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April 1, 2026Open Access

Rotating, Magnetic, Radiatively Driven Stellar Winds. 1. Basic Equations

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Authors

YSYasumichi Saito

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Overview

This analysis models radiatively driven winds in stars, revealing key singular points affected by radiation terms.

Key Points

  • The aim is to formulate and analyze basic equations for radiatively driven stellar winds influenced by magnetic fields.
  • Develop a model of magnetohydrodynamic wind flow in the equatorial plane of a star.
  • Analyze the basic equations to identify singular points.
  • Examine the influence of rotation on the existence of magnetosonic points.
  • Identified critical points as slow magnetosonic, Alfvenic, and fast magnetosonic.
  • The radiation terms modify the locations of the magnetosonic points.
  • The slow magnetosonic point does not appear outside the star when rotation is below break-up velocity.

Cite This Study

Yasumichi Saito (1990) studied this question.

synapsesocial.com/papers/69cd7ad45652765b073a8422https://doi.org/10.15113/00011748
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