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HR 511

From Wikipedia, the free encyclopedia
Star in the constellation Cassiopeia
HR 511
Location of HR 511 (circled)
Observation data
Epoch J2000      Equinox J2000
ConstellationCassiopeia
Right ascension01h 47m 44.83444s[1]
Declination+63° 51′ 09.0110″[1]
Apparent magnitude (V)5.63[2]
Characteristics
Spectral typeK0 V[3]
U−Bcolor index+0.40[2]
B−Vcolor index+0.80[3]
Astrometry
Radial velocity (Rv)+2.62±0.12[1] km/s
Proper motion (μ)RA: +581.684mas/yr[1]
Dec.: −246.462mas/yr[1]
Parallax (π)99.5902±0.0438 mas[1]
Distance32.75 ± 0.01 ly
(10.041 ± 0.004 pc)
Absolute magnitude (MV)5.61[4]
Details
Mass0.825±0.021[5] M
Radius0.819±0.024[6] R
Luminosity0.516±0.010[5] L
Temperature5,407±4.0[7] K
Metallicity [Fe/H]−0.02[8] dex
Rotation21.67 days[9]
Rotational velocity (v sin i)2.0[9] km/s
Age2.2 - 3.5[9] Gyr
Other designations
V987 Cassiopeiae,BD+63°238,GJ 75,HD 10780,HIP 8362,HR 511,SAO 11983,LHS 1297,LTT 10619[10]
Database references
SIMBADdata
ARICNSdata

HR 511 (also designatedV987 Cassiopeiae andGliese 75 among others) is anorange dwarf ofspectral type K0V in theconstellationCassiopeia. With anapparent magnitude of 5.63,[2] it is faintly visible to thenaked eye. The star is relatively close, 32.8light-years from 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 II and is much morex-ray luminous than the Sun. It is considered a relatively active star.[9] Based on an iron abundance of [Fe/H] = −0.02, themetallicity of this star appears to be similar to that of the Sun.[8]

References

[edit]
  1. ^abcdefVallenari, A.; et al. (Gaia collaboration) (2023)."Gaia Data Release 3. Summary of the content and survey properties".Astronomy and Astrophysics.674: A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID 244398875. Gaia DR3 record for this source atVizieR.
  2. ^abcMermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)",Catalogue of Eggen's UBV Data. SIMBAD,Bibcode:1986EgUBV........0M
  3. ^abWhite, 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,S2CID 122854
  4. ^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,S2CID 118577511
  5. ^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,S2CID 18993744. See Table 10.
  6. ^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,S2CID 14786643
  7. ^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,S2CID 18478960
  8. ^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
  9. ^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,CiteSeerX 10.1.1.43.4478,doi:10.1086/301488,S2CID 16930014
  10. ^"HR 511",SIMBAD,Centre de données astronomiques de Strasbourg, retrieved2016-07-09

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