Some Limits on Cosmic-Ray Heating of H I Clouds by Magnetic Stars

Details Some Limits on Cosmic-Ray Heating of H I Clouds by Magnetic Stars Some Limits on Cosmic-Ray Heating of H I Clouds by Magnetic Stars

Oct 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972ap%26ss..18..403g&link_type=abstract

Astrophysics and Space Science, Volume 18, Issue 2, pp.403-407

Astronomy and Astrophysics

Astrophysics

Scientific paper

Estimates are made of the low-energy, cosmic-ray power generated by the rotational braking of magnetic Ap stars through interaction with the interstellar medium. The resulting cosmic-ray power density (≲1.4×10-29 J s-1 m-3) in the galactic plane is at least three orders too small to maintain the observed kinetic temperatures (˜100 K) of Hi clouds. About 0.4% of Hi clouds contain an Ap star; in such cases ˜1026 J s-1 may be generated by the star during the early part of its Main Sequence life-time, but this makes only a small contribution to the heating of the cloud.

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