Location of S Persei (circled) near the Double Cluster (north is left) | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Perseus |
Right ascension | 2h 22m 51.70928s [1] |
Declination | 58° 31′ 11.4476″ [1] |
Apparent magnitude (V) | +9.23 [2] (7.9 - 12.0 [3] ) |
Characteristics | |
Spectral type | M3 Iae–M7 [3] |
B−V color index | +2.65 [2] |
Variable type | SRc [3] |
Astrometry | |
Radial velocity (Rv) | -39.71 [4] km/s |
Proper motion (μ) | RA: –0.49 ± 0.23 [5] mas/yr Dec.: −1.19 ± 0.20 [5] mas/yr |
Parallax (π) | 0.413 ± 0.017 mas [5] |
Distance | 7,900 ± 300 ly (2,420 ± 100 pc) |
Absolute magnitude (MV) | –6.36 (at mV 9.23) [2] |
Details | |
Mass | 20 [6] M☉ |
Radius | 1,212 [7] – 1,364 [8] R☉ |
Luminosity | 123,000 [9] – 186,000 [10] L☉ |
Surface gravity (log g) | 0.0 [11] cgs |
Temperature | 3,500 [12] (3,000 [13] – 3,600 [10] ) K |
Other designations | |
Database references | |
SIMBAD | data |
S Persei is a red supergiant or hypergiant located near the Double Cluster in Perseus, north of the cluster NGC 869. It is a member of the Perseus OB1 association and one of the largest known stars. If placed in the Solar System, its photosphere would engulf the orbit of Jupiter. It is also a semiregular variable, a star whose variations are less regular than those of Mira variables.
S Persei was named by German astronomer Adalbert Krueger in 1874 after observing that it varied in brightness. [14] It was subsequently listed in major stellar catalogues of that era as HD 14528 and BD+57°552.
S Persei varies slowly by several magnitudes, a factor of over 40 in brightness. It has a main period of somewhat over two years, but shows significant unpredictability. There is a strong variation in the amplitude from around one magnitude to about four magnitudes, and these have been interpreted as beats due to a second period of about 940 days. [16] Other analyses find only the primary period of 813 ± 60 days. [17]
S Persei is classified as a semiregular variable star of type SRc, indicating that it is a supergiant, and it has one of the largest visual amplitudes of any variable of this type. [3] While the General Catalogue of Variable Stars lists it as varying between magnitudes 7.9 and 12.0, it has since been seen fainter. [17]
The spectral type of S Persei also varies. Typically it is a red supergiant of spectral class M3 or M4, but particularly at deep visual minima it may show a much cooler spectral type of M7 or M8, highly unusual for a supergiant. [18]
Many of the visually bright variable stars belong to this class of semiregulars, as these stars are extremely large and luminous, and hence visible across long distances. S Persei has been described as a hypergiant [19] and has a radius over 700 times the sun's radius (R☉). [2] Its angular diameter has been measured directly and found to be somewhat elliptical. Modelled as a uniform disk, the radius corresponds to 1,212 ± 124 R☉. [7]
The temperature has been calculated from the spectrum using a DUSTY model, [20] giving an effective photospheric temperature of 3,500 K and a temperature of 1,000 K for the surrounding dust torus. [12] This is consistent with previous studies, but the derived luminosity from different authors varies from 86,000 L☉ to 186,000 L☉. [10] [21] [22] Older studies frequently calculated higher luminosities, lower temperatures, and consequently larger values for the radius. [23]
The mass of S Persei is also uncertain, but expected to be around 20 M☉. [6] Mass is being lost at 2.4 to 2.6×10−5 M☉ per year, [12] leading to an extensive and complex circumstellar environment of gas and dust. [10]
S Persei is surrounded by clouds containing water molecules which produce maser emission. This allows the distance to be measured very accurately using very long baseline interferometry, giving an annual parallax of 0.413 ± 0.017 milliarcseconds. For comparison the Gaia Data Release 2 parallax is 0.2217±0.1214 mas . [24] It lies somewhat further away than the centres of the Double Cluster open clusters, but definitely within the Per OB1 association and the Perseus Arm of the galaxy. [5]
S Persei is a double star. The red supergiant has an A0 11th magnitude companion at 69". [25] There are also several other 8th to 10th magnitude stars within half a degree of S Persei. [26]
Red supergiants (RSGs) are stars with a supergiant luminosity class of spectral type K or M. They are the largest stars in the universe in terms of volume, although they are not the most massive or luminous. Betelgeuse and Antares are the brightest and best known red supergiants (RSGs), indeed the only first magnitude red supergiant stars.
