Stellar granulation. I - The observability of stellar photospheric convection

Details Stellar granulation. I - The observability of stellar photospheric convection Stellar granulation. I - The observability of stellar photospheric convection

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...172..200d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 172, no. 1-2, Jan. 1987, p. 200-224. Research supported by the Naturvetenskapl

Astronomy and Astrophysics

Astrophysics

43

Convection Currents, Photosphere, Solar Granulation, Spectral Line Width, Stellar Atmospheres, Stellar Spectrophotometry, Absorption Spectra, Line Shape, Radial Velocity, Sunlight

Scientific paper

The application of astrophysical techniques, data analysis methods, and theoretical tools to investigate the stellar equivalent of solar granulation is considered. The aim is to study stellar photospheric convection patterns, the ensuing atmospheric inhomogeneities, and their effects on other observable parameters. Through experimental observations of sunlight, the ESO coude echelle spectrometer (in the special double-pass scanner mode) has been shown to be adequate for this task. The spectrometer, its performance, and its mode of operation are described. The selection of spectral lines is discussed for seven program stars (Sirius, Canopus, Procyon, Beta Hydri, Alpha Cen A, Alpha Cen B, and Arcturus). Examples are shown of observed stellar line profiles and the asymmetry of these line profiles is described by the computed line bisectors. The stellar bisector patterns for differently strong lines turn out to constitute a characteristic signature for each spectral type.

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