Comparative modelling of the spectra of cool giants

被引：0

作者：

机构：

[1] Lebzelter, T.

[2] Heiter, U.

[3] Abia, C.

[4] Eriksson, K.

[5] 4,Ireland, M.

[6] Neilson, H.

[7] Nowotny, W.

[8] Maldonado, J.

[9] Merle, T.

[10] Peterson, R.

[11] Plez, B.

[12] Short, C.I.

[13] Wahlgren, G.M.

[14] Worley, C.

[15] Aringer, B.

[16] Bladh, S.

[17] De Laverny, P.

[18] Goswami, A.

[19] Mora, A.

[20] Norris, R.P.

[21] Recio-Blanco, A.

[22] 16,Scholz, M.

[23] Thévenin, F.

[24] Tsuji, T.

[25] Kordopatis, G.

[26] Montesinos, B.

[27] Wing, R.F.

来源：

Lebzelter, T. (thomas.lebzelter@univie.ac.at) | 1600年 / EDP Sciences卷 / 547期

关键词：

Context. Our ability to extract information from the spectra of stars depends on reliable models of stellar atmospheres and appropriate techniques for spectral synthesis. Various model codes and strategies for the analysis of stellar spectra are available today. Aims. We aim to compare the results of deriving stellar parameters using different atmosphere models and different analysis strategies. The focus is set on high-resolution spectroscopy of cool giant stars. Methods. Spectra representing four cool giant stars were made available to various groups and individuals working in the area of spectral synthesis; asking them to derive stellar parameters from the data provided. The results were discussed at a workshop in Vienna in 2010. Most of the major codes currently used in the astronomical community for analyses of stellar spectra were included in this experiment. Results. We present the results from the different groups; as well as an additional experiment comparing the synthetic spectra produced by various codes for a given set of stellar parameters. Similarities and differences of the results are discussed. Conclusions. Several valid approaches to analyze a given spectrum of a star result in quite a wide range of solutions. The main causes for the differences in parameters derived by different groups seem to lie in the physical input data and in the details of the analysis method. This clearly shows how far from a definitive abundance analysis we still are. © ESO; 2012;

D O I：

暂无

中图分类号：

学科分类号：

摘要：

Journal article (JA)

引用

共 50 条

[1] Comparative modelling of the spectra of cool giants
Lebzelter, T.
Heiter, U.
Abia, C.
Eriksson, K.
Ireland, M.
Neilson, H.
Nowotny, W.
Maldonado, J.
Merle, T.
Peterson, R.
Plez, B.
Short, C. I.
Wahlgren, G. M.
Worley, C.
Aringer, B.
Bladh, S.
de Laverny, P.
Goswami, A.
Mora, A.
Norris, R. P.
Recio-Blanco, A.
Scholz, M.
Thevenin, F.
Tsuji, T.
Kordopatis, G.
Montesinos, B.
Wing, R. F.
ASTRONOMY & ASTROPHYSICS, 2012, 547
[2] Gaia spectroscopy overview and comparative spectrum modeling for cool giants
Heiter, U.
Lebzelter, T.
GREAT-ESF WORKSHOP: STELLAR ATMOSPHERES IN THE GAIA ERA, 2011, 328
[3] Model atmospheres and spectra for cool hydrogen-deficient stars and peculiar giants
Pavlenko, Yakiv V.
HYDROGEN-DEFICIENT STARS, 2008, 391 : 65 - 68
[4] New temperature and metallicity scale of cool giants from K-band spectra
Ghosh, Supriyo
Ojha, D. K.
Ninan, J. P.
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2021, 501 (03) : 4596 - 4609
[5] THE CIRCUMSTELLAR ENVELOPES AND CHROMOSPHERES OF COOL GIANTS AND SUPER-GIANTS
HAGEN, W
STENCEL, RE
DICKINSON, DF
ASTROPHYSICAL JOURNAL, 1983, 274 (01): : 286 - 301
[6] Dynamic model atmospheres of cool giants
Höfner, S
Gautschy-Loidl, R
Aringer, B
Nowotny, W
Hron, J
Freytag, B
High Resolution Infrared Spectroscopy in Astronomy, Proceedings, 2005, : 269 - 280
[7] A Spectroscopic Analysis of the Hyades Cool Giants
Gray, David F.
Martinez, A.
ASTRONOMICAL JOURNAL, 2019, 157 (03):
[8] Cool giants and supergiants: chromospheres and winds
Jordan, C
ASTRONOMY & GEOPHYSICS, 1997, 38 (06) : 21 - 24
[9] Cool giants and supergiants: Chromospheres and winds
Jordan, Carole
Astronomy and Geophysics, 1997, 38 (06): : 21 - 24
[10] Asteroseismology of Cool Dwarfs and Giants with Kepler
Gilliland, Ronald L.
16TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN, 2012, 448 : 167 - 176

← 1 2 3 4 5 →