Psi Cassiopeiae

ψ Cassiopeiae
Location of ψ Cassiopeiae (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Cassiopeia[1]
Right ascension 01h 25m 56.023s[2]
Declination +68° 07′ 48.05″[2]
Apparent magnitude (V) +4.72[3]
Characteristics
Evolutionary stage red clump[4]
Spectral type K0 III-IIIb CN0.5[5]
U−B color index +0.94
B−V color index +1.051[6]
Astrometry
Radial velocity (Rv)−12.7±0.3[3] km/s
Proper motion (μ) RA: 74.122 mas/yr[2]
Dec.: 26.310 mas/yr[2]
Parallax (π)16.2403±0.1061 mas[2]
Distance201 ± 1 ly
(61.6 ± 0.4 pc)
Absolute magnitude (MV)0.869[6]
Details
ψ Cas A
Mass2.5[7] M☉
Radius11[8] R☉
Luminosity44[8] L☉
Surface gravity (log g)2.74[9] cgs
Temperature4,442[8] K
Metallicity [Fe/H]−0.13[6] dex
Age5.2[6] Gyr
Other designations
ψ Cas, 36 Cas, BD+67°123, FK5 46, HD 8491, HIP 6692, HR 399, SAO 11751, ADS 1129, CCDM J01259+6808, WDS J01259+6808A[10]
Database references
SIMBADdata

Psi Cassiopeiae is a binary star[11] system in the northern constellation of Cassiopeia. Its name is a Bayer designation that is Latinized from ψ Cassiopeiae, and is abbreviated ψ Cas or Psi Cas. The pair have a combined apparent visual magnitude of +4.72,[3] which is bright enough to be visible to the naked eye. Based on an annual parallax of 16.24 mas,[2] it is located at a distance of approximately 201 light-years (62 pc). The system is drifting closer to the Sun with a line of sight velocity component of −13 km/s.[3]

The orange-hued primary component, ψ Cassiopeiae A, has an apparent magnitude of +5.0;[12][13] it is a double star, designated CCDM J01259+6808AB,[14] with a fourteenth magnitude star (component B) located 3 arcseconds from the primary. Located about 25 arcseconds distant there is a 9.8 magnitude optical companion CCDM J01259+6808CD, designated ψ Cassiopeiae B in older star catalogues,[12] which is itself another double;[12][15] CD comprises a 9.4 magnitude component C and a 10 magnitude component D.[16]

The primary has a stellar classification of K0 III-IIIb CN0.5,[5] which presents as an evolved K-type giant star. The suffix notation indicates a mild overabundance of the CN molecule. It is a red clump giant,[4] indicating it is on the horizontal branch of its evolutionary track. At an estimated age of 5.2 billion years,[6] it has 2.5[7] times the mass of the Sun and has expanded to 11 times the Sun's radius. It is radiating 44 times the luminosity of the Sun from its photosphere at an effective temperature of 4,442 K.[8]

References

  1. ^ 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. XHIP record for this object at VizieR.
  2. ^ a b c d e 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 at VizieR.
  3. ^ a b c d Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
  4. ^ a b Ting, Yuan-Sen; et al. (2018). "A Large and Pristine Sample of Standard Candles across the Milky Way: ∼100,000 Red Clump Stars with 3% Contamination". The Astrophysical Journal. 858 (1): L7. arXiv:1803.06650. Bibcode:2018ApJ...858L...7T. doi:10.3847/2041-8213/aabf8e.
  5. ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373. S2CID 123149047.
  6. ^ a b c d e Soubiran, C.; et al. (2008). "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants". Astronomy and Astrophysics. 480 (1): 91–101. arXiv:0712.1370. Bibcode:2008A&A...480...91S. doi:10.1051/0004-6361:20078788. S2CID 16602121.
  7. ^ a b Charbonnel, C.; et al. (2020). "Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era". Astronomy and Astrophysics. 633: A34. arXiv:1910.12732. Bibcode:2020A&A...633A..34C. doi:10.1051/0004-6361/201936360.
  8. ^ a b c d Hon, Marc; et al. (2021). "A "Quick Look" at All-sky Galactic Archeology with TESS: 158,000 Oscillating Red Giants from the MIT Quick-look Pipeline". The Astrophysical Journal. 919 (2): 131. arXiv:2108.01241. Bibcode:2021ApJ...919..131H. doi:10.3847/1538-4357/ac14b1.
  9. ^ Soubiran, C.; et al. (June 2010). "The PASTEL catalogue of stellar parameters". Astronomy and Astrophysics. 515: A111. arXiv:1004.1069. Bibcode:2010A&A...515A.111S. doi:10.1051/0004-6361/201014247. S2CID 118362423.
  10. ^ "psi Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-08-29.
  11. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
  12. ^ a b c Norton, Arthur Philip (1973). Star Atlas and Reference Handbook: (Epoch 1950.0). The Reference Handbook and Lists of Interesting Objects Rev. and Rewritten by Christopher R. Kitchin U.a. Sky Publishing Corporation. ISBN 978-0-85248-900-0. Retrieved 2025-05-22.
  13. ^ "Vizier". Retrieved 2009-04-13.
  14. ^ "* psi Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-04-13.
  15. ^ "BD+67 124". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-04-13.
  16. ^ "VizieR Detailed Page". Retrieved 2009-04-13.
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