Titlebook: New Light on Dark Stars; Red Dwarfs, Low-Mass I. Neill Reid,Suzanne L. Hawley Book 20001st edition Springer-Verlag London 2000 Galaxy.astro

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The stellar luminosity function,for understanding star formation and investigating the structure of our Galaxy. In recent years, most emphasis has been placed on determining the shape of Φ(M) at faint magnitude — and hence the mass spectrum, with the ultimate goal of assessing the likely dark-matter contribution of VLM stars and b

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Brown dwarfs,es: 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.

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Epilogue, which numerically dominate the Galactic disk stellar population. Neither of us anticipated the explosion of discoveries of cool, lower-mass brown dwarfs, requiring the addition of two new spectral classes, and, almost simultaneously, the first detections of extrasolar planets. We have, as far as po

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own dwarf.Comprehensive discussion of the statistical and asPerhaps the most common question that a child asks when he or she sees the night sky from a dark site for the first time is: ‘How many stars are there?‘ This happens to be a question which has exercised the intellectual skills of many astro

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The stellar luminosity function,e of Φ(M) at faint magnitude — and hence the mass spectrum, with the ultimate goal of assessing the likely dark-matter contribution of VLM stars and brown dwarfs. However, it was Galactic structure analyses, rather than an interest in the relative number of luminous and faint stars ., which prompted the first derivation of the luminosity function.