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 | |
| 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, 32.8 light years from the Sun.[1]
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
- 1 2 3 4 5 6 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.Vizier catalog entry
- 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:1112.3316, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101. See Table 10.
- ↑ 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
- ↑ 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
- 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
- 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
External links
- "ARICNS 4C00155". ARI Data Base for Nearby Stars. Astronomisches Rechen-Institut. March 4, 1998. Retrieved 2008-02-27.
- SolStation
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