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Low-Mass Stellar and Brown Dwarf Binary Systems

Reid, I. N. and Koerner, D. W. and Gizis, J. E. and Kirkpatrick, J. D. (2001) Low-Mass Stellar and Brown Dwarf Binary Systems. In: Ultracool Dwarfs: New Spectral Types L and T. Springer , Berlin, pp. 111-118. ISBN 978-3-642-62682-1.

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Binary systems have long been recognised as providing one of the most powerful methods of probing the physical properties of stars drawn from the full range of the HR diagram. Most notably, the overwhelming majority of measurements of mass, the fundamental stellar parameter, rest on observations of astrometric or spectroscopic binaries. For main sequence stars, those individual measurements can be combined to define a mass-luminosity relation which, applied to a suitably-constructed sample, permits derivation of Ψ(M), the mass function. The latter, in its turn, provides a valuable constraint on star formation theory by defining the end product of an assortment of processes, including collapse, fragmentation, coagulation and accretion, which combine to transform gas into stars. In similar fashion, the frequency of binaries as a function of mass and the distribution of mass ratios and separations offer important clues to the underlying mechanism(s) which conspire reduce individual molecular cloud cores to to gaseous spheres in hydrostatic equilibrium.

Item Type:Book Section
Related URLs:
URLURL TypeDescription ReadCube access
Gizis, J. E.0000-0002-8916-1972
Kirkpatrick, J. D.0000-0003-4269-260X
Additional Information:© 2001 Springer-Verlag Berlin Heidelberg.
Group:Infrared Processing and Analysis Center (IPAC)
Subject Keywords:Main Sequence Star; Brown Dwarf; Spectroscopic Binary; Molecular Cloud Core; Total System Mass
Record Number:CaltechAUTHORS:20191111-155445158
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:99788
Deposited By: Tony Diaz
Deposited On:12 Nov 2019 23:18
Last Modified:16 Nov 2021 17:49

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