58 Eridani

58 Eridani is a main-sequence star in the constellation Eridanus. It is considered a solar analogue,[12] 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.[10]

58 Eridani
Observation data
Epoch J2000      Equinox J2000
Constellation Eridanus
Right ascension  04h 47m 36.29176s[1]
Declination –16° 56′ 04.0419″[1]
Apparent magnitude (V) 5.49[2]
Characteristics
Evolutionary stage main sequence
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[4]
Astrometry
Radial velocity (Rv)21.72±0.14[1] km/s
Proper motion (μ) RA: 130.04±0.37[5] mas/yr
Dec.: 169.27±0.28[5] mas/yr
Parallax (π)75.5213 ± 0.0795[1] mas
Distance43.19 ± 0.05 ly
(13.24 ± 0.01 pc)
Absolute magnitude (MV)4.87[6]
Details
Mass1.053±0.007[7] M☉
Radius0.96±0.03[1] R☉
Luminosity0.992±0.001[1] L☉
Surface gravity (log g)4.50±0.02[8] cgs
Temperature5,820±5.7[9] K
Metallicity [Fe/H]0.030±0.007[8] dex
Rotation7.6 days[10]
Rotational velocity (v sin i)3.37±0.11[8] km/s
Age600[11] Myr
Other designations
58 Eri, IX Eri, BD−17°954, GJ 177, HD 30495, HIP 22263, HR 1532, SAO 149888, LTT 2088
Database references
SIMBADdata

Characteristics

This is a BY Draconis variable with the designation IX Eridani, which ranges in magnitude from 5.47 down to 5.51 with a period of 11.3 days.[4] The X-ray emissions from this star's corona indicate an age of less than a billion (109) years,[13] 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.[14]

gollark: ~play harbinger of ☭
gollark: Sadly yes.
gollark: ~q
gollark: How come you have skip powers?
gollark: I only know how to materialize discord bots from pure aether, not make one myself.

See also

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. 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. Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085.
  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.
  6. 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.
  7. 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.
  8. 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.
  9. 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
  10. 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
  11. 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
  12. 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.
  13. 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.
  14. 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.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.