Gliese 229
Gliese 229 (also written as Gl 229 or GJ 229) is a red dwarf star about 19 light years away in the constellation Lepus. It has 58% of the mass of the Sun,[4] 69% of the Sun's radius,[5] and a very low projected rotation velocity of 1 km/s at the stellar equator.[7]
The star is known to be a low activity flare star, which means it undergoes random increases in luminosity because of magnetic activity at the surface. The spectrum shows emission lines of calcium in the H and K bands. The emission of X-rays has been detected from the corona of this star.[8] These may be caused by magnetic loops interacting with the gas of the star's outer atmosphere. No large-scale star spot activity has been detected.[2]
In 1994 a substellar companion was imaged and it was confirmed in 1995. Gliese 229B is a brown dwarf orbiting the star; although it is too small to sustain hydrogen-burning nuclear fusion, with a mass of 20 to 50 times that of Jupiter (0.02 to 0.05 solar masses) it is still too massive to be a planet. Gliese 229B was the first confirmed substellar-mass object. This object has a surface temperature of 950 K.[9]
The space velocity components of this star are U = +12, V = –11 and W = –12 km/s.[10] The orbit of this star through the Milky Way galaxy has an eccentricity of 0.07 and an orbital inclination of 0.005.[2]
References
- ^ a b c d e Perryman, M. A. C. et al (1997). "The Hipparcos Catalogue". Astronomy and Astrophysics 323: L49–L52. Bibcode 1997A&A...323L..49P.
- ^ a b c d e Byrne, P. B.; Doyle, J. G.; Menzies, J. W. (May 1, 1985). "Optical photometry and spectroscopy of the flare star Gliese 229 (=HD42581)". Monthly Notices of the Royal Astronomical Society 214: 119–130. Bibcode 1985MNRAS.214..119B.
- ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick. Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. http://adsabs.harvard.edu/abs/1967IAUS...30...57E. Retrieved 2009-10-19.
- ^ a b Zechmeister, M.; Kürster, M.; Endl, M. (October 2009). "The M dwarf planet search programme at the ESO VLT + UVES. A search for terrestrial planets in the habitable zone of M dwarfs". Astronomy and Astrophysics 505 (2): 859–871. Bibcode 2009A&A...505..859Z. doi:10.1051/0004-6361/200912479.
- ^ a b White, Stephen M.; Jackson, Peter D.; Kundu, Mukul R. (December 1989). "A VLA survey of nearby flare stars". Astrophysical Journal Supplement Series 71: 895–904. Bibcode 1989ApJS...71..895W. doi:10.1086/191401.
- ^ Morales, J. C.; Ribas, I.; Jordi, C. (February 2008). "The effect of activity on stellar temperatures and radii". Astronomy and Astrophysics 478 (2): 507–512. Bibcode 2008A&A...478..507M. doi:10.1051/0004-6361:20078324. Data from CDS table J/A+A/478/507.
- ^ a b Reiners, A. (May 2007). "The narrowest M-dwarf line profiles and the rotation-activity connection at very slow rotation". Astronomy and Astrophysics 467 (1): 259–268. arXiv:astro-ph/0702634. Bibcode 2007A&A...467..259R. doi:10.1051/0004-6361:20066991.
- ^ Schmitt JHMM, Fleming TA, Giampapa MS (September 1995). "The X-Ray View of the Low-Mass Stars in the Solar Neighborhood". Ap J. 450 (9): 392–400. Bibcode 1995ApJ...450..392S. doi:10.1086/176149.
- ^ Geißler, K.; Chauvin, G.; Sterzik, M. F. (March 2008). "Mid-infrared imaging of brown dwarfs in binary systems". Astronomy and Astrophysics 480 (1): 193–198. Bibcode 2008A&A...480..193G. doi:10.1051/0004-6361:20078229.
- ^ Gliese, W. (1969). "Catalogue of Nearby Stars". Veröffentlichungen des Astronomischen Rechen-Instituts Heidelberg. Bibcode 1969VeARI..22....1G.
External links
← Star systems within 15–20 light-years →
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Altair ( 16.69 ± 0.04 ly; 1 star)
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In left column are stellar classes of primary members of star systems. ‡Distance error margin extends out of declared distance interval. Bold are systems containing at least one component with absolute magnitude of +8.5 or brighter. Italic are systems possibly located within declared distance interval, but probably not.
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