Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010mnras.408..293f&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 408, Issue 1, pp. 293-299.
Astronomy and Astrophysics
Astronomy
1
Mhd, Waves, Methods: Numerical, Stars: Chromospheres, Stars: Coronae, Stars: Magnetic Field
Scientific paper
A modified theory of turbulence generation is combined with the magnetohydrodynamic equations to numerically compute the wave energies generated at the base of magnetic flux tubes for stars with effective temperatures ranging from Teff = 3000 to 7000K, gravity logg = 4.44 and with different metal abundances: solar, 0.1, 0.01 and 0.001 of solar metallicity. The results show that the effect of metallicity is very important for cool stars (Teff < 5500K). The current numerical approach allows for non-linear waves with large amplitudes and thus the obtained results for time-averaged wave energy fluxes are higher than those obtained by the analytical approach. For hot stars the effect is negligible. The computed energy fluxes are essential for constructing theoretical models of the magnetic chromosphere of low-metallicity stars. The maximum obtained wave energy flux for low-metallicity stars is about 7.3 × 108 erg cm-2 s-1.
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