Saturation of Magnetic Flux Generation at low Rossby Numbers: The M Stars

Details Saturation of Magnetic Flux Generation at low Rossby Numbers: The M Stars Saturation of Magnetic Flux Generation at low Rossby Numbers: The M Stars

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..728r&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Physics

Stellar Activity, Magnetic And Electric Fields, Polarization Of Starlight, X-Ray

Scientific paper

We present magnetic flux measurements in a sample of M dwarfs including rapid rotators. In this work, we add seven stars with high X-ray and H-alpha emission. Our measurements are made using near-infrared FeH molecular spectra observed with HIRES at Keck. Because of their large convective overturn times, the rotation velocity of M stars with small Rossby numbers is relatively slow and does not hamper the measurement of Zeeman splitting. The Rossby numbers of our sample stars are as small as 0.01. We find that magnetic flux saturates in the same regime as saturation of coronal and chromospheric emission, at a critical Rossby number of around 0.1. The filling factors of both field and emission are near unity by then. We conclude that the strength of surface magnetic fields remains independent of rotation rate below that; making the Rossby number yet smaller by a factor often has little effect. These saturated M-star dynamos generate an integrated magnetic flux of roughly 3 kG, with a scatter of about 1 kG. The relation between emission and flux also has substantial scatter.

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