Red Dwarf Masses
نویسندگان
چکیده
منابع مشابه
The “Living with a Red Dwarf” Program
Red Dwarfs (main-sequence / dwarf M or dM) stars are the most common stars in the Galaxy. These cool, faint, low mass stars comprise over 75% of all stars. Because of their low luminosities (∼0.0008–0.06 of the Sun’s luminosity), the circumstellar habitable zones (HZs) of dM stars are located within ∼0.05–0.4 AU of the host star. Nevertheless, the prospect of life on a planet located within the...
متن کاملThe Nature of Red Dwarf Galaxies
Using dark matter halos traced by galaxy groups selected from the Sloan Digital Sky Survey Data Release 4, we find that about 1/4 of the faint galaxies ( Mr − 5 log h > −17.05, hereafter dwarfs) that are the central galaxies in their own halo are not blue and star forming, as expected in standard models of galaxy formation, but are red. Many red dwarf galaxies are physically associated with mor...
متن کاملThe “ Living with a Red Dwarf ” Program
Red Dwarfs (main-sequence / dwarf M or dM) stars are the most common stars in the Galaxy. These cool, faint, low mass stars comprise over 75% of all stars. Because of their low luminosities (∼0.0008–0.06 of the Sun’s luminosity), the circumstellar habitable zones (HZs) of dM stars are located within ∼0.05–0.4 AU of the host star. Nevertheless, the prospect of life on a planet located within the...
متن کاملDynamical masses of ultra-compact dwarf galaxies in Fornax
Aims. We determine masses and mass-to-light ratios of five ultra-compact dwarf galaxies and one dwarf elliptical nucleus in the Fornax cluster from high resolution spectroscopy. We examine whether they are consistent with pure stellar populations or whether dark matter is needed to explain their masses. Methods. Velocity dispersions were derived from selected wavelength regions using a direct-f...
متن کاملWhite Dwarf Masses in Magnetic CVs : Multi - temperatureFits to
One method of obtaining the mass of the white dwarf in magnetic CVs is through their hard X-ray spectra. However, previous mass estimates using this method give lower limits because the temperature of the plasma in the post-shock region (where the hard X-rays are emitted) is lower than the temperature of the shock itself. In AM Her systems, the additional cooling of the post-shock plasma by cyc...
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ژورنال
عنوان ژورنال: International Astronomical Union Colloquium
سال: 1983
ISSN: 0252-9211
DOI: 10.1017/s025292110000974x