Axial Rotation and Stellar Evolution

Details Axial Rotation and Stellar Evolution Axial Rotation and Stellar Evolution

Feb 1936

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1936natur.137..317h&link_type=abstract

Nature, Volume 137, Issue 3460, pp. 317-318 (1936).

Computer Science

Scientific paper

IF, as is now generally supposed, stars exhibiting spectra containing uniformly widened lines, commonly designated by the suffix n, are in rapid axial rotation, then the following interesting condition is imposed upon the problem of stellar evolution. It arises from the comparatively recent determination1 that a large number of the early F-type stars (as well as B and A stars) have noticeably widened lines, while but few of the later F's and practically no G or later type stars exhibit this characteristic; and that such n stars cluster closely about the absolute magnitude + 2.0, and thus, by virtue of the mass-luminosity relation, about the stellar mass of twice that of the sun.

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