HR 1614 (284 G. Eridani, GJ 183) is a star in the constellation Eridanus. Based upon parallax measurements, it is about 28.8 light-years (8.8 parsecs) distant from the Earth.[1] It is a main sequence star with a stellar classification of K3V.[2] The chromosphere has an effective temperature of about 4,945 K,[3] which gives this star the orange hue characteristic of K-type stars.[4] It has about 84% of the Sun's mass and 78% of the Sun's radius.[5]

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.[6] The activity cycle for this star is 11.1 years in length.[7] Based upon gyrochronology, the estimated age of this star is 4.5 Gyr.[8]

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.[9] The estimated age of this group is 2 Gyr, suggesting a corresponding age for this star.[10]

See also

References

  1. ^
  2. ^ 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. arXiv:0911.0760. Bibcode:2009A&A...508.1313F. doi:10.1051/0004-6361/200913327. S2CID 118361131
  3. ^ 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/0308429. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378. S2CID 18478960
  4. ^ "The Colour of Stars". Australia Telescope, Outreach and Education. Commonwealth Scientific and Industrial Research Organisation. December 21, 2004. Archived from the original on March 18, 2012. Retrieved 2012-01-16.
  5. ^ 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/0607235. Bibcode:2007ApJS..168..297T. doi:10.1086/509763. S2CID 18775378
  6. ^ 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
  7. ^ "H-K Project: Activity Cycles". Mt. Wilson Observatory. Archived from the original on 2012-02-06. Retrieved 2006-11-30.
  8. ^ Barnes, Sydney A. (November 2007). "Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors". The Astrophysical Journal. 669 (2): 1167–1189. arXiv:0704.3068. Bibcode:2007ApJ...669.1167B. doi:10.1086/519295. S2CID 14614725
  9. ^ 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
  10. ^ 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