Nu Phoenicis

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Nu Phoenicis
Phoenix constellation map.svg
Red circle.svg

Location of ν Phoenicis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Phoenix
Right ascension 01h 15m 11.12150s[1]
Declination –45° 31′ 53.9954″[1]
Apparent magnitude (V) 4.95[2]
Spectral type F9 V Fe+0.4[3]
U−B color index +0.09[2]
B−V color index +0.57[2]
Radial velocity (Rv) +11.7[4] km/s
Proper motion (μ) RA: 665.13 ± 0.20[1] mas/yr
Dec.: 177.63 ± 0.19[1] mas/yr
Parallax (π) 66.16 ± 0.24[1] mas
Distance 49.3 ± 0.2 ly
(15.11 ± 0.05 pc)
Absolute magnitude (MV) 4.28[5]
Mass 1.20−1.25[6] M
Radius 1.25[7] R
Surface gravity (log g) 4.30[3] cgs
Temperature 6,069[3] K
Metallicity [Fe/H] +0.02[3] dex
Rotational velocity (v sin i) 3.7[7] km/s
Age 5.7[5] Gyr
Other designations
CD–46° 346, GCTP 257.00, Gl 55, HD 7570, HIP 5862, HR 370, LHS 1220, LTT 696, SAO 215428.[8]
Database references

Nu Phoenicis is a F-type main-sequence star in the southern constellation of Phoenix. It is visible to the naked eye with an apparent visual magnitude of 4.95.[2] This is a solar analogue, meaning its observed properties appear similar to the Sun, although it is somewhat more massive. At an estimated distance of around 49 light years,[1] this star is located relatively near the Sun.

Based on observations of excess infrared radiation from this star, it may possess a dust ring that extends outward several AU from an inner edge starting at 10 AU.[9]

See also[edit]


  1. ^ a b c d e f van Leeuwen, F. (November 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 ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data. SIMBAD, Bibcode:1986EgUBV........0M. 
  3. ^ a b c d 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. ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, Bibcode:2009A&A...501..941H, arXiv:0811.3982Freely accessible, doi:10.1051/0004-6361/200811191. 
  5. ^ a b Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. Bibcode:2008ApJ...687.1264M. arXiv:0807.1686Freely accessible. doi:10.1086/591785. 
  6. ^ Sousa, S.G.; et al. (2006), "Spectroscopic parameters for a sample of metal-rich solar-type stars", Astronomy and Astrophysics, 458 (3): 873–880, Bibcode:2006A&A...458..873S, doi:10.1051/0004-6361:20065658. 
  7. ^ a b Fuhrmann, K.; Chini, R. (2012), "Multiplicity among F-type Stars", The Astrophysical Journal Supplement, 203 (2): 20, Bibcode:2012ApJS..203...30F, doi:10.1088/0067-0049/203/2/30, 30. 
  8. ^ "nu. Phe -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2015-12-22. 
  9. ^ Beichman, C. A.; Tanner, A.; Bryden, G.; Stapelfeldt, K. R.; et al. (2006). "IRS Spectra of Solar-Type Stars: A Search for Asteroid Belt Analogs". Astrophysical Journal. 639 (2): 1166–1176. Bibcode:2006ApJ...639.1166B. arXiv:astro-ph/0601467Freely accessible. doi:10.1086/499424. 

External links[edit]