Understanding X-ray super-saturation

Details Understanding X-ray super-saturation Understanding X-ray super-saturation

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006cxo..prop.2106h&link_type=abstract

Chandra Proposal ID #08200549

Computer Science

Chandra Proposal Id #08200549

Scientific paper

X-ray emission is commonly used to measure magnetic activity in cool stars. While X-ray levels and magnetic activity levels rise with stellar rotation rate, X-ray luminosities actually decline or "super-saturate" in the most rapidly rotating stars. Conflicting theories have been used to explain this: e.g., magnetic dynamos are inhibited, surface fields are more confined or their heating is less efficient, or emission is reduced due to centrifugal stripping of the outer corona. We will test different explanations of super-saturation through a multi-wavelength study of the star, AP 139. By comparing rotational modulation in its X-ray lightcurves and temperatures with maps of surface activity we can learn if and how this phenomenon is related to changes in the star's surface fields.

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