Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1974
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974a%26a....37..149k&link_type=abstract
Astronomy and Astrophysics, vol. 37, no. 1, Dec. 1974, p. 149-162.
Astronomy and Astrophysics
Astronomy
212
Cosmic Dust, Early Stars, Interstellar Matter, Mass Ratios, Stellar Envelopes, Astronomical Models, Black Body Radiation, Flow Characteristics, Infrared Astronomy, Interstellar Gas, Opacity, Radiation Pressure, Stellar Evolution, Stellar Luminosity
Scientific paper
A cocoon will form around any star which is accreting interstellar matter at a large enough rate. The interstellar grains in the cocoon absorb the direct starlight, and re-emit in the infra-red. In many cases the cocoon is also opaque to this reradiated radiation, and therefore a gradient of radiation pressure builds up and retards the infalling material. As the mass of the central star grows, and its luminosity-to-mass ratio increases, this effect becomes more important. Eventually the retardation becomes so severe that the infalling gas and dust mixture cannot cross the surface where the grains melt. Once this has happened, the flow is turned back and a dense shell of interstellar mixture begins to be driven away from the star. However, the shell is unstable, and will probably break up into fragments. This process sets a limit to the luminosity to mass ratio L:M of those stars which can accrete interstellar matter.
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