Gamma Pegasi is a star in the constellation of Pegasus, located at the southeast corner of the asterism known as the Great Square. It has the formal name Algenib /ælˈdʒiːnɪb/;^[14][15] the Bayer designation Gamma Pegasi is Latinized from γ Pegasi and abbreviated Gamma Peg or γ Peg. The average apparent visual magnitude of +2.84^[4] makes this the fourth-brightest star in the constellation. The distance to this star has been measured using the parallax technique, yielding a value of roughly 470 light-years (144 parsecs).

Quick Facts Observation data Epoch J2000 Equinox J2000, Constellation ...

Gamma Pegasi

Location of γ Pegasi (circled)
Observation data Epoch J2000      Equinox J2000
Constellation	Pegasus
Right ascension	00h 13m 14.15123s[1]
Declination	+15° 11′ 00.9368″[1]
Apparent magnitude (V)	+2.78 to 2.89[2]
Characteristics
Spectral type	B2 IV[3]
U−B color index	−0.85[4]
B−V color index	−0.23[4]
Variable type	β Cep[5]
Astrometry
Radial velocity (Rv)	+4.1[6] km/s
Proper motion (μ)	RA: +1.98 mas/yr[1] Dec.: –9.28 mas/yr[1]
Parallax (π)	6.9474 ± 0.4293 mas[7]
Distance	470 ± 30 ly (144 ± 9 pc)
Absolute magnitude (MV)	−2.64[8]
Details
Mass	8.9±0.1[3] M☉
Radius	4.80±0.39[9] R☉
Luminosity	5,840[10] L☉
Surface gravity (log g)	3.98±0.06[9] cgs
Temperature	21,179±237[9] K
Metallicity [Fe/H]	−0.34[11] dex
Rotational velocity (v sin i)	0[12] km/s
Age	18.7±3.2[3] Myr
Other designations
Algenib, gam Peg, 88 Peg, FK5 7, HD 886, HIP 1067, HR 39, SAO 91781[13]
Database references
SIMBAD	data

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Gamma Pegasi is the star's Bayer designation. Although it also had the traditional name Algenib, this name was also used for Alpha Persei. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)^[16] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016^[17] included a table of the first two batches of names approved by the WGSN; which included Algenib for this star (Alpha Persei was given the name Mirfak).

The asterism of γ Pegasi and α Andromedae, in Hindu astronomy, is called Uttara Bhādrapadā (उत्तरभाद्रपदा) or Uttṛṭṭāti. It is the 26th nakshatra. In Chinese, 壁宿 (Bìxiù), meaning Wall (asterism) refers to an asterism consisting of γ Pegasi and α Andromedae .^[18] Consequently, the Chinese name for γ Pegasi itself is 壁宿一 (Bìxiù yī, English: the First Star of Wall.)^[19]

In 1911, American astronomer Keivin Burns discovered that the radial velocity of Gamma Pegasi varied slightly. This was confirmed in 1953 by American astronomer D. Harold McNamara, who identified it as a Beta Cephei variable.^[5] (At the time he actually identified it as a Beta Canis Majoris star, which was subsequently designated a Beta Cephei variable.)^[21] It has a radial pulsation period of 0.15175 days (3.642 hours), but also shows the behavior of a slowly pulsating B star (SPB) with three additional pulsational frequencies.^[5] Hence it is considered a hybrid pulsator.^[22] Its magnitude varies between +2.78 and +2.89 over the course of each pulsation cycle.^[2]

This is a large star with almost nine^[3] times the mass of the Sun and close to five^[9] times the Sun's radius. The stellar classification of B2 IV^[3] suggests this is a subgiant star that is exhausting the hydrogen at its core and is in the process of evolving away from the main sequence. It is either rotating very slowly with no measurable rotational velocity or else it is being viewed from nearly pole-on.^[12] Gamma Pegasi has a total luminosity of 5,840 times that of the Sun,^[10] which is being radiated from its outer atmosphere at an effective temperature of more than 21,000 K.^[9] At this temperature, the star glows with a blue-white hue.^[23]

The star has a weak magnetic field (from -10 G to 30 G,^[24] an upper bound on a dipolar magnetic field strength of about 40 G^[25]).