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Simulation of a Hydrodynamic Stellar Wind from a Rapidly Rotating Star

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Abstract

The mechanism for the formation of disk-like flows from rapidly rotating Be stars is not yet clear. An axisymmetric hydrodynamic stellar wind flow from a rapidly rotating star has been simulated numerically as a step in solving this problem. The change in the shape of the star as it rotates and the turbulence excited in the stellar wind at Reynolds numbers ∼109−1013 are taken into account. Calculations show the formation of a disk-like flow from the stellar surface at the equator, which expands into the polar regions due to a pressure gradient on scales of the order of the stellar radius. A poloidal velocity vortex is formed at high latitudes. No turbulence is excited near the equator within the simplest standard models and, therefore, no quasi-Keplerian disk-like flow emerges in the equatorial plane. A dependence of the total mass flux on the stellar rotation rate at various surface temperatures has been obtained.

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Authors and Affiliations

  1. MEPhI National Research Nuclear University, Kashirskoe sh. 31, Moscow, 115409, Russia

    S. V. Bogovalov, S. M. Romanikhin & I. V. Tronin

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  1. S. V. Bogovalov
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  2. S. M. Romanikhin
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  3. I. V. Tronin
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Correspondence to S. V. Bogovalov.

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Bogovalov, S.V., Romanikhin, S.M. & Tronin, I.V. Simulation of a Hydrodynamic Stellar Wind from a Rapidly Rotating Star. Astron. Lett. 45, 81–91 (2019). https://doi.org/10.1134/S1063773719020026

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  • DOI: https://doi.org/10.1134/S1063773719020026

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