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Star Formation: Can There BE a Break in the IMF Near 0.1Mʘ?

Published online by Cambridge University Press:  14 August 2015

Takenori Nakano
Takenori Nakano*
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory Nobeyama, Minamimaki, Minamisaku, Nagano 384-13, Japan

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The initial mass function of stars (IMF) at small masses depends on several factors. First, it depends on the mass function of cloud cores in which stars form. Second, there must be a lower limit to the core mass for contraction; very small mass cores may not contract even if they exist. This must affect greatly the IMF near its lower end. Third, not all core matter may become stars; we must determine the stellar mass M* , or the star formation efficiency M*/Mcc, as a function of the mass of the cloud core, Mcc. In this paper we discuss the second and third points.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 11 , Issue 1: Highlights of Astronomy. As presented at the XXIIIrd General Assembly of the IAU (Part A), 1997 , 1998 , pp. 425 - 426
Copyright
Copyright © Kluwer 1998

References

André, P., Ward-Thompson, D., Barsony, M. 1993, ApJ, 406, 122.Google Scholar
D’Antona, F., Mazzitelli, I. 1985, ApJ, 296, 502.Google Scholar
D’Antona, F., Mazzitelli, I. 1994, ApJS, 90, 467.Google Scholar
Hayashi, C., Nakano, T. 1963, Prog. Theor. Phys., 30, 460.Google Scholar
Nakano, T. 1998, ApJ, in press.Google Scholar
Nakano, T., Hasegawa, T., Norman, C. 1995, ApJ, 450, 183.Google Scholar
Shu, F.H.. Adams, F.C., Lizano, S. 1987, ARAA, 25, 23.Google Scholar