Computer Science – Sound
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...420..392m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 420, no. 1, p. 392-400
Computer Science
Sound
27
Dwarf Stars, M Stars, Plasma Heating, Sound Waves, Stellar Coronas, Wave Propagation, X Ray Astronomy, Computerized Simulation, Hydrodynamics, Radiative Transfer, Time Dependence
Scientific paper
We use a time-dependent hydrodynamics code to follow the propagation of acoustic waves into the corona of an M dwarf star. An important qualitative difference between M dwarfs and stars such as the Sun is that the acoustic spectrum in M dwarfs is expected to peak at periods close to the acoustic cutoff PA: this allows more effective penetration of waves into the corona. In our code, radiative losses in the photosphere, chromosphere, and corona are computed using Rosseland mean opacities, Mg II kappa and Ly alpha emission, and optically thin emissivities respectively. We find that acoustic heating can maintain a corona with a temperature of order 0.7-1 x 106 K and a surface X-ray flux as large as 105ergs/sq cm/s. In a recent survey of X-rays from M dwarfs, some (20%-30%) of the stars lie at or below this limiting X-ray flux: we suggest that such stars may be candidates for acoustically maintained coronae.
Cheng Qing-Qi
Mullan Dermott J.
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