Phi Gruis

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Omega Persei
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Grus
Right ascension 23h 18m 09.88348s[1]
Declination −40° 49′ 27.7089″[1]
Apparent magnitude (V) 5.49[2]
Characteristics
Spectral type F4 V[3]
U−B color index −0.05[2]
B−V color index +0.47[2]
Astrometry
Proper motion (μ) RA: +126.28[1] mas/yr
Dec.:  mas/yr
Parallax (π) 28.24 ± 0.34[1] mas
Distance 115 ± 1 ly
(35.4 ± 0.4 pc)
Absolute magnitude (MV) 2.82[4]
Details
Mass 1.26[5] M
Surface gravity (log g) 4.10±0.14[5] cgs
Temperature 6,607±225[5] K
Metallicity [Fe/H] −0.24[3] dex
Rotational velocity (v sin i) 19.9±1.0[4] km/s
Age 1.623[5] Gyr
Other designations
φ Gru,  Gruis, CD−41° 15211, GJ 4330, HD 219693, HIP 115054, HR 8859, SAO 231539[6]
Database references
SIMBAD data

φ Gruis, Latinised as Phi Gruis, is a solitary,[7] yellow-white hued star in the southern constellation of Grus. It is faintly visible to the naked eye with an apparent visual magnitude of +5.49.[2] Based upon an annual parallax shift of 28.24 mas as seen from the Earth,[1] it is 115 light years from the Sun. This is an F-type main-sequence star with a stellar classification of F4 V,[3] with the luminosity class of 'V' indicating it is currently generating energy through hydrogen fusion at its core.

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, Bibcode:2007A&A...474..653V, arXiv:0708.1752Freely accessible, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d Przybylski, A.; Kennedy, P. M. (1965), "Radial velocities and three-colour photometry of 166 southern stars", Monthly Notices of the Royal Astronomical Society, 131: 95–104, Bibcode:1965MNRAS.131...95P, doi:10.1093/mnras/131.1.95. 
  3. ^ a b c Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, Bibcode:2006AJ....132..161G, arXiv:astro-ph/0603770Freely accessible, doi:10.1086/504637. 
  4. ^ a b Ammler-von Eiff, M.; Reiners, A. (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: 31, Bibcode:2012A&A...542A.116A, arXiv:1204.2459Freely accessible, doi:10.1051/0004-6361/201118724, A116. 
  5. ^ a b c d David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, Bibcode:2015ApJ...804..146D, arXiv:1501.03154Freely accessible, doi:10.1088/0004-637X/804/2/146. 
  6. ^ "phi Gru -- Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-06-19. 
  7. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, Bibcode:2008MNRAS.389..869E, arXiv:0806.2878Freely accessible, doi:10.1111/j.1365-2966.2008.13596.x.