Phi2 Orionis

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For other stars with this Bayer designation, see Phi Orionis.
φ2 Orionis
Orion constellation map.svg
Red circle.svg
φ2 (circled) in the constellation Orion
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Orion
Right ascension 05h 36m 54.38819s[1]
Declination +09° 17′ 26.4096″[1]
Apparent magnitude (V) 4.081[2]
Characteristics
Spectral type G8 III-IV[3]
U−B color index +0.618[2]
B−V color index +0.966[2]
Astrometry
Radial velocity (Rv)+98.96±0.09[4] km/s
Proper motion (μ) RA: +97.24[1] mas/yr
Dec.: −305.57[1] mas/yr
Parallax (π)27.76 ± 0.27[1] mas
Distance117 ± 1 ly
(36.0 ± 0.4 pc)
Absolute magnitude (MV)+1.33±0.07[5]
Details[4]
Mass1.07±0.04 M☉
Radius7.72±0.27 R☉
Luminosity31.6 L☉
Surface gravity (log g)3.00±0.02 cgs
Temperature4,856±11 K
Metallicity [Fe/H]−0.56±0.02 dex
Rotational velocity (v sin i)1.91±0.53 km/s
Age6.91±1.04 Gyr
Other designations
φ2 Ori, 40 Orionis, BD+09° 898, HD 37160, HIP 26366, HR 1907, SAO 112958[6]
Database references
SIMBADdata
Yellow φ2 Orionis with nebulosity east of φ1 Orionis and south-east of λ Orionis

Phi2 Orionis is a star in the constellation Orion, where it forms a small triangle on the celestial sphere with the nearby Meissa and Phi1 Orionis.[7] This star is visible to the naked eye with an apparent visual magnitude of 4.081.[2] Based upon an annual parallax shift of 27.76 mas,[1] it is located around 117 light-years from the Sun.

This is a G-type giant or subgiant star with a stellar classification of G8 III-IV[3] that, at the age of 6.9 billion years, is evolving away from the main sequence. It has 1.07 times the mass of the Sun, but has expanded to 7.72 times the Sun's radius. The star shines with 31.6 times the solar luminosity from its outer atmosphere at an effective temperature of 4,856 K.[4]

References[]

  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. ^ a b c d Cousins, A. W. J. (1984), "Standardization of Broadband Photometry of Equatorial Standards", South African Astronomical Observatory Circulars, 8: 59, Bibcode:1984SAAOC...8...59C.
  3. ^ a b Frasca, A.; et al. (December 2009), "REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters", Astronomy and Astrophysics, 508 (3): 1313–1330, arXiv:0911.0760, Bibcode:2009A&A...508.1313F, doi:10.1051/0004-6361/200913327, S2CID 118361131.
  4. ^ a b c Jofré, E.; et al. (2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics, 574: A50, arXiv:1410.6422, Bibcode:2015A&A...574A..50J, doi:10.1051/0004-6361/201424474, S2CID 53666931, A50.
  5. ^ Charbonnel, Corinne; et al. (April 1998), "Mixing processes during the evolution of red giants with moderate metal deficiencies: the role of molecular-weight barriers", Astronomy and Astrophysics, 332: 204–214, arXiv:astro-ph/9712207, Bibcode:1998A&A...332..204C.
  6. ^ "phi02 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-11-30.CS1 maint: postscript (link)
  7. ^ Kaler, James B. (February 10, 2012), "Phi-1 Orionis", Stars, University of Illinois, retrieved 2016-11-30.
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