58 Eridani

From Wikipedia, the free encyclopedia
Jump to: navigation, search
58 Eridani
Observation data
Epoch J2000      Equinox J2000
Constellation Eridanus
Right ascension 04h 47m 36.29s[1]
Declination –16° 56′ 04.0″[1]
Apparent magnitude (V) 5.50
Spectral type G3 V
U−B color index 0.14
B−V color index 0.63
Variable type BY Dra
Radial velocity (Rv) +16.8 km/s
Proper motion (μ) RA: 130.04 ± 0.37[1] mas/yr
Dec.: 169.27 ± 0.28[1] mas/yr
Parallax (π) 75.32 ± 0.36[1] mas
Distance 43.3 ± 0.2 ly
(13.28 ± 0.06 pc)
Absolute magnitude (MV) 5.01
Mass 0.96 M
Radius 0.96 R
Luminosity 0.96 L
Temperature 5,820 ± 5.7[2] K
Metallicity [Fe/H] 0.00[3] dex
Rotation 7.6 days[3]
Rotational velocity (v sin i) 4 km/s
Age 600[4] Myr
Other designations
58 Eri, BD-17 954, GCTP 1070.00, Gl 177, HD 30495, HIP 22263, HR 1532, LTT 2088, SAO 149888.

58 Eridani is a main-sequence star in the constellation Eridanus. It is considered a solar analogue,[5] which means it has similar physical properties to the Sun. The star has a relatively high proper motion across the sky, and it is located about 43 light years distant. It is a probable member of the IC 2391 moving group of stars that share a common motion through space.[3]

The X-ray emissions from this star's corona indicate an age of less than a billion (109) years,[6] compared to 4.6 billion for the Sun, so it is still relatively young for a star of its mass. Starspot activity has also been detected, which varies from year to year.

A circumstellar disc of dust particles has been detected in orbit around 58 Eridani.[7]

See also[edit]


  1. ^ a b c d e van Leeuwen, F. (2007), "HIP 22263", Hipparcos, the New Reduction, retrieved 2009-12-11 
  2. ^ Kovtyukh et al. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics 411 (3): 559–564, arXiv:astro-ph/0308429, Bibcode:2003A&A...411..559K, doi:10.1051/0004-6361:20031378 
  3. ^ a b c Maldonado, J. et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948 
  4. ^ 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, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785 
  5. ^ E.J. Gaidos, G.W. Henry, S.M. Henry (2000). "Spectroscopy and Photometry of Nearby Young Solar Analogs". Astronomical Journal 120 (2): 1006–1013. Bibcode:2000AJ....120.1006G. doi:10.1086/301488. 
  6. ^ E.J. Gaidos, G. Gonzalez (2002). "Stellar Atmospheres of Nearby Young Solar Analogs". New Astronomy 7 (5): 211–226. arXiv:astro-ph/0203518. Bibcode:2002astro.ph..3518G. doi:10.1016/S1384-1076(02)00108-2. 
  7. ^ E. Gaidos, C. Koresko (2004). "A Survey of 10-Micron Silicate Emission from Dust around Young Sun-Like Stars". New Astronomy 93 (1): 33–42. Bibcode:1999JRASC..93..122F. doi:10.1016/j.newast.2003.07.002. 

External links[edit]