HR 1614

HR 1614[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Eridanus
Right ascension 05h 00m 48.99977s[2]
Declination −05° 45′ 13.2303″[2]
Apparent magnitude (V) 6.208[3]
Characteristics
Spectral type K3 V[3]
U−B color index +1.00[4]
B−V color index +1.06[4]
Astrometry
Radial velocity (Rv)+21.0[5] km/s
Proper motion (μ) RA: 550.12±0.62[2] mas/yr
Dec.: −1,109.23±0.39[2] mas/yr
Parallax (π)114.84 ± 0.50[2] mas
Distance28.4 ± 0.1 ly
(8.71 ± 0.04 pc)
Details
Mass0.838+0.034
−0.033[6] M☉
Radius0.78+0.03
−0.02[6] R☉
Surface gravity (log g)4.55[3] cgs
Temperature4,945±8.7[7] K
Metallicity [Fe/H]0.28[3] dex
Rotational velocity (v sin i)4.1[8] km/s
Age2[9] or 4.5[10] Gyr
Other designations
284 G. Eridani, GJ 183, BD -05°1123, HD 32147, LHS 200, LTT 2142, GCTP 1129.00, SAO 131688, LPM 200, HIP 23311.[1]

HR 1614 (284 G. Eridani, GJ 183) is a star in the constellation Eridanus. Based upon parallax measurements, it is about 28.4 light-years (8.7 parsecs) distant from the Earth.[2] It is a main sequence star with a stellar classification of K3V.[3] The chromosphere has an effective temperature of about 4,945 K,[7] which gives this star the orange hue characteristic of K-type stars.[11] It has about 84% of the Sun's mass and 78% of the Sun's radius.[6]

It is considered a metal-rich dwarf star, which means it displays an unusually high portion of elements heavier than helium in its spectrum. This metallicity is given in term of the ratio of iron to hydrogen, as compared to the Sun. In the case of HR 1614, this ratio is about 90% higher than the Sun.[12] The activity cycle for this star is 11.1 years in length.[13] Based upon gyrochronology, the estimated age of this star is 4.5 Gyr.[10]

A 2015 study estimates that in around 10,460 years, HR 1614 will make its closest approach to the Sun at a distance of 1.8 ly (0.55 pc), although other studies predict a perihelion passage at 0.65–1.30 ly (0.2–0.4 pc) in 1.4 myr.[14] This system is a member of a moving group of at least nine stars that share a common motion through space. The members of this group display the same abundance of heavy elements as does HR 1614, which may indicate a common origin for these stars. The space velocity of this group relative to the Sun is 59 km/s.[15] The estimated age of this group is 2 Gyr, suggesting a corresponding age for this star.[9]

See also

References

  1. 1 2 "HD 32147 -- High proper-motion Star". Centre de Données astronomiques de Strasbourg. Retrieved 2006-06-08.
  2. 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357
  3. 1 2 3 4 5 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, Bibcode:2009A&A...508.1313F, doi:10.1051/0004-6361/200913327
  4. 1 2 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99), Bibcode:1966CoLPL...4...99J
  5. ↑ Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198Freely accessible, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959
  6. 1 2 3 Takeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297–318, arXiv:astro-ph/0607235Freely accessible, Bibcode:2007ApJS..168..297T, doi:10.1086/509763
  7. 1 2 Kovtyukh, V. V.; 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/0308429Freely accessible. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378.
  8. ↑ Schröder, C.; Reiners, A.; Schmitt, J. H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo", Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377
  9. 1 2 Feltzing, S.; Holmberg, J. (2000). "The reality of old moving groups - the case of HR 1614. Age, metallicity, and a new extended sample". Astronomy and Astrophysics. 357: 153–163. Bibcode:2000A&A...357..153F.
  10. 1 2 Barnes, Sydney A. (November 2007), "Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors", The Astrophysical Journal, 669 (2): 1167–1189, arXiv:0704.3068Freely accessible, Bibcode:2007ApJ...669.1167B, doi:10.1086/519295
  11. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16
  12. ↑ Feltzing, S.; Gonzalez, G. (2001). "The nature of super-metal-rich stars. Detailed abundance analysis of 8 super-metal-rich star candidates". Astronomy and Astrophysics. 367 (2): 253–265. Bibcode:2001A&A...367..253F. doi:10.1051/0004-6361:20000477.
  13. ↑ "H-K Project: Activity Cycles". Mt. Wilson Observatory. Retrieved 2006-11-30.
  14. ↑ Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648Freely accessible. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. A35.
  15. ↑ Eggen, O. J. (1992). "HR 1614 and the dissolution of a supercluster". Astronomical Journal. 104 (5): 1906–1915. Bibcode:1992AJ....104.1906E. doi:10.1086/116366.
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