Zeta Persei is a star in the northern constellation of Perseus. With an apparent visual magnitude of 2.9, it can be readily seen with the naked eye. Parallax measurements place it at a distance of about 750 light-years from Earth.
A yellow hypergiant (YHG) is a massive star with an extended atmosphere, a spectral class from A to K, and, starting with an initial mass of about 20–60 solar masses, has lost as much as half that mass. They are amongst the most visually luminous stars, with absolute magnitude (MV) around −9, but also one of the rarest, with just 20 known in the Milky Way and six of those in just a single cluster. They are sometimes referred to as cool hypergiants in comparison with O- and B-type stars, and sometimes as warm hypergiants in comparison with red supergiants.
V354 Cephei is a red supergiant star located within the Milky Way. It is an irregular variable located over 8,900 light-years away from the Sun. It has an estimated radius of 685 solar radii. If it were placed in the center of the Solar System, it would extend to between the orbits of Mars and Jupiter.
Westerlund 1 is a compact young super star cluster about 3.8 kpc away from Earth. It is thought to be the most massive young star cluster in the Milky Way, and was discovered by Bengt Westerlund in 1961 but remained largely unstudied for many years due to high interstellar absorption in its direction. In the future, it will probably evolve into a globular cluster.
MY Cephei is a red supergiant located in open cluster NGC 7419 in the constellation of Cepheus. It is a semiregular variable star with a maximum brightness of magnitude 14.4 and a minimum of magnitude 15.5.
6 Cassiopeiae is a white hypergiant in the constellation Cassiopeia, and a small-amplitude variable star.
VX Sagittarii is an extreme asymptotic giant branch star located more than 1.5 kiloparsec away from the Sun in the constellation of Sagittarius. It is a pulsating variable star with an unusually large magnitude range. It is also one of the largest stars discovered so far, with a radius varying between 1,350 and 1,940 solar radii (940,000,000 and 1.35×109 km; 6.3 and 9.0 au). It is the most luminous known AGB star, at bolometric magnitude –8.6, which is even brighter than the theoretical limit at –8.0.
V4381 Sagittarii is a variable star in the constellation Sagittarius. A white supergiant of spectral type A2/A3Iab, it is an Alpha Cygni variable that varies between apparent photographic magnitudes 6.57 and 6.62. Its visual apparent magnitude is about 6.54.
HD 33579 is a white/yellow hypergiant and one of the brightest stars in the Large Magellanic Cloud (LMC). It is a suspected variable star.
IRC+10420, also known as V1302 Aql, is a yellow hypergiant star located in the constellation of Aquila at a distance of 4-6 kiloparsecs of the Sun.
PZ Cassiopeiae is a red supergiant star located in the Cassiopeia constellation, and a semi-regular variable star.
V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8
AH Scorpii is a red supergiant variable star located in the constellation Scorpius. It is one of the largest stars known by radius and is also one of the most luminous red supergiant stars in the Milky Way.
10 Persei is a blue supergiant star in the constellation Perseus. Its apparent magnitude is 6.26 although it is slightly variable.
RS Persei is a red supergiant variable star located in the Double Cluster in Perseus. The star's apparent magnitude varies from 7.82 to 10.0, meaning it is never visible to the naked eye.
T Persei is a red supergiant located in the constellation Perseus. It varies in brightness between magnitudes 8.3 and 9.7 and is considered to be a member of the Double Cluster.
V520 Persei is a blue supergiant member of NGC 869, one of the Perseus Double Cluster open clusters. It is an irregular variable star.
XX Persei is a semiregular variable red supergiant star in the constellation Perseus, between the Double Cluster and the border with Andromeda.
U Lacertae is a spectroscopic binary star in the constellation Lacerta.