DX Cancri

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search

Coordinates: Sky map 08h 29m 49.345s, +26° 46′ 33.74″

DX Cancri
An ultraviolet band light curve for a flare on DX Cancri, adapted from Pettersen (1981)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Cancer
Right ascension 08h 29m 49.345s[2]
Declination +26° 46′ 33.74″[2]
Apparent magnitude (V) 14.81[3]
Spectral type M6.5V[4]
Apparent magnitude (J) 8.2[3]
U−B color index +2.11[5]
B−V color index +2.08[5]
Variable type Flare star[3]
Radial velocity (Rv)+9.0[6] km/s
Proper motion (μ) RA: –1140[2] mas/yr
Dec.: –602[2] mas/yr
Parallax (π)279.2496 ± 0.0637[7] mas
Distance11.680 ± 0.003 ly
(3.5810 ± 0.0008 pc)
Absolute magnitude (MV)16.98[8]
Mass0.09[8] M
Radius0.11[9] R
Luminosity0.00065[10] L
Temperature2,840[11] K
Rotation0.46 days[9]
Rotational velocity (v sin i)11.0[12] km/s
Age200[13] Myr
Other designations
G 051-015, GCTP 2016.01, GJ 1111, LHS 248.[3]
Database references
DX Cancri is located in the constellation Cancer.
DX Cancri is located in the constellation Cancer.
DX Cancri
Location of DX Cancri in the constellation Cancer

DX Cancri is a variable star in the northern zodiac constellation of Cancer. With an apparent visual magnitude of 14.81,[3] it is much too faint to be seen with the naked eye. Visually viewing this star requires a telescope with a minimum aperture of 16 in (41 cm).[14] Based upon parallax measurements, DX Cancri is located at a distance of 11.8 light-years (3.6 parsecs) from Earth. This makes it the 18th closest star (or star system) to the Sun.

The star has a stellar classification of M6.5V,[4] identifying it as a type of main sequence star known as a red dwarf. It has about 9% of the mass of the Sun,[8] and 11% of the Sun's radius.[9] The outer envelope of the star has an effective temperature of 2,840 K,[11] making it an M-type star. It is a flare star that has random, intermittent increases in brightness by up to a factor of five. It is a proposed member of the Castor Moving Group of stars that share a common trajectory through space. This group has an estimated age of 200 million years.[15]

See also[edit]


  1. ^ Pettersen, B. R. (February 1981). "Discovery of flare activity on the very low luminosity red dwarf G 51-15". Astronomy & Astrophysics. 95: 135–137. Retrieved 11 November 2021.
  2. ^ a b c d Zacharias, N.; et al. (2003). "The Second U.S. Naval Observatory CCD Astrograph Catalog (UCAC2)". VizieR Online Data Catalog. CDS/ADC Collection of Electronic Catalogues, 1289, 0 (2003). Bibcode:2003yCat.1289....0Z. Retrieved 2010-06-29.
  3. ^ a b c d e "V* DX Cnc -- Flare Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-06-29.
  4. ^ a b Luhman, Kevin L.; Allers, Katelyn N.; Jaffe, Daniel T.; Cushing, Michael C.; Williams, Kurtis A.; Slesnick, Catherine L.; Vacca, William D. (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, S2CID 11153196
  5. ^ 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.
  6. ^ Montes, D.; et al. (November 2001). "Late-type members of young stellar kinematic groups - I. Single stars" (PDF). 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. S2CID 55727428.
  7. ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. Gaia EDR3 record for this source at VizieR.
  8. ^ a b c "The One Hundred Nearest Star Systems". RECONS. Georgia State University. January 1, 2009. Retrieved 2010-06-29.
  9. ^ a b c Morin, J.; et al. (October 2010), "Large-scale magnetic topologies of late M dwarfs", Monthly Notices of the Royal Astronomical Society, 407 (4): 2269–2286, arXiv:1005.5552, Bibcode:2010MNRAS.407.2269M, doi:10.1111/j.1365-2966.2010.17101.x, S2CID 119192200
  10. ^ Vidotto, A. A.; et al. (July 2013). "Effects of M dwarf magnetic fields on potentially habitable planets". Astronomy & Astrophysics. 557: A67. arXiv:1306.4789. Bibcode:2013A&A...557A..67V. doi:10.1051/0004-6361/201321504. S2CID 44335981.
  11. ^ a b Reiners, Ansgar; Basri, Gibor (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. S2CID 17743657.
  12. ^ Jenkins, J. S.; et al. (October 2009). "Rotational Velocities for M Dwarfs". The Astrophysical Journal. 704 (2): 975–988. arXiv:0908.4092. Bibcode:2009ApJ...704..975J. doi:10.1088/0004-637X/704/2/975. S2CID 119203469.
  13. ^ Lestrade, J.-F.; et al. (November 2009), "Search for cold debris disks around M-dwarfs. II", Astronomy and Astrophysics, 506 (3): 1455–1467, arXiv:0907.4782, Bibcode:2009A&A...506.1455L, doi:10.1051/0004-6361/200912306, S2CID 17035185
  14. ^ Sherrod, P. Clay; Koed, Thomas L. (2003), A Complete Manual of Amateur Astronomy: Tools and Techniques for Astronomical Observations, Astronomy Series, Courier Dover Publications, p. 9, ISBN 0486428206
  15. ^ Lestrade, J.-F.; et al. (December 2006), "Search for cold debris disks around M-dwarfs", Astronomy and Astrophysics, 460 (3): 733–741, arXiv:astro-ph/0609574, Bibcode:2006A&A...460..733L, doi:10.1051/0004-6361:20065873, S2CID 119328045

Further reading[edit]

External links[edit]