HR 511

HR 511
Observation data
Epoch J2000      Equinox J2000
Constellation Cassiopeia
Right ascension 01h 47m 44.83s[1]
Declination +63° 51′ 09.0″[1]
Apparent magnitude (V) 5.63[2]
Characteristics
Spectral type K0 V[3]
U−B color index +0.40[2]
B−V color index +0.80[3]
Astrometry
Radial velocity (Rv)+1.41[3] km/s
Proper motion (μ) RA: +582.03±0.35[1] mas/yr
Dec.: −246.93±0.43[1] mas/yr
Parallax (π)99.33 ± 0.53[1] mas
Distance32.8 ± 0.2 ly
(10.07 ± 0.05 pc)
Details
Mass0.825±0.021[4] M☉
Radius0.819±0.024[5] R☉
Luminosity0.516±0.010[4] L☉
Temperature5407±4.0[6] K
Metallicity95.5%[7]
Metallicity [Fe/H]−0.02[7] dex
Rotation21.67 days[8]
Rotational velocity (v sin i)2[8] km/s
Age2.3-4[8] Gyr
Other designations
BD +63°238, GCTP 371.00, GJ 75, HD 10780, HIP 8362, HR 511, LHS 1297, LTT 10619, SAO 11983.[9]

HR 511 (also designated Gliese 75 among others) is an orange dwarf of spectral type K0V in the constellation Cassiopeia. With an apparent magnitude of 5.63,[2] it is faintly visible to the naked eye. The star is relatively close, 32.8 light years from the Sun.[1]

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.[8] Based on an iron abundance of [Fe/H] = -0.02, the metallicity of this star appears to be similar to that of the Sun.[7]

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (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.Vizier catalog entry
  2. 1 2 3 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data. SIMBAD, Bibcode:1986EgUBV........0M
  3. 1 2 3 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:0706.0542Freely accessible, Bibcode:2007AJ....133.2524W, doi:10.1086/514336.
  4. 1 2 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:1112.3316Freely accessible, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101. See Table 10.
  5. ↑ 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:0906.0602Freely accessible, Bibcode:2009A&A...505..205D, doi:10.1051/0004-6361/200911976
  6. ↑ 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
  7. 1 2 3 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
  8. 1 2 3 4 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, doi:10.1086/301488
  9. ↑ "HR 511 -- Variable of BY Dra type", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2016-07-09.
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