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Formation of OB Stars by Radiatively-Driven Implosion

Published online by Cambridge University Press:  04 August 2017

R.I. Klein ,
C.F. McKee ,
M.T. Sandford ,
R. Whitaker  and
P.T.P. Ho
R.I. Klein
Affiliation:
UC, Lawrence Livermore Natl. Lab., Livermore, CA 94550 USA
C.F. McKee
Affiliation:
Phys. Dept. UC, Berkeley, CA 94720 USA
M.T. Sandford
Affiliation:
Los Alamos Natl. Lab., Los Alamos, NM 87545 USA
R. Whitaker
Affiliation:
Los Alamos Natl. Lab., Los Alamos, NM 87545 USA
P.T.P. Ho
Affiliation:
Dept. of Astron. Harvard University, Cambridge, MA 02138 USA

Extract

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A theory for the sequential formation of OB stars in dense molecular clouds was first quantitatively investigated by Elmegreen and Lada (1976). The model was one-dimensional in nature and assumed shock propagation into homogeneous clouds. This picture has provided a successful explanation of the morphology of the Ori OB1 association.

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 435 - 437
Copyright
Copyright © Reidel 1987 

References

Elmegreen, B.G., and Lada, C.J.: 1977, Astrophys. J. 214, 723.Google Scholar
Ho, P., Klein, R.I., and Haschick, A.: 1986, to appear in Astrophys. J. Letters.Google Scholar
Klein, R.I., Sandford, M.T., and Whitaker, R.: 1983, Astrophys. J. 271, 269.Google Scholar
Klein, R.I., Whitaker, R., and Sandford, M.T.: 1985, Chapter in Protostars and Planets II, Ariz. Press, Ed. Black, D. Google Scholar
Stark, A.A., and Blitz, L.: 1978, Astrophys. J. Letters 225, L15.Google Scholar