An explanation of the 'granulation boundary' in the HR diagram

Details An explanation of the 'granulation boundary' in the HR diagram An explanation of the 'granulation boundary' in the HR diagram

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..126..201d&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 126, March 1990, p. 201-205.

Physics

5

Hertzsprung-Russell Diagram, Solar Granulation, Stellar Gravitation, Gravity Waves, Hot Stars, Line Spectra, Stellar Spectra

Scientific paper

The granulation boundary is a line running in the HR diagram from about F0V stars to G1Ib. It divides the HR diagram in two regions in which the 'spectral line bisector' behaves differently. To the right (cooler stars) the Fraunhofer lines in stellar spectra show the characteristics typical for convective motions. For hot stars it indicates the presence of large velocities involving a large part of the line-forming region. Evidence that the opposite behavior shown by spectra of hotter stars can be explained by gravity waves is presented.

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