Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...345..464n&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 345, Oct. 1, 1989, p. 464-471.
Astronomy and Astrophysics
Astrophysics
66
Star Formation, Stellar Envelopes, Stellar Magnetic Fields, Stellar Mass Accretion, Thermal Radiation, Cosmic Dust, Dynamic Pressure, Magellanic Clouds, Main Sequence Stars, Milky Way Galaxy
Scientific paper
Formation of massive stars through spherical accretion has been predicted to occur only in clouds which are nearly dust-free and can provide an extremely high accretion rate. It is shown that such severe restrictions are effectively removed with nonspherical accretion. By the effects of magnetic fields, rotation, and so on, the contracting envelope usually becomes rather flat. With such a configuration the thermal radiation converted from the stellar radiation by dust near its sublimation zone easily escapes from the envelope and then hardly affects the motion of dust and gas. Consequently, the gas falls nearly freely to the sublimation zone. The steady inflow occurs only when the dynamical pressure of this motion is greater than the stellar radiation pressure at this zone. With the present model the accretion onto a stellar core of 100 solar mass occurs when the accretion rate is greater than 0.0001 solar mass/yr, 50 times smaller than the rate with spherical accretion. No special restrictions on grain abundances are required, in contrast to spherical accretion. The causes for the rarity of massive stars are discussed.
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