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Age-rotation relationship for late-type main-sequence starsWith advancing spectral type and increasing age, late main-sequence stars exhibit monotonic decrease in rotational velocity. It is of great interest to extend the rotation-age relationship to stars of later spectral type. In recent times it has become possible to measure directly the rotational periods from the photometric modulation by Ca II H and K line emission. There have also been successful attempts to relate the chromospheric activity as manifested through Ca II H and K lines to the rotation period, and it was shown that the fraction of total stellar luminosity in Ca II H and K lines, corrected for photospheric contribution, is a function of a single parameter related to P and B-V. In the present investigation, this rotation-activity relation is utilized to infer the rotation periods as a function of spectral type. The period versus B-V plot is employed as a basis to infer that the rotational period of main-sequence stars is a single-valued function of mass (B-V color) and age.
Document ID
19840065171
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Rengarajan, T. N.
(Tata Institute of Fundamental Research, Bombay, India; Harvard-Smithsonian Center for Astrophysics, Cambridge MA, United States)
Date Acquired
August 12, 2013
Publication Date
August 15, 1984
Publication Information
Publication: Astrophysical Journal, Part 2 - Letters to the Editor
Volume: 283
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
84A47958
Funding Number(s)
CONTRACT_GRANT: NAGW-17
Distribution Limits
Public
Copyright
Other

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