Phi Persei
{{short description|Star in the constellation Perseus}}
{{Starbox begin
| name = φ Persei
}}
{{Starbox image
|image=
{{Location mark
|image=Perseus constellation map.svg|alt=|float=center|width=280
|label=|position=right
|mark=Red circle.svg|mark_width=10|mark_link=Phi Persei
|x=978|y=307
}}
|caption=Location of φ Persei (circled)
}}
{{Starbox observe
| epoch = J2000
| constell = Perseus
| dec = {{DEC|+50|41|19.4328}}
| appmag_v = 4.06 {{nowrap|(3.96 - 4.11)}}
}}
{{Starbox character
| class = B2Vep + sdO
| variable = γ Cas
}}
{{Starbox astrometry
| parallax = 4.54
| p_error = 0.20
}}
{{Starbox orbit
| period_unitless = 126.6731 days
| axis_unitless = {{val|5.89|ul=mas}}
| inclination = 77.6
| node = 295.7
| periastron = 2456110.03
| k1 = 9.97
| k2 = 81.3
}}
{{Starbox detail
| component1 = A
| component2 = B
}}
{{Starbox catalog
| names = φ Persei, φ Per, Phi Per, 54 Andromedae, BD+49°444, FK5 57, GC 2102, HD 10516, HIP 8068, HR 496, PPM 26670, SAO 22554
}}
{{Starbox reference
| Simbad = Phi+Persei
}}
{{Starbox end}}
Phi Persei (Phi Per, φ Persei, φ Per) is a class B2Vep fourth-magnitude star in the constellation Perseus, location about 720 light-years from Earth.
System
Phi Persei is spectroscopic binary consisting of a blue main sequence primary of class B2 and a hot subdwarf secondary. The two stars have an orbit of 217 days and are separated by about {{solar radius|200|link=y}}. Phi Persei is a runaway star and extrapolating its space velocity backwards by the modelled age of the system (57 million years) places it within the Alpha Persei cluster.
The primary star rotates rapidly with a projected equatorial velocity of {{val|440|u=km/s}}. Due to its rapid rotation, the primary star has a polar radius about {{solar radius|5.5}} and an equatorial radius of about {{solar radius|8.0}}. With an effective temperature of nearly {{val|30,000|fmt=commas|ul=K}}, it has a bolometric luminosity nearly 15,000 times higher than the Sun. The rapidly-spinning star is surrounded by a circumstellar disk. The binary orbit, the spin of the primary star, and the disk are all seen nearly edge-on. There are no eclipses, but models of the system show that the disk significantly obscures the primary star. The primary formed as a {{solar mass|3.8}} star and has accreted material from its companion.
The secondary star is also a class O subdwarf, hotter than the primary but smaller and less massive. It is proposed that it is the core of a {{solar mass|7}} star, with the outer layers stripped as it expanded away from the main sequence. Its luminosity is higher than expected for a normal {{solar mass|1.2}} helium star, which suggests it may have evolved to helium shell burning. Although the subdwarf has a bolometric luminosity about half that of the primary, it emits most of its radiation as ultraviolet, being only about 3% as bright as the primary at visible wavelengths.
Variability
File:PhiPerLightCurve.png light curve for Phi Persei, adapted from Božić et al. (1995)]]
Phi Persei is a variable star with both rapid and longterm variations in its brightness and spectrum. Variations occur on a daily timescale which may be related to the rotation of the primary star. Any variations originating with the secondary are difficult to detect due to its comparative faintness. Slower variations, including deep fades, are also seen. Some of the variations may correspond to the orbital period, possibly eclipses of gas streams or hot spots, but the occasional deep fades do not match any particular orbital phase. The variations are classified as γ Cassiopeiae-type, shell stars with eruptions and irregular fading.
Naming
Flamsteed followed Ptolemy in treating φ Persei as being in Andromeda and gave it the designation 54 Andromedae. It is isolated from the main stars of Perseus, but lies within its formal borders.
In Chinese, {{lang|zh|天大將軍}} ({{lang|zh-Latn|Tiān Dà Jiāng Jūn}}), meaning Heaven's Great General, refers to an asterism consisting of φ Persei, γ Andromedae, 51 Andromedae, 49 Andromedae, χ Andromedae, υ Andromedae, τ Andromedae, 56 Andromedae, β Trianguli, γ Trianguli and δ Trianguli. Consequently, the Chinese name for φ Persei itself is {{lang|zh|天大將軍二}} ({{lang|zh-Latn|Tiān Dà Jiāng Jūn èr}}, {{langx|en|the Second Star of Heaven's Great General}}.).
{{clear left}}
References
{{reflist|refs=
{{cite constellation|Phi Persei}}
{{cite journal | last=Wilson | first=R. E. | year=1953 | title=General Catalogue of Stellar Radial Velocities | journal=Carnegie Institute Washington D.C. Publication | publisher=Carnegie Institution for Science | bibcode=1953GCRV..C......0W | lccn=54001336 }}
| last=Wagman | first=M.
| title=Flamsteed's Missing Stars
| journal=Journal for the History of Astronomy |issue=3 | volume=18 | page=212 |date=August 1987
| bibcode=1987JHA....18..209W | doi=10.1177/002182868701800305| s2cid=118445625
}}
}}
External links
- [http://hubblesite.org/newscenter/archive/releases/1997/39 HST Press release on the φ Per binary system]
{{Stars of Perseus}}
{{DEFAULTSORT:Phi Persei}}
Category:Perseus (constellation)
Category:B-type main-sequence stars