Radiatively driven winds from magnetic, fast-rotating stars
Authors
Nerney, S.
Advisors
Second Readers
Subjects
HOT STARS
MAGNETOHYDRODYNAMICS
STELLAR MAGNETIC FIELDS
STELLAR ROTATION
STELLAR WINDS
ACCELERATION (PHYSICS)
COMPUTATION
MATHEMATICAL MODELS
MOMENTUM
PROBLEM SOLVING
THOMSON SCATTERING
VELOCITY MEASUREMENT
MAGNETOHYDRODYNAMICS
STELLAR MAGNETIC FIELDS
STELLAR ROTATION
STELLAR WINDS
ACCELERATION (PHYSICS)
COMPUTATION
MATHEMATICAL MODELS
MOMENTUM
PROBLEM SOLVING
THOMSON SCATTERING
VELOCITY MEASUREMENT
Date of Issue
1986-01
Date
Jan 01, 1986
Publisher
Language
Abstract
An analytical procedure is developed to solve the magnetohydrodynamic equations for the stellar wind problem in the strong-magnetic field, optically thick limit for hot stars. The slow-mode, Alfven, and fast-mode critical points are modified by the radiation terms in the force equation but in a manner that can be treated relatively easily. Once the velocities at the critical points and the distances to the points are known, the streamline constants are determined in a straight-forward manner. This allows the structure of the wind to be elucidated without recourse to complicated computational schemes.
Type
Conference Paper
Description
SEE ParentDocumentRecord|Ntt=19860015036 "NASA. Marshall Space Flight Center Research Reports: 1985 NASA(ASEE Summer Faculty Fellowship Program"; p. 16 p
Series/Report No
Department
Organization
Unspecified Center
Identifiers
NPS Report Number
Sponsors
Funding
Format
Citation
Distribution Statement
Approved for public release; distribution is unlimited.
Rights
This publication is a work of the U.S. Government as defined in Title 17, United States Code, Section 101. Copyright protection is not available for this work in the United States.