The faint end of the Hyades main sequence

Details The faint end of the Hyades main sequence The faint end of the Hyades main sequence

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982aj.....87..899s&link_type=abstract

Astronomical Journal, vol. 87, June 1982, p. 899-905.

Astronomy and Astrophysics

Astronomy

48

Astronomical Photometry, Main Sequence Stars, Star Clusters, Stellar Spectra, Binary Stars, Color, Dwarf Stars, Infrared Astronomy, Late Stars, Optical Emission Spectroscopy

Scientific paper

The paper presents BVRIJHK photometry and optical spectroscopy of low-mass stars in the Hyades cluster. A cluster main sequence to Mv = 13.5 m is determined, where M = 0.2 solar masses. A number of Hyades stars are proposed as probable binaries, and it is suggested that most of the late-type stars detected by Stern et al. (1981) are binaries. Of the five certain Hyades X-ray detections of stars later than M0, three are high-probability binaries and another is a possible binary. It is also suggested that those Hyades sources that are relatively strong X-ray sources are in close binary systems and have been spun up relative to single Hyades M dwarfs, their enhanced X-ray and chromospheric activity being a product of their increased angular momentum.

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