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Pulsations as a mass-loss trigger in evolved hot stars†

Published online by Cambridge University Press:  18 February 2014

Michaela Kraus ,
Dieter H. Nickeler ,
Maximiliano Haucke ,
Lydia Cidale ,
Roberto Venero ,
Marcelo Borges Fernandes ,
Sanja Tomić  and
Michel Curé
Michaela Kraus
Affiliation:
Astronomický ústav, Akademie věd České Republiky, Fričova 298, 251 65 Ondřejov, Czech Republic email: [email protected]
Dieter H. Nickeler
Affiliation:
Astronomický ústav, Akademie věd České Republiky, Fričova 298, 251 65 Ondřejov, Czech Republic email: [email protected]
Maximiliano Haucke
Affiliation:
Departamento de Espectroscopía Estelar, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, B1900FWA, La Plata, Argentina
Lydia Cidale
Affiliation:
Departamento de Espectroscopía Estelar, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, B1900FWA, La Plata, Argentina Instituto de Astrofísica de La Plata, CCT La Plata, CONICET-UNLP, Paseo del Bosque s/n, B1900FWA, La Plata, Argentina
Roberto Venero
Affiliation:
Departamento de Espectroscopía Estelar, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, B1900FWA, La Plata, Argentina Instituto de Astrofísica de La Plata, CCT La Plata, CONICET-UNLP, Paseo del Bosque s/n, B1900FWA, La Plata, Argentina
Marcelo Borges Fernandes
Affiliation:
Observatório Nacional, Rua General José Cristino 77, 20921-400 São Cristovão, Rio de Janeiro, Brazil
Sanja Tomić
Affiliation:
Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade, Serbia
Michel Curé
Affiliation:
Departmento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, Casilla 5030, Valparaíso, Chile
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Abstract

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During their post-main sequence evolution, massive stars pass through several short-lived phases, in which they experience enhanced mass loss in the form of clumped winds and mass ejection events of unclear origin. The discovery that stars populating the blue luminous part of the Hertzsprung-Russell diagram can pulsate suggests that stellar pulsations might influence or trigger enhanced mass loss and eruptions. We present recent results for two objects in different phases: a B[e] star at the end of the main sequence and a B-type supergiant.

Keywords

stars: early-typestars: emission-linestars: Bestars: mass lossstars: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 217 - 220
Copyright
Copyright © International Astronomical Union 2014 

Footnotes

†

Based on observations acquired at the Ondřejov Observatory, Czech Republic, the Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, and with the HERMES spectrograph, which is supported by the Fund for Scientific Research of Flanders (FWO), Belgium, the Research Council of K.U.Leuven, Belgium, the Fonds National Recherches Scientific (FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland and the Thüringer Landessternwarte Tautenburg, Germany.

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