HR 511

In this article, we will explore the impact of HR 511 on various aspects of today's society. From its influence on technology to its effects on popular culture, HR 511 has captured the attention of millions of people around the world. Through in-depth analysis, we will examine how HR 511 has shaped our lives and caused significant changes in our perception of the world. Since its emergence, HR 511 has sparked passionate debates and has been the subject of countless investigations, leading us to reflect on its relevance in the contemporary context.

HR 511
Location of HR 511 (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Cassiopeia[1]
Right ascension 01h 47m 44.83444s[2]
Declination +63° 51′ 09.0110″[2]
Apparent magnitude (V) 5.63[3]
Characteristics
Spectral type K0 V[4]
U−B color index +0.40[3]
B−V color index +0.80[4]
Astrometry
Radial velocity (Rv)+2.62±0.12[2] km/s
Proper motion (μ) RA: +581.684 mas/yr[2]
Dec.: −246.462 mas/yr[2]
Parallax (π)99.5902±0.0438 mas[2]
Distance32.75 ± 0.01 ly
(10.041 ± 0.004 pc)
Absolute magnitude (MV)5.61[5]
Details
Mass0.825±0.021[6] M☉
Radius0.819±0.024[7] R☉
Luminosity0.516±0.010[6] L☉
Temperature5,407±4.0[8] K
Metallicity −0.02[9] dex
Rotation21.67 days[10]
Rotational velocity (v sin i)2.0[10] km/s
Age2.2 - 3.5[10] Gyr
Other designations
V987 Cassiopeiae, BD+63°238, GJ 75, HD 10780, HIP 8362, HR 511, SAO 11983, LHS 1297, LTT 10619[11]
Database references
SIMBADdata
ARICNSdata

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.[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 = −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 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