Mu Pegasi

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Mu Pegasi
Diagram showing star positions and boundaries of the Pegasus constellation and its surroundings
Cercle rouge 100%.svg

Location of μ Pegasi (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pegasus
Right ascension 22h 50m 00.19315s[1]
Declination +24° 36′ 05.6984″[1]
Apparent magnitude (V) 3.514[2]
Characteristics
Spectral type G8 III[3]
U−B color index +0.674[2]
B−V color index +0.932[2]
Astrometry
Radial velocity (Rv) +13.54 ± 0.20[4] km/s
Proper motion (μ) RA: +144.70[1] mas/yr
Dec.: –41.87[1] mas/yr
Parallax (π) 30.74 ± 0.27[1] mas
Distance 106.1 ± 0.9 ly
(32.5 ± 0.3 pc)
Absolute magnitude (MV) 0.432[5]
Details
Mass 1.3[6] M
Radius 9.6 ± 0.4[7] R
Surface gravity (log g) 2.50[3] cgs
Temperature 4,950[3] K
Metallicity [Fe/H] –0.03[3] dex
Rotational velocity (v sin i) 4.0[8] km/s
Other designations
μ Peg, 48 Peg, BD+23 4615, FK5 862, GJ 4298, HD 216131, HIP 112748, HR 8684, SAO 90816.[9]

Mu Pegasi (μ Peg, μ Pegasi) is a star in the northern constellation of Pegasus. It has the traditional name Sadalbari, which derives from the Arabic term for "luck star of the splendid one".[10] The apparent visual magnitude of this star is 3.5,[2] which is bright enough to be seen with the naked eye even on a moonlit night. The distance to this star can be determined with parallax measurements, which yields a value of 106.1 light-years (32.5 parsecs).[1]

The spectrum of this star matches a stellar classification of G8 III.[3] The luminosity class of 'III' means that it has exhausted the hydrogen fuel at its core and evolved into a giant star. It is slightly more massive than the Sun, but has expanded to nearly ten times the Sun's radius.[7] (Mishenina et al. (2006) list it with an estimated 2.7 times the mass of the Sun.[5]) The effective temperature of the outer atmosphere is about 4,950 K,[3] which is cooler than the Sun and gives it the yellow hue of a G-type star.[11][12] The abundance of elements other than hydrogen and helium, what astronomers term the metallicity, is similar to the abundance in the Sun.[3]

References

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