By Christopher Wills
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Extra info for The Spark Of Life: Darwin And The Primeval Soup
J. Letters, 211, L69. J. 1985, preprint. Larson, R. S. (in press). B. S. 194, 809. Layzer, D. J. 131,351. Levreault, R. M. , 211,634. Mathieu, R. J. Letters, 261, L97. Myers, P. J. 210, 105. Norman, C. and Silk, J. , 238, 158. , Stahler, S. E. , 271, 632. J. , 176,483. Rowan-Robinson, M. , 234, 111. Rozyczka, M. 1983, Astr. , 125, 45. Scalo, J. 1985, preprint. Silk, J. J, 256, 514. Silk, J. , 211,638. PHYSICAL PROCESSES IN STAR FORMATION Silk, J. 1980, in Star Formation, eds. A. Maeder and 1. Martinet (Geneva: Geneva Observatory), p 133.
The key to cloud support and longevity undoubtedly lies in understanding the origin of the suprathermal line widths. These yield enough dynamical pressure to give support against collapse. Yet supersonic turbulence would dissipate very rapidly, within a cooling time, or in much less than the collapse PHYSICAL PROCESSES IN ST AR FORMATION 37 time-scale. A promising source of internal energy input that may be capable of keeping clouds from collapse consists of premain sequence objects generating strong winds (Norman and Silk 1980).
Indeed, not a single genuine protostar has been discovered, despite intensive infrared searches. In this brief review of star formation processes, I will emphasize aspects that are most relevant for constructing models of galaxy evolution. In particular, I will discuss constraints from observations of molecular clouds, and the initial mass function, large-scale star formation processes, and cloud support and fragmentation. II. CONSTRAINTS FROM MOLECULAR CLOUD OBSERVATIONS Cloud properties are summarized in Table 1.