HR 511

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HR 511
Cassiopeia constellation map.svg
Red circle.svg

Location of HR 511 (circled)
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
Distance 32.8 ± 0.2 ly
(10.07 ± 0.05 pc)
Details
Mass 0.825±0.021[4] M
Radius 0.819±0.024[5] R
Luminosity 0.516±0.010[4] L
Temperature 5407±4.0[6] K
Metallicity 95.5%[7]
Metallicity [Fe/H] −0.02[7] dex
Rotation 21.67 days[8]
Rotational velocity (v sin i) 2[8] km/s
Age 2.3-4[8] Gyr
Other designations
V987 Cassiopeiae, BD+63°238, GJ 75, HD 10780, HIP 8362, HR 511, LHS 1297, LTT 10619, SAO 11983.[9]
Database references
SIMBAD data
ARICNS data

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,[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[edit]

  1. ^ a b c d e f 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. ^ a b c Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data.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 
  3. ^ a b c 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. ^ 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:1112.3316Freely 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. ^ a b c 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. ^ 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, 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. 

External links[edit]

  • "ARICNS 4C00155". ARI Data Base for Nearby Stars. Astronomisches Rechen-Institut. March 4, 1998. Retrieved 2008-02-27. 
  • SolStation