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Brown dwarfs are substellar objects that have more mass than the biggest gas giant planets, but less than the least massive main-sequence stars.Their mass is approximately 13 to 80 times that of Jupiter (M J) [2] [3] —not big enough to sustain nuclear fusion of ordinary hydrogen (1 H) into helium in their cores, but massive enough to emit some light and heat from the fusion of deuterium (2 H).
The first brown dwarf discovered orbiting a star was Gliese 229 B, also discovered in 1995. [3] The first brown dwarf found to have a planet was 2M1207, discovered in 2004. [4] As of 2015, more than 2,800 brown dwarfs have been identified. [5] An isolated object with less than about 13 Jupiter masses is technically a sub-brown dwarf or rogue ...
Nemesis is a hypothetical red dwarf [1] or brown dwarf, [2] originally postulated in 1984 [3] to be orbiting the Sun at a distance of about 95,000 AU (1.5 light-years), [2] somewhat beyond the Oort cloud, to explain a perceived cycle of mass extinctions in the geological record, which seem to occur more often at intervals of 26 million years.
In 1995, astronomers confirmed the discovery for the first time of a brown dwarf, a body too small to be a star and too big to be a planet - sort of a celestial tweener. Researchers now have taken ...
Brown dwarf: Smallest known brown dwarf. [53] EPIC 201702477 54,120 [54] BE Ursae Majoris A 54,250 O-type subdwarf [55] LP 40-365: 54,250 White dwarf: A white dwarf that might have formed in a type Iax supernova. Range of values of 40,350 to 82,095 km [56] Epsilon Indi Ba 55,656 Brown dwarf [57] LHS 6343 C 55,978 [58] Epsilon Indi Bb 57,050 [57 ...
CWISEP J1935-1546 was discovered in 2019 by Marocco et al. as an extremely cold brown dwarf with a temperature range of 270-360 K and a distance of 5.6-10.9 parsec. It was discovered with the help of the python package XGBoost, using machine-learning algorithms and the CatWISE catalog, as well as the WiseView tool. [6]
Spectral type L is usually a type of brown dwarfs. Also, very young gas giants that are still cooling from the accretion process may have an L-type spectrum. Moreover, some hydrogen-fusing stars also fall into the L-type.
Sub-brown dwarf; Ultra-cool dwarf; 0–9. 2MASS J11011926−7732383; 2MASS J00361617+1821104; 2MASS 1237+6526; 2MASS 1507−1627; 2MASS J02431371−2453298; 2MASS ...