58 Eridani

58 Eridani
Observation data
Epoch J2000      Equinox J2000
Constellation Eridanus
Right ascension 04h 47m 36.29148s[1]
Declination –16° 56′ 04.0413″[1]
Apparent magnitude (V) 5.49[2]
Characteristics
Spectral type G1.5 V CH-0.5[3]
U−B color index +0.13[2]
B−V color index +0.64[2]
Variable type BY Dra
Astrometry
Radial velocity (Rv)23.00 ± 0.56[4] 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
Distance43.3 ± 0.2 ly
(13.28 ± 0.06 pc)
Absolute magnitude (MV)4.87[5]
Details
Mass1.053 ± 0.007[6] M☉
Surface gravity (log g)4.50±0.02[7] cgs
Temperature5,820 ± 5.7[8] K
Metallicity [Fe/H]0.030±0.007[7] dex
Rotation7.6 days[9]
Rotational velocity (v sin i)3.37±0.11[7] km/s
Age600[10] Myr
Other designations
58 Eri, BD-17° 954, GCTP 1070.00, Gl 177, HD 30495, HIP 22263, HR 1532, LTT 2088, SAO 149888.
Database references
SIMBADdata

58 Eridani is a main-sequence star in the constellation Eridanus. It is considered a solar analogue,[11] 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.[9]

The X-ray emissions from this star's corona indicate an age of less than a billion (109) years,[12] 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.[13]

See also

References

  1. 1 2 3 4 5 van Leeuwen, F. (November 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.
  2. 1 2 3 Cousins, A. W. J. (1973), "UBV photometry of some southern stars", Monthly Notes of the Astronomical Society of Southern Africa, 32: 11, Bibcode:1973MNSSA..32...11C.
  3. ↑ 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, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637.
  4. ↑ Valenti, Jeff A.; Fischer, Debra A. (July 2005), "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs", The Astrophysical Journal Supplement Series, 159 (1): 141–166, Bibcode:2005ApJS..159..141V, doi:10.1086/430500.
  5. ↑ 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, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191.
  6. ↑ Ramírez, I.; et al. (December 2014), "The Solar Twin Planet Search. I. Fundamental parameters of the stellar sample", Astronomy & Astrophysics, 572: 19, arXiv:1408.4130, Bibcode:2014A&A...572A..48R, doi:10.1051/0004-6361/201424244, A48.
  7. 1 2 3 dos Santos, Leonardo A.; et al. (August 2016), "The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars", Astronomy & Astrophysics, 592: 8, arXiv:1606.06214, Bibcode:2016A&A...592A.156D, doi:10.1051/0004-6361/201628558, A156.
  8. ↑ 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
  9. 1 2 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
  10. ↑ 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
  11. ↑ 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.
  12. ↑ E.J. Gaidos; G. Gonzalez (2002). "Stellar Atmospheres of Nearby Young Solar Analogs". New Astronomy. 7 (5): 211–226. arXiv:astro-ph/0203518. Bibcode:2002NewA....7..211G. doi:10.1016/S1384-1076(02)00108-2.
  13. ↑ 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. arXiv:astro-ph/0307398. Bibcode:1999JRASC..93..122F. doi:10.1016/j.newast.2003.07.002.
  • "58 Eridani". SolStation. Archived from the original on 26 June 2006. Retrieved 2006-07-28.
  • "Gl 177". ARICNS. 2006-06-06. Archived from the original on March 2, 2004. Retrieved 2015-12-28.
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