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Delta-slow solution to explain B supergiant stars' winds

Published online by Cambridge University Press:  23 January 2015

M. Haucke ,
I. Araya ,
C. Arcos ,
M. Curé ,
L. Cidale ,
S. Kanaan ,
R. Venero  and
M. Kraus
M. Haucke
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, UNLP, Argentina. email: [email protected]
I. Araya
Affiliation:
Instituto de Física y Astronomía, UV, Chile.
C. Arcos
Affiliation:
Instituto de Física y Astronomía, UV, Chile.
M. Curé
Affiliation:
Instituto de Física y Astronomía, UV, Chile.
L. Cidale
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, UNLP, Argentina. email: [email protected]
S. Kanaan
Affiliation:
Instituto de Física y Astronomía, UV, Chile.
R. Venero
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, UNLP, Argentina. email: [email protected]
M. Kraus
Affiliation:
Astronomický ústav, Akademie věd České Republiky, Ondřejov, Czech Republic
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Abstract

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A new radiation-driven wind solution called δ-slow was found by Curé et al. (2011) and it predicts a mass-loss rate and terminal velocity slower than the fast solution (m-CAK, Pauldrach et al. 1986). In this work, we present our first synthetic spectra based on the δ-slow solution for the wind of B supergiant (BSG) stars. We use the output of our hydrodynamical code HYDWIND as input in the radiative transport code FASTWIND (Puls et al. 2005). In order to obtain stellar and wind parameters, we try to reproduce the observed Hα, Hβ, Hγ, Hδ, Hei 4471, Hei 6678 and Heii 4686 lines. The synthetic profiles obtained with the new hydrodynamical solutions are in good agreement with the observations and could give us clues about the parameters involved in the radiation force.

Keywords

stars: mass lossstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 104 - 105
Copyright
Copyright © International Astronomical Union 2015 

References

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