HR 511
  | |
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Cassiopeia |
| Right ascension | 01h47m44.83363s[1] |
| Declination | +63° 51′ 09.0073″[1] |
| Apparent magnitude(V) | 5.63[2] |
| Characteristics | |
| Spectral type | K0 V[3] |
| U−Bcolor index | +0.40[2] |
| B−Vcolor index | +0.80[3] |
| Astrometry | |
| Radial velocity(Rv) | +1.41[3]km/s |
| Proper motion(μ) | RA:+582.028±0.070[1]mas/yr Dec.:−246.228±0.086[1]mas/yr |
| Parallax(π) | 99.5746 ± 0.0595mas[1] |
| Distance | 32.75 ± 0.02ly (10.043 ± 0.006pc) |
| Absolute magnitude(MV) | 5.61[4] |
| Details | |
| Mass | 0.825±0.021[5]M☉ |
| Radius | 0.819±0.024[6]R☉ |
| Luminosity | 0.516±0.010[5]L☉ |
| Temperature | 5,407±4.0[7]K |
| Metallicity[Fe/H] | −0.02[8]dex |
| Rotation | 21.67 days[9] |
| Rotational velocity(vsini) | 2.0[9]km/s |
| Age | 2.2 - 3.5[9]Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
HR 511(also designatedV987 CassiopeiaeandGliese 75among others) is anorange dwarfofspectral typeK0V in theconstellationCassiopeia.With anapparent magnitudeof 5.63,[2]it is faintly visible to the naked eye. The star is relatively close, 32.8light yearsfrom theSun.[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 anymoving star groups.This star has displayed unusual emissions ofCa IIand is much morex-rayluminous than the Sun. It is considered a relatively active star.[9]Based on an iron abundance of [Fe/H] = −0.02, themetallicityof this star appears to be similar to that of the Sun.[8]
References
[edit]- ^abcdefBrown, A. G. A.;et al. (Gaia collaboration) (August 2018)."GaiaData Release 2: Summary of the contents and survey properties ".Astronomy & Astrophysics.616.A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051.Gaia DR2 record for this sourceatVizieR.
- ^abcMermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)",Catalogue of Eggen's UBV Data. SIMBAD,Bibcode:1986EgUBV........0M
- ^abcWhite, 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,S2CID122854
- ^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,S2CID118577511
- ^abBoyajian, 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,S2CID18993744.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,S2CID14786643
- ^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,S2CID18478960
- ^abFeltzing, 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
- ^abcdGaidos, 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,CiteSeerX10.1.1.43.4478,doi:10.1086/301488,S2CID16930014
- ^"HR 511",SIMBAD,Centre de données astronomiques de Strasbourg,retrieved2016-07-09
External links
[edit]- "ARICNS 4C00155".ARI Data Base for Nearby Stars.Astronomisches Rechen-Institut. March 4, 1998. Archived fromthe originalon 2008-10-17.Retrieved2008-02-27.
- SolStation
