Chromospheric and coronal emissions from the giants in the Hyades

Details Chromospheric and coronal emissions from the giants in the Hyades Chromospheric and coronal emissions from the giants in the Hyades

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...271..672b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 271, Aug. 15, 1983, p. 672-680. Research supported by the Smithsonian Insti

Astronomy and Astrophysics

Astronomy

39

Chromosphere, Emission Spectra, Giant Stars, Star Clusters, Stellar Coronas, Ultraviolet Spectra, Calcium, Cool Stars, Iue, Late Stars, Spaceborne Astronomy, Stellar Spectrophotometry, Stellar Temperature

Scientific paper

The visible Ca II K and International Ultraviolet Explorer spectra from the four K0 III stars (theta-1, gamma, delta, and epsilon Tau) in the Hyades, along with a field giant of similar spectral type, beta Gem, have been measured. Among the Hyades giants, the range of the high-temperature emissions can be a factor of 6 or more for C IV and an order of magnitude in the X-ray luminosity measured by Stern et al. (1981). For these presumably coeval cluster giants with similar macroscopic parameters, such as age, mass, effective temperature, gravity, and projected rotational velocity, the observed range in chromospheric and coronal emissions is not easily explained by the dominant factors thought to control these emissions in cool stars. It is possible that the emissions are time variable, on a time scale longer than six months. This would be the first evidence that giants undergo magnetic activity cycles similar to those of dwarf stars.

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