Phi Persei

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φ Persei
Perseus constellation map.svg
Red circle.svg

Location of φ Persei (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 01h 43m 39.63792s[1]
Declination 50° 41′ 19.4328″[1]
Apparent magnitude (V) 4.06[2] (3.96 - 4.11[3])
Characteristics
Spectral type B2Vep[4]
U−B color index -0.92[2]
B−V color index -0.04[2]
Variable type γ Cas[3]
Astrometry
Radial velocity (Rv) +0.80[5] km/s
Proper motion (μ) RA: +24.59[1] mas/yr
Dec.: -14.01[1] mas/yr
Parallax (π) 4.54 ± 0.20[1] mas
Distance 720 ± 30 ly
(220 ± 10 pc)
Absolute magnitude (MV) −3.11[6]
Orbit[6][7]
Period (P) 126.6731 days
Semi-major axis (a) 5.89 mas
Inclination (i) 77.6°
Longitude of the node (Ω) 295.7°
Periastron epoch (T) 2456110.03
Semi-amplitude (K1)
(primary)
9.97 km/s
Semi-amplitude (K2)
(secondary)
81.3 km/s
Details
A
Mass 10.1[8] M
Radius 5.5 - 8.0[6] R
Luminosity 41,783[9] L
Surface gravity (log g) 4.46[9] cgs
Temperature 32,090[9] K
Rotational velocity (v sin i) 440[9] km/s
B
Mass 1.14[10] M
Radius 1.3[10] R
Surface gravity (log g) 4.2[6] cgs
Temperature 53,000[10] K
Age 21.5[8] Myr
Other designations
φ Persei, φ Per, Phi Per, BD+49°444, FK5 57, GC 2102, HD 10516, HIP 8068, HR 496, PPM 26670, SAO 22554
Database references
SIMBAD data

Phi Persei (Phi Per, φ Persei, φ Per) is a Class B2Vpe, fourth-magnitude star in the constellation Perseus. Phi Persei is binary consisting of a blue main sequence primary of class B2 and an apparent magnitude of 4.01 and a hot subdwarf secondary. Due to its rapid rotation, the primary has a polar radius about 5.5 R and an equatorial radius of about 8.0 R. Phi Persei is also a variable star with rapid variations in its brightness and spectrum. The Phi Persei stellar system is located about 716 light-years from Earth.

Naming[edit]

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.[11]

In Chinese, 天大將軍 (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, φ Persei itself is known as 天大將軍二 (Tiān Dà Jiāng Jūn èr, English: the Second Star of Heaven's Great General.).[12]

References[edit]

  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.  Vizier catalog entry
  2. ^ a b c Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D. 
  3. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....1.2025S. 
  4. ^ Hoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally published in: 1964BS....C......0H. 5050. Bibcode:1995yCat.5050....0H. 
  5. ^ Wilson, R. E. (1953). General Catalogue of Stellar Radial Velocities. Carnegie Institution for Science. Bibcode:1953GCRV..C......0W. LCCN 54001336. 
  6. ^ a b c d Gies, Douglas R.; Bagnuolo, William G.; Ferrara, Elizabeth C.; Kaye, Anthony B.; Thaller, Michelle L.; Penny, Laura R.; Peters, Geraldine J. (1998). "Hubble Space Telescope Goddard High Resolution Spectrograph Observations of the Be + sdO Binary φ Persei". The Astrophysical Journal. 493: 440–450. Bibcode:1998ApJ...493..440G. doi:10.1086/305113. 
  7. ^ "Sixth Catalog of Orbits of Visual Binary Stars". Retrieved 29 December 2016. 
  8. ^ a b Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410: 190–200. arXiv:1007.4883Freely accessible. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x.  Vizier catalog entry
  9. ^ a b c d Zorec, J.; Frémat, Y.; Domiciano De Souza, A.; Royer, F.; Cidale, L.; Hubert, A.-M.; Semaan, T.; Martayan, C.; Cochetti, Y. R.; Arias, M. L.; Aidelman, Y.; Stee, P. (2016). "Critical study of the distribution of rotational velocities of Be stars". Astronomy & Astrophysics. 595: A132. Bibcode:2016A&A...595A.132Z. doi:10.1051/0004-6361/201628760. 
  10. ^ a b c Krtička, J.; Kubát, J.; Krtičková, I. (2016). "Stellar wind models of subluminous hot stars". Astronomy & Astrophysics. 593: A101. arXiv:1607.04445Freely accessible. Bibcode:2016A&A...593A.101K. doi:10.1051/0004-6361/201628433. 
  11. ^ Wagman, M. (August 1987). "Flamsteed's Missing Stars". Journal for the History of Astronomy, Vol.18, NO. 3/AUG, P.209, 1987. 18: 212. Bibcode:1987JHA....18..209W. doi:10.1177/002182868701800305. 
  12. ^ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 10 日

External links[edit]