HR 511

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HR 511
Observation data
Epoch J2000
Constellation
(pronunciation)		 Cassiopeia
Right ascension 01h 47m 44.83s
Declination +63° 51′ 09.0″
Apparent magnitude (V) 5.63
Characteristics
Spectral type K0 V
U-B color index 0.41
B-V color index 0.81
Variable type None
Astrometry
Radial velocity (Rv) +2.8 km/s
Proper motion (μ) RA: 582.03 mas/yr
Dec.: −246.86 mas/yr
Parallax (π) 100.24 ± 0.68 mas
Distance 32.5 ± 0.2 ly
(9.98 ± 0.07 pc)
Absolute magnitude (MV) 5.64
Details
Mass 0.85[1] M☉
Radius 0.83[2] R☉
Luminosity 0.53[3] L☉
Temperature 5420[3] K
Metallicity 95.5%[4]
Rotation 21.67 days (2 km/s)[3]
Age 2.3-4 × 109[3] years
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.[3] Based on an iron abundance of [-0.02], the metallicity of this star appears to be similar to that of the Sun.[4]

[edit] References

  1. ^ H. M. Johnson, C. D. Wright (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". Astrophysical Journal Supplement Series 53: 643–711. doi:10.1086/190905. 
  2. ^ Approximating the star as a black body, then RHR 511 / RSun = (TSun/THR 511)2 × ( LHR 511 / LSun )0.5 = 1.14 × 0.73 = 0.83
  3. ^ a b c d e E. J. Gaidos, G. W. Henry, S. M. Henry (2000). "Spectroscopy and Photometry of Nearby Young Solar Analogs" ([dead link]). The Astronomical Journal 120 (2): 1006–1013. doi:10.1086/301488. 
  4. ^ a b S. Feltzing, G. Gonzalez (2001). "The nature of super-metal-rich stars. Detailed abundance analysis of 8 super-metal-rich star candidates". Astronomy and Astrophysics 367: 253–265. doi:10.1051/0004-6361:20000477. 

[edit] External links