Structure and Evolution of Low-mass Stars: Where Do Magnetic stars Become Completely Convective?

Details Structure and Evolution of Low-mass Stars: Where Do Magnetic stars Become Completely Convective? Structure and Evolution of Low-mass Stars: Where Do Magnetic stars Become Completely Convective?

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12..893m&link_type=abstract

The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August

Astronomy and Astrophysics

Astrophysics

Structure, Magnetic, Completely Convective

Scientific paper

Stars on the main sequence are expected to be completely convective if their mass lies below a certain value, Mcc. Standard stellar structure codes suggest that Mcc is in the range (0.3-0.4)M&sun;. However, certain physical effects that are not incorporated in standard models may alter the value of Mcc significantly. Here we quantify the alterations that are brought about in Mcc when we include magnetic field effects. In particular, we modify the criterion for convective stability in the manner prescribed by Gough and Tayler (1966). We find that magnetic M dwarfs tend to have radii that are larger than expected for their Teff values, or Teff values that are too low for their radii. Available observational data provide quantitative support for these structural findings. Moreover, we find that, given the magnetic fields which are allowed to exist stably in low-mass stars, Mcc may fall to values that are as small as 0.1M&sun;. We suggest that this result is pertinent to understanding why coronae and chromospheres in active M dwarfs fail to exhibit detectable alterations at spectral class M3-M4.

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