Section 3.1 The properties of giant molecular clouds are summarized in
Blitz, L. 1993, in Protostars and Planets III, ed. E. H. Levy and J. I. Lunine (Tucson: U. of Arizona Press), p. 125.
Much of the data on these clouds comes from large-scale CO surveys, such as that of Solomon, P. M. & Rivolo, A. R. 1989, ApJ, 339, 919.
Section 3.2 The role of the magnetic field in the virial theorem is covered by
Shu, F.H. 1991, The Physics of Astrophysics, Vol. II: Gas Dynamics, (Mill Valley: University Science Books), Chapter 24.
Section 3.3 A cogent summary of dense cores and Bok globules, written from an observational perspective, is
Myers, P. C. 1995, in Molecular Clouds and Star Formation, ed. C. Yuan and J. You (Singapore: World Scientific), p. 47.
Historically, the significance of the globules in star formation was first recognized in the prescient work of
Bok, B. J. & Reilly, E. F. 1947, ApJ, 105, 255.
Our discussion of B335 is based on the comprehensive study by
Frerking, M. A., Langer, W. D., & Wilson, R. W. 1987, ApJ, 313, 320.
The relation between cloud sizes and velocity dispersions was first uncovered by
For the three-dimensional shapes of dense cores, see
Ryden, B. S. 1996, ApJ, 471, 822, which also contains earlier references. The use of dust emission to probe internal structure is exemplified by
André, P., Ward-Thompson, D., & Motte, F. 1996, AA, 314, 625.
The Formation of Stars
Steven W. Stahler and Francesco Palla © 2004 WILEY-VCH Verlag GmbH & Co.
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