LP 944-20
Coordinates: 03h 39m 35.22s, −35° 25′ 44.09″
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Fornax |
Right ascension | 03h 39m 35.220s[1] |
Declination | –35° 25′ 44.09″[1] |
Apparent magnitude (V) | 18.69[2] |
Characteristics | |
Spectral type | M9[1] |
Apparent magnitude (B) | ~20.17[1] |
Apparent magnitude (I) | ~13.288[1] |
Apparent magnitude (J) | ±0.021 10.725[1] |
Apparent magnitude (H) | ±0.021 10.017[1] |
Apparent magnitude (K) | ±0.023 9.548[1] |
Astrometry | |
Proper motion (μ) | RA: ±60 317[1] mas/yr Dec.: ±52 276[1] mas/yr |
Parallax (π) | 155.89 ± 1.03[3][4] mas |
Distance | 20.9 ± 0.1 ly (6.41 ± 0.04 pc) |
Absolute magnitude (MV) | 20.02 |
Details | |
Mass | 0.07[2] M☉ |
Other designations | |
LP 944-20, SIPS J0339−3525, LEHPM 3451, 2MASSI J0339352−352544, [B2006] J033935.2−352544, APMPM J0340−3526, 2MASS J03393521−3525440, 2MASSW J0339352−352544, BRI B0337−3535, BRI 0337−3535, 2MUCD 10201 | |
Database references | |
SIMBAD | data |
LP 944-20 is a dim brown dwarf of spectral class M9 located about 21 light-years from the Solar System in the constellation of Fornax. With a visual apparent magnitude of 18,[2] it has one of the dimmest visual magnitudes listed on the RECONS page.
On 15 December 1999 a flare was detected.[5]
Distance
The first parallax measurement from 1996 found that LP 944-20 (designated there as BRI 0337−3535) has a relative parallax of mas, and its correction from relative to absolute parallax (i.e. mean parallax of the reference frame stars) is mas. This yields an absolute parallax of mas, with a standard deviation (according to [6]) of mas, which corresponds to a distance of ±0.1 5pc, or ±0.3 16.2ly.[7] (The same values of absolute parallax and its standard deviation are in the RECONS' TOP100 list.[2][note 1]
A newer parallax, published in 2013, is ±1.03 mas ( 155.89±0.04 pc or 6.41±0.14 ly). 20.92[3]
Lithium and clouds
Observations published in 2007 showed that the atmosphere of LP 944-20 contains much lithium and that it has dusty clouds.[8]
Notes
- ↑ In RECONS' TOP100 older versions the standard deviation value was 4.20 mas, not 4.21 mas.
References
- 1 2 3 4 5 6 7 8 9 10 "SIPS J0339-3525 -- Brown Dwarf (M<0.08solMass)". Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-14.
- 1 2 3 4 Research Consortium on Nearby Stars, Georgia State University (January 1, 2012). "The 100 nearest star systems". RECONS. Retrieved 2012-06-11. External link in
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(help) - 1 2 Dieterich, Sergio B.; Todd J. Henry; Wei-Chun Jao; Jennifer G. Winters; Altonio D. Hosey (2013). "The Solar Neighborhood XXXII: The Hydrogen Burning Limit". arXiv:1312.1736v1.
- ↑ Lurie, John C.; Henry, Todd J.; Jao, Wei-Chun; Quinn, Samuel N.; Winters, Jennifer G.; Ianna, Philip A.; Koerner, David W.; Riedel, Adric R.; Subasavage, John P. (2014). "The Solar Neighborhood. XXXIV. a Search for Planets Orbiting Nearby M Dwarfs Using Astrometry". The Astronomical Journal. 148 (5): 91. arXiv:1407.4820. Bibcode:2014AJ....148...91L. doi:10.1088/0004-6256/148/5/91.
- ↑ http://www.solstation.com/stars/lp944-20.jpg
- ↑ Mean and Variance of Random Variables
- ↑ Tinney, C. G. (1996). "CCD astrometry of southern very low-mass stars". Monthly Notices of the Royal Astronomical Society. 281 (2): 644–658. Bibcode:1996MNRAS.281..644T. doi:10.1093/mnras/281.2.644.
- ↑ Pavlenko, Ya. V.; et al. (September 2007). "Lithium in LP944-20". Monthly Notices of the Royal Astronomical Society. 380 (3): 1285–1296. arXiv:0707.0694. Bibcode:2007MNRAS.380.1285P. doi:10.1111/j.1365-2966.2007.12182.x.