4 Cassiopeiae

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4 Cassiopeiae

A light curve for 4 Cassiopeiae, plotted from Hipparcos data.[1] The assumed period is from Koen and Eyer (2002).[2]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cassiopeia
Right ascension 23h 24m 50.26237s[3]
Declination +62° 16′ 58.1094″[3]
Apparent magnitude (V) 4.96[4] (4.95 – 5.00)[5]
Characteristics
Evolutionary stage AGB[6]
Spectral type M2− IIIab[4]
B−V color index 1.676±0.010[4]
Variable type suspected[5]
Astrometry
Radial velocity (Rv)−38.99±0.23[7] km/s
Proper motion (μ) RA: +12.29[3] mas/yr
Dec.: −12.44[3] mas/yr
Parallax (π)4.15 ± 0.21 mas[3]
Distance790 ± 40 ly
(240 ± 10 pc)
Absolute magnitude (MV)−1.94[4]
Details
Mass2.3[8] M☉
Radius78[9] R☉
Luminosity1,419[9] L☉
Temperature4,000[9] K
Other designations
4 Cas, NSV 14549, BD+61°2444, FK5 882, HD 220652, HIP 115590, HR 8904, SAO 20614, WDS J23248+6217A[10]
Database references
SIMBADdata
Messier 52, with the bright star 4 Cassiopeiae on the right (north) edge of the image

4 Cassiopeiae is a red giant in the northern constellation of Cassiopeia,[10] located approximately 790 light-years away from the Sun.[3] It is visible to the naked eye as a faint, red-hued star with a baseline apparent visual magnitude of 4.96.[4] At the distance of this system, its visual magnitude is diminished by an extinction of 0.56 due to interstellar dust.[11] This system is moving closer to the Earth with a heliocentric radial velocity of −39 km/s.[7]

An evolved red giant star, currently on the asymptotic giant branch,[6] 4 Cassiopeiae has a stellar classification of M2− IIIab.[4] It is a suspected variable star of unknown type with a brightness that varies from visual magnitude 4.95 down to 5.00.[5]

Multiple star catalogues list a number of companions to 4 Cassiopeiae, all unrelated stars at different distances.[12] As of 2011, the magnitude 9.88 component B lay at an angular separation of 96.10″ along a position angle of 226° relative to the primary. Components C, E, F, and G are all fainter and more than two arc-minutes from 4 Cassiopeiae, and components C and G are themselves close doubles.[13]

4 Cassiopeiae is 40' north of the open cluster Messier 52, near the constellation border with Cepheus, although it is not a member of the cluster.[14]

References

  1. ^ "Light Curve", Hipparcos ESA, ESA, retrieved 3 October 2022.
  2. ^ Koen, Chris; Eyer, Laurent (March 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.
  3. ^ a b c d e f 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.
  4. ^ a b c d e f Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  5. ^ a b c Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017), "General catalogue of variable stars", Astronomy Reports, 5.1, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  6. ^ a b Eggen, O. J. (1992), "Asymptotic giant branch stars near the sun", The Astronomical Journal, 104: 275, Bibcode:1992AJ....104..275E, doi:10.1086/116239.
  7. ^ a b Famaey, B.; et al. (2009), "Spectroscopic binaries among Hipparcos M giants. I. Data, orbits, and intrinsic variations", Astronomy and Astrophysics, 498 (2): 627–640, arXiv:0901.0934, Bibcode:2009A&A...498..627F, doi:10.1051/0004-6361/200810698, S2CID 18739721.
  8. ^ Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (March 2019). "Stellar and substellar companions of nearby stars from Gaia DR2 - Binarity from proper motion anomaly". A&A. 623: 623. arXiv:1811.08902. Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371.
  9. ^ a b c 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. Gaia DR2 record for this source at VizieR.
  10. ^ a b "4 Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-13.
  11. ^ Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430 (1): 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304.
  12. ^ 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.
  13. ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
  14. ^ Baumgardt, H.; Dettbarn, C.; Wielen, R. (2000). "Absolute proper motions of open clusters. I. Observational data". Astronomy and Astrophysics Supplement Series. 146 (2): 251. arXiv:astro-ph/0010306. Bibcode:2000A&AS..146..251B. doi:10.1051/aas:2000362. S2CID 7180188.
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