子：
6.5
通讯作者：
J. Tennyson
中科院分区：
文献类型：
--
作者：
Y. Pavlenko;S. Yurchenko;J. Tennyson
语境。这项研究基于大角星 (K2 III) 光谱中 2.3 μm 处 CO 单取代同位素体的第一泛音 (Δv = 2) 谱带和红巨星 HD 196610 (M6 III) 光谱中 4 μm 处 SiO 单取代同位素体的模型。
目标。我们的目标是研究涉及晚型恒星光谱中 CO 和 SiO 同位素体第一泛音带计算的问题，并确定同位素丰度。
方法。我们使用理论合成光谱与观测到的 CO 和 SiO 恒星分子带的拟合来确定 C、O 和 Si 同位素的丰度。
结果。使用三个可用线表计算的 2.3 μm 处 12C16O 第一泛音带的合成光谱与大角星观测光谱的拟合提供了相同的碳丰度 [C] = − 0.6 和碳 12C/13C 同位素比 = 10 ± 2。然而，对于所使用的三个线表，与观测光谱的拟合质量不同。此外，导出的氧同位素比 16O/18O = 2000 ± 500 大于太阳系中已知的氧同位素比，其中 16O/18O = 500。红巨星 HD 196610 大气中的硅同位素比已被修正。使用 ExoMol SiO2 线列表以及 SiO2 同位素异数体的适当统计权重，获得“非太阳能”比率 28Si:29Si:30Si = 0.86 ± 0.03:0.12 ± 0.02:0.02 ± 0.01。
结论。我们发现：（a）通过拟合观测光谱确定的计算同位素碳和硅比率分别取决于所采用的 C 和 Si 丰度； (b) 核自旋简并参数的正确处理对于当今 HITRAN 和 ExoMol 线表在天体物理计算中的应用至关重要。
Context. This study is based on models of the first overtone (Δv = 2) bands of the monosubstituted isotopologues of CO at 2.3 μm in the spectrum of Arcturus (K2 III) and of the monosubstituted isotopologues of SiO at 4 μm in the spectrum of the red giant HD 196610 (M6 III).
Aims. We aim to investigate problems involving the computation of the first overtone bands of isotopologues of CO and SiO in the spectra of late-type stars and to determine isotopic abundances.
Methods. We used fits of theoretical synthetic spectra to the observed stellar molecular bands of CO and SiO for determining the abundances for isotopes of C, O, and Si.
Results. Fits of synthetic spectra of the 12C16O first overtone bands at 2.3 μm computed with three available line lists to the observed spectrum of Arcturus provide the same carbon abundance [C] = − 0.6 and isotopic ratio of carbon 12C/13C = 10 ± 2. However, the quality of fits to the observed spectrum differ for three line lists used. Furthermore, the derived oxygen isotopic ratio 16O/18O = 2000 ± 500 is larger than that known in the solar system, where 16O/18O = 500. The silicon isotopic ratio in the atmosphere of the red giant HD 196610 has been revised. Using the ExoMol SiO line list with appropriate statistical weights for the SiO isotopologues, the “non-solar” ratio 28Si:29Si:30Si = 0.86 ± 0.03:0.12 ± 0.02:0.02 ± 0.01 is obtained.
Conclusions. We find that: (a) the computed isotopic carbon and silicon ratios determined by the fits to the observed spectrum depend on the adopted abundance of C and Si, respectively; and (b) Correct treatment of the nuclear spin degeneracies parameter is of crucial importance for today’s application of HITRAN and ExoMol line lists in the astrophysical computations.
