Star in the constellation Cassiopeia
HR 511 (also designatedV987 Cassiopeiae andGliese 75 among others) is anorange dwarf ofspectral type K0V in theconstellation Cassiopeia . With anapparent magnitude of 5.63,[ 3] naked eye . The star is relatively close, 32.8light-years from theSun , just above 10parsecs .[ 2]
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.[ 10] metallicity of this star appears to be similar to that of the Sun.[ 9]
^ Anderson, E.; Francis, Ch. (May 2012), "XHIP: An extended hipparcos compilation",Astronomy Letters ,38 (5):331– 346,arXiv :1108.4971 Bibcode :2012AstL...38..331A ,doi :10.1134/S1063773712050015 ,eISSN 1562-6873 ,ISSN 1063-7737 ,S2CID 119257644 ^a b c d e f g Vallenari, 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record for this source atVizieR .^a b c Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)",Catalogue of Eggen's UBV Data. SIMBAD ,Bibcode :1986EgUBV........0M ^a b White, 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 ^ 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 ^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 ,S2CID 18993744 ^ 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 ^ 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 ^a b 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 ^a b c d 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 ,CiteSeerX 10.1.1.43.4478 doi :10.1086/301488 ,S2CID 16930014 ^ "HR 511" ,SIMBAD Centre de données astronomiques de Strasbourg , retrieved2016-07-09
