Sub-brown dwarfs or brown sub - dwarfs are cold formations, by weight lying below the limit of brown dwarfs . They are generally considered to be planets . Their mass is less than 0.012 [1] [2] the mass of the Sun or, accordingly, 12.57 of the mass of Jupiter, the lower limit is not defined. At the same time, the pattern of formation of sub-brown dwarfs is similar to the pattern of star formation. They are born by the collapse of a gas cloud, and not by the accretion or collapse of the core from the material of the circumstellar disk, like planets. The scientific community has not yet come to a final conclusion about what is considered a planet and what is a sub-brown dwarf. At the moment, astronomers are divided into two camps that decide the question of whether to consider the process of planet formation as a criterion for classification.
Possible Brown Sub-Dwarfs
- COROT-Exo-3 b
- 2M1207 b
- SCR 1845-6357 B
- Cha 110913-773444
- UGPS J072227.51-054031.2
- WISE 0855-0714
See also
- Planetar
- Planemo
- Gas planets
Notes
- ↑ David S. Spiegel; Adam Burrows & John A. Milsom (2010), "The Deuterium-Burning Mass Limit for Brown Dwarfs and Giant Planets", arΧiv : 1008.5150v2 [astro-ph] (English) - See S. 2, 6.
- ↑ G. Chabrier; I. Baraffe; F. Allard & PH Hauschildt (2005), "Review on low-mass stars and brown dwarfs", arΧiv : astro-ph / 0509798v1 [astro-ph] (Eng.) - See S. 16. - Quote: [...] The distinction between BD and giant planets has become these days a topic of intense debate. In 2003, the IAU has adopted the deuterium-burning minimum mass, m DBMM ≃ 0.012M ⊙ (Saumon et al. 1996, Chabrier et al. 2000b) as the official distinction between the two types of objects. [...] Translation: [ ...] The distinction between brown dwarfs and giant planets has now become a topic of intense debate. In 2003, the MAS accepted the minimum mass necessary for combustion of the deuterium m DBMM ≃ 0.012M ⊙ (Saumon et al. 1996, Chabrier et al. 2000b) as the official value for distinguishing between the two types of objects. [...]