Abstract
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. We give evidence that the opposite behaviour shown by spectra of hotter stars can be explained by gravity waves.
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De Jager, C. An explanation of the ‘granulation boundary’ in the HR diagram. Sol Phys 126, 201–205 (1990). https://doi.org/10.1007/BF00158308
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DOI: https://doi.org/10.1007/BF00158308