Astrophysics and Space Science

, Volume 3, Issue 1, pp 150–159 | Cite as

Mass loss from coronae and its effect upon stellar rotation

  • Kyoji Nariai


The acoustic energy-generation rate from the convective zone was calculated for various models. Results show that chromosphere and corona can be expected around stars with temperature lower than 8000K at the main sequence, and lower than 6500K at logg=2.

When a star is rotating rapidly, mass loss from its corona is large, and can be an effective mechanism of braking the stellar rotation. If this mechanism is effective, we can explain the slow rotation of stars later than F2 to be the result of the loss of the angular momentum through a stellar wind that is effective in their main sequence phase. Stars with massM>1.5M lose mass through a stellar wind during their contraction phase. The mass-loss rate is larger than the solar value because of the larger energy input into the chromosphere-corona system and because of the smaller gravitational potential at the surface. T Tauri stars may be the observational counterparts for such stars. As the duration of contraction phase is very short (less than 107 years), the braking mechanism works only in the presence of a strong magnetic field (Ap) or in the presence of a companion (Am).


Magnetic Field Mass Loss Angular Momentum Energy Input Gravitational Potential 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© D. Reidel Publishing Company 1969

Authors and Affiliations

  • Kyoji Nariai
    • 1
  1. 1.NASA-Goddard Space Flight CenterGreenbeltUSA

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