Magnetic structure in cool stars. IV - Rotation and CA II H and K emission of main-sequence stars

Details Magnetic structure in cool stars. IV - Rotation and CA II H and K emission of main-sequence stars Magnetic structure in cool stars. IV - Rotation and CA II H and K emission of main-sequence stars

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...107...31m&link_type=abstract

Astronomy and Astrophysics, vol. 107, no. 1, Mar. 1982, p. 31-35. Research supported by the Netherlands Foundation for Astronom

Astronomy and Astrophysics

Astrophysics

79

Binary Stars, Cool Stars, H Lines, K Lines, Late Stars, Magnetic Stars, Main Sequence Stars, Stellar Rotation, Stellar Structure, Angular Velocity, Calcium, Chromosphere, Line Spectra, Spectrum Analysis, Stellar Spectra, Stellar Temperature

Scientific paper

The measured Ca II H and K emission indices of stars are converted to surface fluxes (FH + FK). This conversion largely eliminates the dependence on spectral type in the relation between the uncorrected Ca II H and K emission and the rotational velocity of a star which has been found by Vaughan et al. This relation holds for single main-sequence stars as well as for short-period binaries indicating that the enhanced emission in short-period binaries is a result of rapid rotation enforced by tidal coupling. A plot of surface fluxes against υ sin i values suggests a color-dependent discontinuity in the relation. This discontinuity may explain the two branches in (FH + FK) for (B-V) < 1.00 among main-sequence stars. From the relation between (FH + FK) and rotational velocity it is deduced that the average rotational velocity of late-type main-sequence Hyades decreases with decreasing effective temperature.

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