The morphology of reversed spectral-line bisectors

Details The morphology of reversed spectral-line bisectors The morphology of reversed spectral-line bisectors

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989pasp..101..832g&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 101, Sept. 1989, p. 832-838. Research supported by NSER

Computer Science

Numerical Analysis

19

Astronomical Spectroscopy, Solar Granulation, Stellar Atmospheres, Convection, Hertzsprung-Russell Diagram, Numerical Analysis, Stellar Spectra, Velocity Distribution

Scientific paper

Spectral-line asymmetries of stars on the hot side of the granulation boundary in the H-R diagram are contrasted with those on the cool side by comparing the line bisectors of 41 Cyg to those of Alpha CMi. The reversed line bisectors for stars on the hot side of the boundary are interpreted to indicate large upward-stream velocities, about -10 to -20 km/s, over a small time-averaged fraction of the surface, equal to about 10 percent. Scaling properties of the bisectors imply no differential velocities within the up-flow.

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