MHD wave energy fluxes for late-type dwarfs

  • R. Rosner
  • Z. E. Musielak
General Discussion: The Role of Magnetic Fields
Part of the Lecture Notes in Physics book series (LNP, volume 291)


We calculate the efficiency of MHD wave generation by turbulent motions in the stratified stellar atmospheres of late-type main sequence stars, under the assumption that the embedded magnetic fields are uniform. In contradiction with previous results, we show that there is no significant increase in the efficiency of wave generation because of the presence of magnetic fields, at least within the theory's limits of applicability. Thus, we show that MHD energy fluxes for late-type stars whose surface magnetic fields are uniform are less than those obtained for acoustic waves in a magnetic field-free atmosphere, and do not vary enough for a given spectral type in order to explain observed UV and X-ray fluxes. Thus, our results show that MHD energy fluxes obtained if stellar surface magnetic fields are uniform cannot explain the observed stellar coronal emissions.


Energy Flux Spectral Type Convective Zone Background Magnetic Field Surface Magnetic Field 
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Copyright information

© Springer-Verlag 1987

Authors and Affiliations

  • R. Rosner
    • 1
  • Z. E. Musielak
    • 2
  1. 1.Harvard-Smithsonian Center for AstrophysicsUSA
  2. 2.Space Science LaboratoryNASA Marshall Space Flight CenterUSA

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