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Hydrodynamic disk solutions for Be stars using HDUST

Published online by Cambridge University Press:  16 August 2023

C. Arcos Open the ORCID record for C. Arcos [Opens in a new window] ,
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] ,
A. Rubio  and
A. Carciofi
C. Arcos
Affiliation:
Instituto de Física y Astronomía, Universidad de Valparaíso, Chile
M. Curé
Affiliation:
Instituto de Física y Astronomía, Universidad de Valparaíso, Chile
I. Araya
Affiliation:
Vicerrectoría de Investigación, Universidad Mayor, Chile
A. Rubio
Affiliation:
Instituto de astronomia, geofísica e ciências atmosféricas, Universidade de São Paulo, Brazil
A. Carciofi
Affiliation:
Instituto de astronomia, geofísica e ciências atmosféricas, Universidade de São Paulo, Brazil
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Abstract

. In this work, we implemented a hydrodynamical solution for fast rotating stars, which leaves high values of mass-loss rates and low terminal velocities of the wind. This 1D density distribution adopts a viscosity mimicking parameter which simulates a quasi-Keplerian motion. Then, it is converted to a volumetric density considering vertical hydrostatic equilibrium using a power-law scale height, as usual in viscous decretion disk models. We calculate the theoretical hydrogen emission lines and the spectral energy distribution utilizing the radiative transfer code HDUST. Our disk-wind structures are in agreement with viscous decretions disk models.

Keywords

stars: emission-lineBestars: windsoutflowshydrodynamics
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S370: Winds of Stars and Exoplanets , August 2021 , pp. 168 - 173
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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