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A '''flare star''' is a type of [[variable star]] that will suddenly and unpredictably have a massive increase in its brightness across the [[electromagnetic spectrum]] for a few minutes.  These are similar to solar flares but far more energetic and intense in relation to the star's normal output.  For example, [[Luyten 726-8]] emits as much as 75 times its normal brightness during a flare.<ref>http://www.solstation.com/stars/luy726-8.htm#uv-cet</ref>

A '''flare star''' is a type of [[variable star]] that will suddenly and unpredictably have a massive increase in its brightness across the [[electromagnetic spectrum]] for a few minutes.  These are similar to solar flares but far more energetic and intense in relation to the star's normal output.  For example, [[Luyten 726-8]] emits as much as 75 times its normal brightness during a flare.<ref>http://www.solstation.com/stars/luy726-8.htm#uv-cet</ref>

Virtually all known flare stars are M class or late K class [[red dwarf|red dwarfs]], however it is also possible for [[brown dwarf|brown dwarfs]] to also be capable of such flaring.  The frequency of these flares occur anywhere from within and hour to several days apart, but only need a few minutes to reach maximum brightness.  The decay back to normal, quiescent levels of brightness takes several more minutes to hours.

Virtually all known flare stars are M class or late K class [[red dwarf|red dwarfs]], but it is also possible for [[brown dwarf|brown dwarfs]] to also be capable of such flaring.  The frequency of these flares vary from less than an hour to several days, but only need a few minutes to reach maximum brightness.  The decay back to normal, quiescent levels of brightness takes several more minutes to hours.

It is believed the cause of the massive flares are the sudden release of magnetic energy in the photosphere of the star.  A star's magnetic field varies in strength over time.  As solar material and magnetic fields are coupled together, one effect of this coupling is excess energy being transferred to the plasma of the star when the magnetic field drops in strength.  This heats up the solar plasma very quickly which causes it to radiate intensely as a spike in brightness, or a flare.  In addition to increased luminosity, high energy particles are released such as x-rays and gamma rays.<ref name="aavso">http://www.aavso.org/vstar/vsots/fall03.shtml</ref>  

It is believed the cause of the massive flares is the sudden release of magnetic energy in the photosphere of the star.  A star's magnetic field varies in strength over time.  As solar material and magnetic fields are coupled together, one effect of this coupling is excess energy being transferred to the plasma of the star when the magnetic field drops in strength.  This heats up the solar plasma very quickly, which causes it to radiate intensely as a spike in brightness, or a flare.  In addition to increased luminosity, high energy particles are released such as x-rays and gamma rays.<ref name="aavso">http://www.aavso.org/vstar/vsots/fall03.shtml</ref>  

The first known flare stars are '''V1396 Cygni''' and '''AT Microscopii''', discovered as such in 1924.  The most famous flare star is [[Luyten 726-8]], otherwise known by its flare star name ''UV Ceti''.<ref name="aavso">http://www.aavso.org/vstar/vsots/fall03.shtml</ref>  Today most flare stars that fall under the same category are considered UV Ceti type variable stars, and use the UV abbreviation for their variable star name, although sometimes the V abbreviation is used.  

The first known flare stars are '''V1396 Cygni''' and '''AT Microscopii''', discovered as such in 1924.  The most famous flare star is [[Luyten 726-8]], otherwise known by its flare star name ''UV Ceti''.<ref name="aavso">http://www.aavso.org/vstar/vsots/fall03.shtml</ref>  Today most flare stars that fall under the same category are considered UV Ceti type variable stars, and use the UV abbreviation for their variable star name, although sometimes the V abbreviation is used.