影响因子：
3
作者：
G. Tinetti;P. Drossart;P. Eccleston;P. Hartogh;A. Heske;J. Leconte;G. Micela;M. Ollivier;G. Pilbratt;L. Puig;D. Turrini;B. Vandenbussche;Paulina Wolkenberg;J. Beaulieu;L. A. Buchave;Martin Ferus;M. Griffin;M. Guedel;K. Justtanont;P. Lagage;Pedro Machado;G. Malaguti;Michiel Min;H. Nørgaard-Nielsen;Mirek Rataj;T. Ray;Ignasi Ribas;M. Swain;R. Szabó;Stephanie C. Werner;J. Barstow;Matt Burleigh;James Cho;V. C. du Foresto;A. Coustenis;L. Decin;T. Encrenaz;M. Galand;M. Gillon;R. Helled;J. C. Morales;A. G. Muñoz;A. Moneti;Isabella Pagano;E. Pascale;G. Piccioni;David Pinfield;Subhajit Sarkar;F. Selsis;J. Tennyson;A. Triaud;O. Venot;I. Waldmann;David Waltham;Gillian S. Wright;J. Amiaux;J. Auguères;M. Berthé;N. Bezawada;G. Bishop;Neil Bowles;Deirdre Coffey;J. Colomé;M. Crook;P. Crouzet;Vania Da Peppo;I. E. Sanz;M. Focardi;M. Frericks;Tom Hunt;R. Kohley;K. Middleton;G. Morgante;R. Ottensamer;E. Pace;Chris Pearson;R. Stamper;K. Symonds;M. Rengel;E. Renotte;P. Ade;L. Affer;Christophe Alard;Nicole F. Allard;F. Altieri;Yves André;Claudio Arena;I. Argyriou;Alan Aylward;C. Baccani;Gáspár Á. Bakos;M. Banaszkiewicz;Mike Barlow;V. Batista;G. Bellucci;S. Benatti;Pernelle Bernardi;Bruno Bézard;M. Błęcka;É. Bolmont;B. Bonfond;R. Bonito;A. Bonomo;J. Brucato;Allan Sacha Brun;I. Bryson;W. Bujwan;S. Casewell;B. Charnay;C. Pestellini;Guo Chen;A. Ciaravella;R. Claudi;R. Clédassou;M. Damasso;M. Damiano;C. Danielski;Pieter Deroo;A. D. di Giorgio;Carsten Dominik;V. Doublier;S. Doyle;René Doyon;Benjamin Drummond;Bastien Duong;S. Eales;Billy Edwards;Maria Farina;E. Flaccomio;Leigh Fletcher;F. Forget;Steve Fossey;Markus Fränz;Yuka Fujii;A. Garcia-Piquer;W. Gear;H. Geoffray;Jean-Claude Gérard;L. Gesa;H. Gomez;Rafał Graczyk;C. Griffith;D. Grodent;M. Guarcello;J. Gustin;K. Hamano;P. Hargrave;Y. Hello;Kevin Heng;E. Herrero;A. Hornstrup;Benoît Hubert;Shigeru Ida;M. Ikoma;N. Iro;Patrick Irwin;C. Jarchow;Jean Jaubert;Hugh R. A. Jones;Queyrel Julien;Shingo Kameda;F. Kerschbaum;P. Kervella;T. Koskinen;M. Krijger;N. Krupp;M. Lafarga;F. Landini;E. Lellouch;G. Leto;A. Luntzer;T. Rank-Lüftinger;Antonio Maggio;J. Maldonado;Jean-Pierre Maillard;Urs Mall;J. Marquette;Stéphane Mathis;P. Maxted;T. Matsuo;A. Medvedev;Yamila Miguel;V. Minier;G. Morello;Alessandro Mura;N. Narita;V. Nascimbeni;N. Nguyen Tong;V. Noce;F. Oliva;E. Pallé;Paul Palmer;M. Pancrazzi;A. Papageorgiou;V. Parmentier;M. Perger;A. Petralia;S. Pezzuto;Ray Pierrehumbert;I. Pillitteri;G. Piotto;G. Pisano;L. Prisinzano;A. Radioti;J. Réess;L. Rezac;M. Rocchetto;A. Rosich;N. Sanna;A. Santerne;G. Savini;G. Scandariato;B. Sicardy;Carles Sierra;G. Sindoni;K. Skup;I. Snellen;M. Sobiecki;L. Soret;A. Sozzetti;A. Stiepen;A. Strugarek;Jake Taylor;William Taylor;L. Terenzi;M. Tessenyi;A. Tsiaras;C. Tucker;Diana Valencia;G. Vasisht;A. Vazan;F. Vilardell;S. Vinatier;S. Viti;Rens Waters;P. Wawer;A. Wawrzaszek;A. Whitworth;Yuk L. Yung;S. Yurchenko;M. Z. Osorio;R. Zellem;T. Zingales;F. Zwart
通讯作者：
