HR 511

From Wikipedia, the free encyclopedia
  (Redirected from V987 Cassiopeiae)
Jump to: navigation, search
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
Characteristics
Spectral type K0 V
U−B color index 0.41
B−V color index 0.81
Astrometry
Radial velocity (Rv) +2.8 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)
Absolute magnitude (MV) 5.64
Details
Mass 0.825 ± 0.021[2] M
Radius 0.819 ± 0.024[3] R
Luminosity 0.516 ± 0.010[2] L
Temperature 5407 ± 4.0[4] K
Metallicity 95.5%[5]
Metallicity [Fe/H] -0.02[5] dex
Rotation 21.67 days[6]
Rotational velocity (v sin i) 2[6] km/s
Age 2.3-4[6] Gyr
Other designations
GJ 75, HR 511, BD +63°238, HD 10780, LHS 1297, LTT 10619, GCTP 371.00, SAO 11983, HIP 8362.
Database references
SIMBAD data

HR 511 (also designated Gliese 75 among others) is an orange dwarf of spectral type K0V in the constellation Cassiopeia. The star is relatively close, 32.5 light years from the Sun.

This star is estimated to be about the same age as the sun. 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.[6] Based on an iron abundance of [Fe/H] = -0.02, the metallicity of this star appears to be similar to that of the Sun.[5]

References[edit]

  1. ^ a b c d e van Leeuwen, F. (2007). "HIP 8362". Hipparcos, the New Reduction. Retrieved 2009-12-11. 
  2. ^ 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 . See Table 10.
  3. ^ 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 
  4. ^ 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 
  5. ^ 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 
  6. ^ a b c d Gaidos; 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 

External links[edit]

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