Coronal X-ray emission and rotation of cool main-sequence stars

Details Coronal X-ray emission and rotation of cool main-sequence stars Coronal X-ray emission and rotation of cool main-sequence stars

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...294..515h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 294, no. 2, p. 515-524

Astronomy and Astrophysics

Astronomy

77

Cool Stars, Main Sequence Stars, Stellar Activity, Stellar Coronas, Stellar Rotation, X Ray Astronomy, X Ray Sources, Astronomical Photometry, Open Clusters, Rosat Mission, Sky Surveys (Astronomy), Solar Neighborhood, Stellar Magnetic Fields

Scientific paper

We analyze the coronal X-ray emission of single main sequence stars of spectral type F through M with photometrically (CaII H+K or broad-band photometry) determined rotation periods, using X-ray data from the ROSAT all-sky-survey. Our sample contains both field stars in the solar neighborhood and members of the Pleiades and Hyades open clusters. Field stars and members of the two young open clusters follow the same rotation-activity relation, i.e., we find no intrinsic dependence of coronal activity on age. Assuming a power law relationship between coronal X-ray emission and stellar rotation, we estimate a power law index close to unity. With a high level of confidence (alpha = 0.99), we find a qualitative change in behavior around Rossby number values R0 approximately equals 1. For R0 greater than 1, coronal activity drops more rapidly with increasing Rossby number as for R0 less than 1. Assuming an exponential relation between the Lx/Lbol ratios and Rossby number, R0 approximately equals 1/3 is the characteristic Rossby number for a drop of X-ray activity.

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