1 Cassiopeiae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cassiopeia
Right ascension 23h 06m 36.818s[1]
Declination +59° 25′ 11.14″[1]
Apparent magnitude (V) +4.84[2]
Characteristics
Spectral type B0.5 III[3]
U−B color index −0.87
B−V color index −0.060±0.004[2]
Astrometry
Radial velocity (Rv)−9.1±0.9[2] km/s
Proper motion (μ) RA: 6.94±0.14[1] mas/yr
Dec.: −1.95±0.14[1] mas/yr
Parallax (π)2.89 ± 0.13 mas[1]
Distance1,130 ± 50 ly
(350 ± 20 pc)
Absolute magnitude (MV)−2.91[2]
Details
Mass13.1[4] M☉
Radius10.2[5] R☉
Luminosity18,200[4] L☉
Surface gravity (log g)3.98[4] cgs
Temperature27,200[4] K
Metallicity [Fe/H]−0.40[6] dex
Rotational velocity (v sin i)31[7] km/s
Age5.7±0.1[8] Myr
Other designations
1 Cas, BD+58°2545, FK5 1201, HD 218376, HIP 114104, HR 8797, SAO 35147[9]
Database references
SIMBADdata

1 Cassiopeiae is a single[10] star in the northern constellation of Cassiopeia, located around 1,130 light years from the Sun.[1] It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of +4.84.[2] This object is moving closer to the Earth with a heliocentric radial velocity of −9 km/s.[2]

The stellar classification of 1 Cassiopeiae is B0.5 III,[3] matching an evolved B-type giant star. It is 5.7[8] million years old with a projected rotational velocity of 31.[7] The star has 13.1[4] times the mass of the Sun and 10.2[5] times the Sun's radius. It is radiating 18,200[4] times the Sun's luminosity from its photosphere at an effective temperature of 27,200 K.[4]

References

  1. ^ 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.Vizier catalog entry
  2. ^ 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
  3. ^ a b Zorec, J.; et al. (July 2009). "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ_1, D) parameters into Teff". Astronomy and Astrophysics. 501 (1): 297–320. arXiv:0903.5134. Bibcode:2009A&A...501..297Z. doi:10.1051/0004-6361/200811147. S2CID 14969137.
  4. ^ a b c d e f g Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal, 129 (3): 1642–1662, arXiv:astro-ph/0412542, Bibcode:2005AJ....129.1642F, doi:10.1086/427855, S2CID 119512018
  5. ^ a b Underhill, A. B.; et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars", Monthly Notices of the Royal Astronomical Society, 189 (3): 601–605, Bibcode:1979MNRAS.189..601U, doi:10.1093/mnras/189.3.601
  6. ^ Gies, Douglas R.; Lambert, David L. (March 1992). "Carbon, nitrogen, and oxygen abundances in early B-type stars". Astrophysical Journal, Part 1. 387: 673–700. Bibcode:1992ApJ...387..673G. doi:10.1086/171116.
  7. ^ a b Simón-Díaz, S.; et al. (January 2017). "The IACOB project . III. New observational clues to understand macroturbulent broadening in massive O- and B-type stars". Astronomy & Astrophysics. 597: 17. arXiv:1608.05508. Bibcode:2017A&A...597A..22S. doi:10.1051/0004-6361/201628541. S2CID 3478126. A22.
  8. ^ a b Tetzlaff, N.; et al. (January 2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv:1007.4883. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID 118629873.
  9. ^ "1 Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-03.
  10. ^ 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.
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