Convection in the photosphere of Arcturus

Details Convection in the photosphere of Arcturus Convection in the photosphere of Arcturus

Nov 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974a%26a....36..143d&link_type=abstract

Astronomy and Astrophysics, vol. 36, no. 1, Nov. 1974, p. 143-145.

Astronomy and Astrophysics

Astrophysics

18

Convective Flow, Line Spectra, Photosphere, Stellar Atmospheres, Stellar Spectra, Doppler Effect, Red Shift, Solar Atmosphere, Solar Granulation

Scientific paper

Convective motions in stellar atmospheres involve hot gases that rise, cool off and then sink back. High-excitation spectral lines are preferentially formed in the hot, rising and thus locally blue-shifted elements while low-excitation lines are preferentially formed in the cooler, sinking and red-shifted elements. By comparing accurate wavelengths for spectral lines in Arcturus with laboratory values, a relation is found, such that high-excitation lines are systematically blue-shifted relative to low-excitation lines. This relation is very similar to the one previously known for the sun and is interpreted as the existence of convection cells, similar to the solar granulation, in the photosphere of Arcturus.

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