Turbulent Dynamos and the Minimum X-ray Flux in Solar-Type Main Sequence Stars

Details Turbulent Dynamos and the Minimum X-ray Flux in Solar-Type Main Sequence Stars Turbulent Dynamos and the Minimum X-ray Flux in Solar-Type Main Sequence Stars

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp43b..01b&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP43B-01

Astronomy and Astrophysics

Astronomy

7524 Magnetic Fields, 7539 Stellar Astronomy, 7544 Stellar Interiors And Dynamo Theory

Scientific paper

We investigate whether a small-scale turbulent dynamo can account quantitatively for the observed lower limit of X-ray surface flux in solar-type main sequence stars. Our approach is to use 3D numerical simulations of a turbulent dynamo driven by convection to characterize the dynamic behavior, magnetic field strengths, and filling factors in a non-rotating stratified medium, and to predict these magnetic properties at the surface of cool stars. We use simple applications of stellar structure theory for the convective envelopes of main-sequence stars to scale our simulations to the outer layers of stars in the F0--M0 spectral range, which allows us to estimate the unsigned magnetic flux on the surface of non-rotating reference stars. With these estimates we use the observed magnetic flux--X-ray flux correlation of Pevtsov et al. (2003) to predict the level of X-ray emission from such a turbulent dynamo, and find that our results compare well with observed lower limits of surface X-ray flux. This suggests that dynamo action from a convecting, non-rotating plasma is a viable alternative to acoustic heating models as an explanation for the basal emission level seen in chromospheric, transition region, and coronal diagnostics from late-type stars.

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