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Simultaneous observations of Ca II K and Mg II k in T Tauri starsThe first simultaneous, calibrated observations of the Ca II K and Mg II k resonance lines in T Tauri stars are presented. It is found that for T Tauri stars with mass greater than 1.5 solar mass, which have radiative cores and tend to be fast rotators, the k line seems to arise in an extended region (probably also responsible for the H-alpha emission), whereas the K line apparently originates closer to the highly inhomogeneous stellar surface. The lower mass stars, which are fully convective and tend to be slow rotators, are more easily described by a largely chromospheric model, consistent with main-sequence activity structures but at greater values of the nonradiative flux. The strongest emission-line stars in the low-mass group, however, are also likely to have extended k line regions.
Document ID
19850056895
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Calvet, N.
(Centro de Investigacion de Astronomia Merida, Venezuela)
Basri, G.
(California, University Berkeley, CA, United States)
Imhoff, C. L.
(Computer Sciences Corp. Greenbelt, MD, United States)
Giampapa, M. S.
(National Solar Observatory Tucson, AZ, United States)
Date Acquired
August 12, 2013
Publication Date
June 15, 1985
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 293
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
85A39046
Funding Number(s)
CONTRACT_GRANT: NAS5-25774
CONTRACT_GRANT: NSF AST-81-06094
Distribution Limits
Public
Copyright
Other

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