50 Cassiopeiae is a white star in the northern constellationofCassiopeia. In the past, it had been misidentified as a suspected nebula, and given the number NGC 771.^[9] The star is visible to the naked eye, having an apparent visual magnitude of +3.95.^[2] Based upon an annual parallax shiftof20.76 mas, it is located 157 light years away. It is moving closer, having a heliocentric radial velocity of −18 km/s,^[4] and will approach to within 82 ly in 1.879 million years.^[2]

Alight curve for 50 Cassiopeiae, plotted from TESS data^[10]

It is an A-type main-sequence star with a stellar classification of A2 V.^[3] It is a suspected variable star with a very small amplitude.^[11] 50 Cas has an estimated 2.56 times the mass of the Sun,^[3] and about 2.5 times the Sun's radius.^[6] It is radiating 64 times the Sun's luminosity from its photosphere at an effective temperature of around 9,376 K.^[3]

The star was the brightest star in the occasionally used 1775 to 19th century constellation Custos Messium, typically drawn as a depiction of Charles Messier standing on top of the giraffe (Camelopardus), between Cepheus and Cassiopeia.^[12]

References[edit]

^ ^a ^b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data 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.

^ ^a ^b ^c ^d ^e Anderson, E.; Francis, C (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.

^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.

^ ^a ^b de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.

^ ^a ^b ^c 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. S2CID 18759600.

^ ^a ^b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy and Astrophysics, 367 (2): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.

^ Gáspár, András; et al. (August 2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 14, arXiv:1604.07403, Bibcode:2016ApJ...826..171G, doi:10.3847/0004-637X/826/2/171, S2CID 119241004, 171.

^ "50 Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-06-25.

^ Wolfgang Steinicke (19 August 2010). Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer's New General Catalogue. Cambridge University Press. ISBN 978-1-139-49010-8.

^ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 8 December 2021.