G. Tinetti;P. Drossart;P. Eccleston;P. Hartogh;A. Heske;J. Leconte;G. Micela;M. Ollivier;G. Pilbratt;L. Puig;D. Turrini;B. Vandenbussche;Paulina Wolkenberg;J. Beaulieu;L. A. Buchave;Martin Ferus;M. Griffin;M. Guedel;K. Justtanont;P. Lagage;Pedro Machado;G. Malaguti;Michiel Min;H. Nørgaard-Nielsen;Mirek Rataj;T. Ray;Ignasi Ribas;M. Swain;R. Szabó;Stephanie C. Werner;J. Barstow;Matt Burleigh;James Cho;V. C. du Foresto;A. Coustenis;L. Decin;T. Encrenaz;M. Galand;M. Gillon;R. Helled;J. C. Morales;A. G. Muñoz;A. Moneti;Isabella Pagano;E. Pascale;G. Piccioni;David Pinfield;Subhajit Sarkar;F. Selsis;J. Tennyson;A. Triaud;O. Venot;I. Waldmann;David Waltham;Gillian S. Wright;J. Amiaux;J. Auguères;M. Berthé;N. Bezawada;G. Bishop;Neil Bowles;Deirdre Coffey;J. Colomé;M. Crook;P. Crouzet;Vania Da Peppo;I. E. Sanz;M. Focardi;M. Frericks;Tom Hunt;R. Kohley;K. Middleton;G. Morgante;R. Ottensamer;E. Pace;Chris Pearson;R. Stamper;K. Symonds;M. Rengel;E. Renotte;P. Ade;L. Affer;Christophe Alard;Nicole F. Allard;F. Altieri;Yves André;Claudio Arena;I. Argyriou;Alan Aylward;C. Baccani;Gáspár Á. Bakos;M. Banaszkiewicz;Mike Barlow;V. Batista;G. Bellucci;S. Benatti;Pernelle Bernardi;Bruno Bézard;M. Błęcka;É. Bolmont;B. Bonfond;R. Bonito;A. Bonomo;J. Brucato;Allan Sacha Brun;I. Bryson;W. Bujwan;S. Casewell;B. Charnay;C. Pestellini;Guo Chen;A. Ciaravella;R. Claudi;R. Clédassou;M. Damasso;M. Damiano;C. Danielski;Pieter Deroo;A. D. di Giorgio;Carsten Dominik;V. Doublier;S. Doyle;René Doyon;Benjamin Drummond;Bastien Duong;S. Eales;Billy Edwards;Maria Farina;E. Flaccomio;Leigh Fletcher;F. Forget;Steve Fossey;Markus Fränz;Yuka Fujii;A. Garcia-Piquer;W. Gear;H. Geoffray;Jean-Claude Gérard;L. Gesa;H. Gomez;Rafał Graczyk;C. Griffith;D. Grodent;M. Guarcello;J. Gustin;K. Hamano;P. Hargrave;Y. Hello;Kevin Heng;E. Herrero;A. Hornstrup;Benoît Hubert;Shigeru Ida;M. Ikoma;N. Iro;Patrick Irwin;C. Jarchow;Jean Jaubert;Hugh R. A. Jones;Queyrel Julien;Shingo Kameda;F. Kerschbaum;P. Kervella;T. Koskinen;M. Krijger;N. Krupp;M. Lafarga;F. Landini;E. Lellouch;G. Leto;A. Luntzer;T. Rank-Lüftinger;Antonio Maggio;J. Maldonado;Jean-Pierre Maillard;Urs Mall;J. Marquette;Stéphane Mathis;P. Maxted;T. Matsuo;A. Medvedev;Yamila Miguel;V. Minier;G. Morello;Alessandro Mura;N. Narita;V. Nascimbeni;N. Nguyen Tong;V. Noce;F. Oliva;E. Pallé;Paul Palmer;M. Pancrazzi;A. Papageorgiou;V. Parmentier;M. Perger;A. Petralia;S. Pezzuto;Ray Pierrehumbert;I. Pillitteri;G. Piotto;G. Pisano;L. Prisinzano;A. Radioti;J. Réess;L. Rezac;M. Rocchetto;A. Rosich;N. Sanna;A. Santerne;G. Savini;G. Scandariato;B. Sicardy;Carles Sierra;G. Sindoni;K. Skup;I. Snellen;M. Sobiecki;L. Soret;A. Sozzetti;A. Stiepen;A. Strugarek;Jake Taylor;William Taylor;L. Terenzi;M. Tessenyi;A. Tsiaras;C. Tucker;Diana Valencia;G. Vasisht;A. Vazan;F. Vilardell;S. Vinatier;S. Viti;Rens Waters;P. Wawer;A. Wawrzaszek;A. Whitworth;Yuk L. Yung;S. Yurchenko;M. Z. Osorio;R. Zellem;T. Zingales;F. Zwart
影响因子：
4.8
作者：
D. Romano;F. Matteucci;F. Matteucci;Zhi-Yu Zhang;Zhi-Yu Zhang;Pantelis Papadopoulos;Pantelis Papadopoulos-P
通讯作者：
D. Romano;F. Matteucci;F. Matteucci;Zhi-Yu Zhang;Zhi-Yu Zhang;Pantelis Papadopoulos;Pantelis Papadopoulos-P