DX Cancri
DX Cancri is a red dwarf star that is about 9% of the mass of our Sun.[7] It is a flare star that has intermittent changes in brightness by up to a fivefold increase.
DX Cancri is far too faint to be seen with the naked eye, even though it is the 18th closest star system to the Sun at a distance of 11.8 light years. It is the closest star in the constellation Cancer.
See also
References
- ^ a b c d Zacharias, N.; et al. (2003). The Second U.S. Naval Observatory CCD Astrograph Catalog (UCAC2). CDS/ADC Collection of Electronic Catalogues, 1289, 0 (2003). http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2003yCat.1289....0Z&db_key=AST&nosetcookie=1. Retrieved 2010-06-29.
- ^ a b c "V* DX Cnc -- Flare Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=DX+Cancri. Retrieved 2010-06-29.
- ^ Luhman, K. L.; et al. (April 2007). "Ophiuchus 1622-2405: Not a Planetary-Mass Binary". The Astrophysical Journal 659 (2): 1629–1636. arXiv:astro-ph/0701242. Bibcode 2007ApJ...659.1629L. doi:10.1086/512539.
- ^ a b Weistrop, D. (August 1981). "The nature of the Giclas +4 stars". Astronomical Journal 86: 1220–1227. Bibcode 1981AJ.....86.1220W. doi:10.1086/113001.
- ^ Montes, D.; et al. (November 2001). "Late-type members of young stellar kinematic groups - I. Single stars". Monthly Notices of the Royal Astronomical Society 328 (1): 45–63. arXiv:astro-ph/0106537. Bibcode 2001MNRAS.328...45M. doi:10.1046/j.1365-8711.2001.04781.x.
- ^ van Altena, W. F.; Lee, J. T.; Hoffleit, E. D. (1995). The general catalogue of trigonometric [stellar] parallaxes (4th ed.). New Haven, CT: Yale University Observatory. http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?1995GCTP..C......0V. Retrieved 2010-06-29.
- ^ a b c "The One Hundred Nearest Star Systems". RECONS. Georgia State University. January 1, 2009. http://www.chara.gsu.edu/~thenry/RECONS/TOP100.posted.htm. Retrieved 2010-06-29.
- ^ Reiners, A.; Basri, G. (February 2007). "The First Direct Measurements of Surface Magnetic Fields on Very Low Mass Stars". The Astrophysical Journal 656 (2): 1121–1135. arXiv:astro-ph/0610365. Bibcode 2007ApJ...656.1121R. doi:10.1086/510304.
- ^ Jenkins, J. S.; et al. (October 2009). "Rotational Velocities for M Dwarfs". The Astrophysical Journal 704 (2): 975–988. Bibcode 2009ApJ...704..975J. doi:10.1088/0004-637X/704/2/975.
External links
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← Star systems within 10–15 light-years →
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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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