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HR 511 (also designated V987 Cassiopeiae and Gliese 75 among others) is an orange dwarf of spectral type K0V in the constellation Cassiopeia. With an apparent magnitude of 5.63,[3] it is faintly visible to the naked eye. The star is relatively close, 32.8 light-years from the Sun, just above 10 parsecs.[2]

This star is estimated to be about the same age as the Sun, with 83% of the mass of the Sun and 82% of the Sun’s radius. It has not been identified as a member of any moving star groups. This star has displayed unusual emissions of Ca II and is much more x-ray luminous than the Sun. It is considered a relatively active star.[10] Based on an iron abundance of [Fe/H] = −0.02, the metallicity of this star appears to be similar to that of the Sun.[9]

References

  1. ^ Anderson, E.; Francis, Ch. (May 2012), “XHIP: An extended hipparcos compilation”, Astronomy Letters, 38 (5): 331–346, arXiv:1108.4971, Bibcode:2012AstL…38..331A, doi:10.1134/S1063773712050015, eISSN 1562-6873, ISSN 1063-7737, S2CID 119257644
  2. ^ a b c d e f g Vallenari, A.; et al. (Gaia collaboration) (2023). “Gaia Data Release 3. Summary of the content and survey properties”. Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A…674A…1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b c Mermilliod, J.-C. (1986), “Compilation of Eggen’s UBV data, transformed to UBV (unpublished)”, Catalogue of Eggen’s UBV Data. SIMBAD, Bibcode:1986EgUBV……..0M
  4. ^ a b White, Russel J.; Gabor, Jared M.; Hillenbrand, Lynne A. (June 2007), “High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun”, The Astronomical Journal, 133 (6): 2524–2536, arXiv:0706.0542, Bibcode:2007AJ….133.2524W, doi:10.1086/514336, S2CID 122854
  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, S2CID 118577511
  6. ^ a b Boyajian, Tabetha S.; et al. (February 2012), “Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars”, The Astrophysical Journal, 746 (1): 101, arXiv:1112.3316, Bibcode:2012ApJ…746..101B, doi:10.1088/0004-637X/746/1/101, S2CID 18993744. See Table 10.
  7. ^ Demory, B.-O.; et al. (October 2009), “Mass-radius relation of low and very low-mass stars revisited with the VLTI”, Astronomy and Astrophysics, 505 (1): 205–215, arXiv:0906.0602, Bibcode:2009A&A…505..205D, doi:10.1051/0004-6361/200911976, S2CID 14786643
  8. ^ 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
  9. ^ a b 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 (1): 253–265, Bibcode:2001A&A…367..253F, doi:10.1051/0004-6361:20000477
  10. ^ a b c d Gaidos, E. J.; Henry, G. W.; Henry, S. M. (2000), “Spectroscopy and Photometry of Nearby Young Solar Analogs”, The Astronomical Journal, 120 (2): 1006–1013, Bibcode:2000AJ….120.1006G, CiteSeerX 10.1.1.43.4478, doi:10.1086/301488, S2CID 16930014
  11. ^ “HR 511”, SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2016-07-09