Herschel observations of the nebula M1-67 around the Wolf-Rayet star WR 124

被引：0

作者：

Vamvatira-Nakou, C. ^{[1
]}

Hutsemékers, D. ^{[1
]}

Royer, P. ^{[2
]}

Waelkens, C. ^{[2
]}

Groenewegen, M.A.T. ^{[3
]}

Barlow, M.J. ^{[4
]}

机构：

[1] Institut d'Astrophysique et de Géophysique, Université de Liège, Quartier Agora, Allée du 6 aoû, 19C-Bât. B5c, Liège (Sart-Tilman),4000, Belgium

[2] Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, Leuven,3001, Belgium

[3] Koninklijke Sterrenwacht van België, Ringlaan 3, Brussels,1180, Belgium

[4] Department of Physics and Astronomy, University College London, Gower Street, London,WC1E 6BT, United Kingdom

来源：

Astronomy and Astrophysics | 2016年 / 588卷

关键词：

Infrared Herschel imaging and spectroscopic observations of the nebula M1-67 around the Wolf-Rayet star WR 124 have been obtained along with optical imaging observations. The infrared images reveal a clumpy dusty nebula that extends up to 1 pc. The comparison with the optical images shows that the ionized gas nebula coincides with the dust nebula; the dust and the gas being mixed together. A photodissociation region is revealed from the infrared spectroscopic analysis. The analysis of the infrared spectrum of the nebula; where forbidden emission lines of ionized elements were detected; showed that the nebula consists of mildly processed material with the calculated abundance number ratios being N/O = 1.0 ± 0.5 and C/O = 0.46 ± 0.27. Based on a radiative transfer model; the dust mass of the nebula was estimated to be 0.22 Mo with a population of large grains being necessary to reproduce the observations. The comparison of the mass-loss rate and the abundance ratios to theoretical models of stellar evolution led to the conclusion that the nebular ejection took place during a RSG/YSG evolutionary phase of a central star with an initial mass of 32 Mo. © ESO; 2016;

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