50 Cassiopeiae

In this article, we will explore 50 Cassiopeiae in depth and its impact on our daily lives. From its origin to its contemporary relevance, we will analyze how 50 Cassiopeiae has evolved over time and how it has affected different aspects of society. We will also examine the different perspectives and opinions related to 50 Cassiopeiae, as well as its role in the current context. Through this comprehensive analysis, we hope to provide a complete and rich insight into 50 Cassiopeiae, providing the reader with a deeper understanding of this topic.

50 Cassiopeiae

50 Cassiopeiae in optical light
Observation data
Epoch J2000      Equinox J2000
Constellation Cassiopeia[1]
Right ascension 02h 03m 26.10206s[2]
Declination +72° 25′ 16.6376″[2]
Apparent magnitude (V) +3.95[1]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A2 V[3]
B−V color index −0.002±0.007[1]
Astrometry
Radial velocity (Rv)−18.2±0.9[4] km/s
Proper motion (μ) RA: −43.57[5] mas/yr
Dec.: +22.30[5] mas/yr
Parallax (π)20.76±0.14 mas[5]
Distance157 ± 1 ly
(48.2 ± 0.3 pc)
Absolute magnitude (MV)0.54[1]
Details
Mass2.56±0.03[3] M☉
Radius2.5[6] R☉
Luminosity63.8+3.5
−6.4[3] L☉
Temperature9,376+240
−235[3] K
Metallicity +0.18±0.28[7] dex
Rotational velocity (v sin i)91[3] km/s
Other designations
50 Cas, BD+71°117, FK5 70, GC 2445, HD 12216, HIP 9598, HR 580, SAO 4560, NGC 771[8]
Database references
SIMBADdata

50 Cassiopeiae is a white star in the northern constellation of Cassiopeia. 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.[1] Based upon an annual parallax shift of 20.76 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.[1]

A light 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

  1. ^ a b c d e f 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.
  2. ^ 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.
  3. ^ 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.
  4. ^ 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.
  5. ^ 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.
  6. ^ 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.
  7. ^ 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.
  8. ^ "50 Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-06-25.
  9. ^ 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.
  10. ^ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 8 December 2021.
  11. ^ Koen, Chris; Eyer, Laurent (2002). "New periodic variables from the Hipparcos epoch photometry". Monthly Notices of the Royal Astronomical Society. 331 (1): 45–59. arXiv:astro-ph/0112194. Bibcode:2002MNRAS.331...45K. doi:10.1046/j.1365-8711.2002.05150.x. S2CID 10505995.
  12. ^ Ian Ridpath's Star Tales - Custos Messium