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Inferring Mass Loss Rates for Cool Luminous Stars from High-Resolution GHRS Spectra

Published online by Cambridge University Press:  25 May 2016

J. L. Linsky ,
G. M. Harper ,
J. Valenti ,
P. D. Bennett  and
A. Brown
J. L. Linsky
Affiliation:
JILA, University of Colorado and NIST, Boulder CO, 80309-0440 U.S.A.
G. M. Harper
Affiliation:
JILA, University of Colorado and NIST, Boulder CO, 80309-0440 U.S.A.
J. Valenti
Affiliation:
JILA, University of Colorado and NIST, Boulder CO, 80309-0440 U.S.A.
P. D. Bennett
Affiliation:
CASA, University of Colorado, Boulder CO, 80309-0389 U.S.A.
A. Brown
Affiliation:
CASA, University of Colorado, Boulder CO, 80309-0389 U.S.A.

Abstract

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We discuss GHRS spectra of single and binary late-type stars and describe in detail the spectra of α TrA and of ζ Aurigae obtained at ten orbital phases. The wind properties of α TrA are derived using a complete redistribution radiative transfer code, and we describe the properties of a new code, PRISMA, that we are building to fit line profiles using partial redistribution in a spherically-symmetric geometry. The ζ Aur spectra show that the mass loss process is variable on the timescale of several months, the wind density structure does not repeat from orbit to orbit, and the wind ionization structure is complex.

Type
Session VII — Mass-Loss, Winds, and Formation of Dust Grains
Information
Symposium - International Astronomical Union , Volume 177: The Carbon Star Phenomenon , 2000 , pp. 303 - 312
Copyright
Copyright © Kluwer 2000 

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