Other
Scientific paper
Feb 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...253..666e&link_type=abstract
Astrophysical Journal, Part 1, vol. 253, Feb. 15, 1982, p. 666-678.
Other
39
B Stars, Interstellar Matter, Nebulae, O Stars, Radiation Pressure, Star Distribution, Stellar Envelopes, Absorptivity, Equations Of Motion, Kinetic Energy, Radiant Flux Density, Stellar Evolution
Scientific paper
Radiation pressure from field stars can exert an outward force on a large shell of gas and dust in the interstellar medium. This radiative force increases with increasing shell size, so a sufficiently large shell can expand at an ever-increasing speed up to a kiloparsec or more in size. The supershells that are observed in our Galaxy and in other galaxies could have originated as smaller shells around OB associations or star complexes and then have grown to their kiloparsec sizes by radiation pressure from background starlight. The formation times for such supershells are between 50 and 100 million years, so the OB associations that initially triggered their growth may not be visible anymore. Background starlight alone can give a giant shell a kinetic energy of 10 to the 51st ergs or more.
Chiang Wei-Hwan
Elmegreen Bruce G.
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