A flare star is a variable star that becomes very much brighter unpredictably for a few minutes at a time.
The first known flare stars were discovered in 1924, they were V1396 Cygni and AT Microscopii. Still the best-known flare star is UV Ceti, that star was discovered in 1948. Today similar flare stars are classified as UV Ceti type variable stars in variable star catalogs. Flares can happen once every few days or, as in the case of Barnard's Star, much less frequently. Proxima Centauri, the nearest star to the Solar System, is also a flare star.
Most flare stars are dim red dwarfs, although research done not too long ago suggests that less massive (lighter) brown dwarfs might also be able to flare. The more massive (heavier) RS Canum Venaticorum variables (RS CVn) are also known to flare, but scientists understand that a companion star in a binary system causes these flares. This companion star disturbs the magnetic field. Nine stars similar to the Sun have also been seen to flare. There is a suggestion that this happens for similar reasons to the flares of the RS CVn variables. A companion causes the flares, this companion is a massive planet like the planet Jupiter that orbits the flaring star closely.
Nearby flare stars[change | edit source]
Proxima Centauri[change | edit source]
Proxima Centauri is closer to the sun than any other star and is a flare star. Proxima Centauri increases its brightness randomly and magnetic force causes this. Convection creates a magnetic field throughout the matter in Proxima Centauri, and this leads to flaring with a total X-ray output similar to that of the Sun though the sun is much more massive (heavier) than Proxima Centauri.
Wolf 359[change | edit source]
The flare star Wolf 359 is another star relatively near the Solar System in the constellation of Leo and has other names (designations) as well. It is a red dwarf of spectral class M6.5 and emits X-rays. It is a UV Ceti flare star, and flares relatively often.
The mean (average) magnetic field varies significantly during periods of time as short as six hours. By comparison, the magnetic field of the Sun averages 1 G (100 µT), although it can rise as high as 3 kG (0.3 T) in active sunspot regions.
Barnard's Star[change | edit source]
TVLM513-46546[change | edit source]
TVLM513-46546 is the name (or designation) scientists give to flare star with very low mass. This small star is only just heavy enough to count as a red dwarf.
References[change | edit source]
- Schaefer, Bradley; King, Jeremy R.; Deliyannis, Constantine P. (2000-02). "Superflares on Ordinary Solar-Type Stars". The Astrophysical Journal (Astrophysical Journal) 529 (2): 1026. doi:10.1086/308325.
- Rubenstein, Eric; Schaefer, Bradley E. (2000-02). "Are Superflares on Solar Analogues Caused by Extrasolar Planets?". The Astrophysical Journal (Astrophysical Journal) 529 (2): 1031. doi:10.1086/308326.
- Kulkarni SR, Rau A (2006). "The Nature of the Deep Lens Survey Fast Transients". Ap J. 644 (1): L63. doi:10.1086/505423.
- Christian DJ, Mathioudakis M, Bloomfield DS, Dupuis J, Keenan FP (2004). "A Detailed Study of Opacity in the Upper Atmosphere of Proxima Centauri". Ap J. 612 (2): 1140–6. doi:10.1086/422803.
- Wood BE, Linsky JL, Müller HR, Zank GP (2001). "Observational Estimates for the Mass-Loss Rates of α Centauri and Proxima Centauri Using Hubble Space Telescope Lyα Spectra". Ap J. 547 (1): L49–L52. doi:10.1086/318888.
- Schmitt JHMM, Fleming TA, Giampapa MS (Sep 1995). "The X-Ray View of the Low-Mass Stars in the Solar Neighborhood". Ap J. 450 (9): 392–400. doi:10.1086/176149.
- Gershberg RE, Shakhovskaia NI (1983). "Characteristics of activity energetics of he UV Cet-type flare stars". Astrophys Space Sci. 95 (2): 235–53. doi:10.1007/BF00653631.
- Reiners A, Schmitt JHMM, Liefke C (2007). "Rapid magnetic flux variability on the flare star CN Leonis". Astronomy and Astrophysics 466 (2): L13–6. doi:10.1051/0004-6361:20077095.
- Staff (January 7, 2007). "Calling Dr. Frankenstein! : Interactive Binaries Show Signs of Induced Hyperactivity". National Optical Astronomy Observatory. http://www.noao.edu/outreach/press/pr07/pr0701.html. Retrieved 2006-05-24.