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New Light on Dark Stars pp 341–389Cite as

Brown dwarfs

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Part of the book series: Astronomy and Planetary Sciences ((ASTRONOMY))

Abstract

The existence of substellar-mass, star-like objects was first considered seriously by Kumar [K11] (Section 3.3), who outlined their essential properties: no central energy source due to hydrogen fusion, degeneracy and short luminous lifetimes. Like low-mass M dwarfs, these objects — renamed ‘brown dwarfs’ by Tarter [T1] — are ideal baryonic dark matter candidates, and have been the targets of a wide variety of surveys over the last three decades. As with any search for a newly-hypothesised object, the first task is to determine whether any exist. In answering this question, one can utilise all available techniques, without regard to the complications of biases and selection effects. However, once the issue of existence has been answered in the affirmative, the emphasis of observational programmes must change, moving from simple discovery searches to addressing specific issues through statistically well-controlled surveys. With the near-contemporaneous discoveries of Gl 229 B and the planet orbiting 51 Peg, both brown-dwarf and planet surveys have moved from the first to the second stage. Early results from the DENIS, 2MASS and SLOAN sky surveys are providing the data necessary for a transition from phenomenology to statistics.

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  1. Formerly of Edinburgh University, Royal Observatory, Edinburgh, Scotland

    Dr I. Neill Reid

  2. Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan, USA

    Dr Suzanne L. Hawley (Associate Professor)

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Reid, I.N., Hawley, S.L. (2000). Brown dwarfs. In: New Light on Dark Stars. Astronomy and Planetary Sciences. Springer, London. https://doi.org/10.1007/978-1-4471-3663-7_9

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