Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981msngr..23....7o&link_type=abstract
The Messenger, No.23, P. 7, 1981
Astronomy and Astrophysics
Astronomy
2
Scientific paper
Circumstellar spectral lines, especially those which directly indicate the flow of stellar material, like P Cygni lines have been observed since the beginning of our entry. The peculiar character of P Cygni itself was conspicuous on Harvard objective prism plates already in 1890. Though until today the number of these obviously mass-loosing stars grew steadily, especially since the beginning of UV astronomy, we do not know very much about the physical mechanisms which are basically responsible for the loss of stellar material. Regarding the hot stars, models are favoured in which the photospheric radiation pressure, especially in the UV, or mechanisms in stellar coronae are supposed to be the driving motors of stellar winds (see e.g. J. P. Cassinelli et al., Publications of the Astronomical Society of the Pacific, 90, 496,1978), while for the cold end of the spectral sequence, acoustic phenomena, generated in the outer stellar convection zones, seem to accelerate the outflowing masses. The medium spectral types F and G appear to show the least tendency towards mass loss. Or is it possible that the lack of suitable theories in this temperature range is at least partially responsible for the lack of systematic observations? Whether these stars are indeed more resistant to mass loss is one of the questions of our programme.
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