CHROMOSPHERIC EMISSION AND ROTATION OF THE HYADES LOWER MAIN SEQUENCE

The identity of chromospheric Ca ð H-and K-line emission has been monitored for two seasons in a large sample of Hyades F and G dwarfs. Mean emission levels vary smoothly with spectral type, suggesting that the rotation rate at a given spectral type varies relatively little, and that the rotation ra...

Full description

Saved in:
Bibliographic Details
Published inPublications of the Astronomical Society of the Pacific Vol. 96; no. 583; pp. 707 - 713
Main Authors DUNCAN, DOUGLAS K., BALIUNAS, SALLIE L., NOYES, ROBERT W., VAUGHAN, ARTHUR H., FRAZER, JAMES, LANNING, HOWARD H.
Format Journal Article
LanguageEnglish
Published Chicago, IL The Astronomical Society of the Pacific 01.09.1984
University of Chicago Press
Subjects
Acoustic spectra
Astronomy
Earth, ocean, space
Exact sciences and technology
K lines
Late type stars
Main sequence stars
Noise spectra
Normal stars (by class): general or individual
Rotation
Solar rotation
Stars
Stellar classification
Stellar rotation
Stellar chromosphere
Stellar rotation
Emission line
Late type star
Online AccessGet full text

Cover

More Information
Summary:The identity of chromospheric Ca ð H-and K-line emission has been monitored for two seasons in a large sample of Hyades F and G dwarfs. Mean emission levels vary smoothly with spectral type, suggesting that the rotation rate at a given spectral type varies relatively little, and that the rotation rate decreases smoothly as a function of mass. In this case the mechanism which controls pre-main-sequence angular momentum loss in late-type stars must be self-regulating to a high degree.
Bibliography:ObjectType-Article-2
SourceType-Scholarly Journals-1
ObjectType-Feature-1
content type line 23
ISSN:0004-6280
1538-3873
DOI:10.1086/131409