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Title:
Ionization structure and emission of winds from low-luminosity pre-main-sequence stars
Authors:
Natta, A.; Giovanardi, C.; Palla, F.
Affiliation:
AA(CNR, Centro di Astronomia Infrarossa, Florence, Italy), AB(Arcetri, Osservatorio Astrofisico; CNR, Centro di Astronomia Infrarossa, Florence, Italy), AC(Arcetri, Osservatorio Astrofisico; CNR, Centro di Astronomia Infrarossa, Florence, Italy)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 332, Sept. 15, 1988, p. 921-939. Research supported by the University of Texas. (ApJ Homepage)
Publication Date:
09/1988
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
GAS TEMPERATURE, PRE-MAIN SEQUENCE STARS, STELLAR LUMINOSITY, STELLAR MASS EJECTION, STELLAR RADIATION, STELLAR WINDS, IONIZED GASES, MAGNETOHYDRODYNAMIC WAVES, RADIATION DISTRIBUTION, STELLAR ENVELOPES
DOI:
10.1086/166702
Bibliographic Code:
1988ApJ...332..921N

Abstract

This paper presents the results of an extensive set of calculations of the ionization and excitation structure in winds surrounding low-luminosity, pre-main-sequence stars. In most of the cases considered, the winds turn out to be mostly neutral. The ionization is due primarily to photoionization from excited levels. Collisional ionization plays a significant role only in winds with high mass-loss rates (10 to the -6th solar mass/yr) and gas temperatures (8000 K or higher). The degree of ionization is a strong function of Tg and of the stellar radiation field. The luminosity in hydrogen lines depends to a first approximation on mass-loss rate and on the ionization of the envelope. Because the ionization depends on properties like the gas temperature and the stellar radiation field, a large range of line luminosities among objects with similar mass-loss rates is predicted.

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