Mu Cephei - Wikipedia. Mu Cephei. Observation data.
Epoch. J2. 00. 0. Equinox. J2. 00. 0. Constellation. Cepheus. Right ascension. 21h 4. Absolute magnitude (MV). It appears garnet red and is located at the edge of the IC 1. Since 1. 94. 3, the spectrum of this star has served as the M2 Ia standard by which other stars are classified.
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Summing radiation at all wavelengths gives a luminosity of around 2. L. It is also one of the largest stars so far discovered. History. This variability was quickly confirmed by German astronomer Friedrich Wilhelm Argelander.
Almost continual records of the star's variability have been maintained since 1. It is now considered to be a semiregular variable of type SRc. Its apparent brightness varies erratically between magnitude 3. Many different periods have been reported, but they are consistently near 8. It is best seen from the northern hemisphere from August to January. This is a runaway star with a peculiar velocity of 8. The Hipparcos satellite was used to measure a parallax of 0.
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However, this value is close to the margin of error. A determination of the distance based upon a size comparison with Betelgeuse gives an estimate of 3. It may be surrounded by a shell extending out to a distance at least equal to 0. This outer shell appears to contain molecular gases such as CO, H2.
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O, and Si. O. This indicates an age of about 2,0. Closer to the star, this material shows a pronounced asymmetry, which may be shaped as a torus. The star currently has a mass loss rate of a few times 1. It has begun to fusehelium into carbon, whereas a main sequence star fuses hydrogen into helium. When a supergiant star has converted elements in its core to iron, the core collapses to produce a supernova and the star is destroyed, leaving behind a vast gaseous cloud and a small, dense remnant. For a star as massive as Mu Cephei the remnant is likely to be a black hole.
The most massive red supergiants will evolve back to blue supergiants, Luminous blue variables, or Wolf- Rayet stars before their cores collapse, and Mu Cephei appears to be massive enough for this to happen. A post- red supergiant will produce a type IIn or type II- b supernova, while a Wolf Rayet star will produce a type Ib or Ic supernova.
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Jim Kaler: Stars. Retrieved 1. 5 December 2.
AAVSO: Variable Star of the Season Archive. Retrieved 1. 5 December 2. Matt Ben Daniel: Starmatt Astrophotography.
Retrieved 1. 5 December 2. Jumk. de Webprojects: Big and Giant Stars. Retrieved 1. 5 December 2.