HOT GAS LINES IN T TAURI STARS

For Classical T Tauri Stars (CTTSs), the resonance doublets of Nv, Si IV, and C IV, as well as the He II 1640 A line, trace hot gas flows and act as diagnostics of the accretion process. In this paper we assemble a large high-resolution, high-sensitivity data set of these lines in CTTSs and Weak T T...

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Published inThe Astrophysical journal. Supplement series Vol. 207; no. 1; pp. 1 - 43
Main Authors Ardila, David R, Herczeg, Gregory J, Gregory, Scott G, Ingleby, Laura, France, Kevin, Brown, Alexander, Edwards, Suzan, Johns-Krull, Christopher, Linsky, Jeffrey L, Yang, Hao
Format Journal Article
LanguageEnglish
Published United States American Astronomical Society 01.07.2013
Subjects
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COMPARATIVE EVALUATIONS
Correlation
DENSITY
Diagnostic systems
GAS FLOW
HELIUM IONS
LUMINOSITY
NITROGEN IONS
PHOTOSPHERE
Physics
PROTOPLANETS
RED SHIFT
SENSITIVITY
SILICON
SILICON IONS
STAR ACCRETION
Stars
T TAURI STARS
ULTRAVIOLET RADIATION
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Summary:For Classical T Tauri Stars (CTTSs), the resonance doublets of Nv, Si IV, and C IV, as well as the He II 1640 A line, trace hot gas flows and act as diagnostics of the accretion process. In this paper we assemble a large high-resolution, high-sensitivity data set of these lines in CTTSs and Weak T Tauri Stars (WTTSs). The sample comprises 35 stars: 1 Herbig Ae star, 28 CTTSs, and 6 WTTSs. For the overall sample, the Si IV and Nv line luminosities are correlated with the C IV line luminosities, although the relationship between Si iv and C iv shows large scatter about a linear relationship and suggests that TW Hya, V4046 Sgr, AA Tau, DF Tau, GM Aur, and V1190 Sco are silicon-poor, while CV Cha, DX Cha, RU Lup, and RW Aur may be silicon-rich.
Bibliography:ObjectType-Article-1
SourceType-Scholarly Journals-1
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ISSN:0067-0049
1538-4365
DOI:10.1088/0067-0049/207/1/1