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Hydrodynamic solutions of radiation driven wind from hot stars

Published online by Cambridge University Press:  16 August 2023

M. Curé Open the ORCID record for M. Curé [Opens in a new window] ,
I. Araya Open the ORCID record for I. Araya [Opens in a new window] ,
C. Arcos Open the ORCID record for C. Arcos [Opens in a new window] ,
N. Machuca  and
A. Rodriguez
M. Curé
Affiliation:
Instituto de Fsica y Astronoma, Universidad de Valparaso, Chile
I. Araya
Affiliation:
Vicerrectora de Investigación, Universidad Mayor, Chile
C. Arcos
Affiliation:
Instituto de Fsica y Astronoma, Universidad de Valparaso, Chile
N. Machuca
Affiliation:
Instituto de Fsica y Astronoma, Universidad de Valparaso, Chile
A. Rodriguez
Affiliation:
Instituto de Fsica y Astronoma, Universidad de Valparaso, Chile
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Abstract

We show the application of the δ- and Ω-slow hydrodynamical solutions to describe the velocity profiles of massive stars. In particular, these solutions can help to unravel some of the problems within the winds of massive stars such as the approximation of the β-law for the velocity profile of B supergiant stars and the slow outflow wind observed in Be stars.

Keywords

stars: early-typestars: windsoutflowsstars: mass lossstars: atmosphereshydrodynamics
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S370: Winds of Stars and Exoplanets , August 2021 , pp. 191 - 193
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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References

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