Portal:Astronomy/Featured/May 2008
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IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. A distance of about 150 light years from the Solar System, it is just luminous enough to be seen with the unaided eye.
The primary (IK Pegasi A) is a main sequence, A-class star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day.[1] Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.
IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses, it may explode as a Type Ia supernova.[2]
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