42 Cassiopeiae

42 Cassiopeiae is a possible binary star[9] system in the northern circumpolar constellation of Cassiopeia. It is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of +5.18. The system is located approximately 291 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +7 km/s.[2]

42 Cassiopeiae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cassiopeia
Right ascension 01h 42m 55.86184s[1]
Declination +70° 37′ 21.09002″[1]
Apparent magnitude (V) +5.18[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type B9 V[4]
B−V color index −0.022±0.002[2]
Variable type suspected β Per[5]
Astrometry
Radial velocity (Rv)+6.6±2.9[2] km/s
Proper motion (μ) RA: +76.763[1] mas/yr
Dec.: −13.955[1] mas/yr
Parallax (π)11.2028 ± 0.1432[1] mas
Distance291 ± 4 ly
(89 ± 1 pc)
Absolute magnitude (MV)0.53[2]
Details
Mass2.68±0.04[3] M☉
Radius2.63±0.13[6] R☉
Luminosity66.12[2] L☉
Surface gravity (log g)3.98±0.04[6] cgs
Temperature10,141±61[6] K
Rotational velocity (v sin i)149[3] km/s
Age67+188
−57[7] Myr
Other designations
42 Cas, NSV 590, BD+69°114, GC 2059, HD 10250, HIP 8016, HR 480, SAO 4470[8]
Database references
SIMBADdata

This is classified as a suspected eclipsing binary of the Algol type,[5] with a period of 16.77 days and a magnitude decrease of 0.3.[10] The primary is a B-type main-sequence star with a stellar classification of B9V.[4] It is roughly 67[7] million years old and is spinning with a projected rotational velocity of 149 km/s.[3] The star has 2.7[3] times the mass of the Sun and 2.6[6] times the Sun's radius. It is radiating 66[2] times the luminosity of the Sun from its photosphere at an effective temperature of 10,141 K.[6]

References
  1. 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.
  2. 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.
  3. Zorec, J.; Royer, F. (January 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.
  4. Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
  5. Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, GCVS 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S.
  6. 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.
  7. Gullikson, Kevin; et al. (January 2016), "Direct Spectral Detection: An Efficient Method to Detect and Characterize Binary Systems", The Astronomical Journal, 151 (1): 16, arXiv:1511.05148, Bibcode:2016AJ....151....3G, doi:10.3847/0004-6256/151/1/3, 3.
  8. "42 Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-22.
  9. 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.
  10. Hoffleit, Dorrit (1996), "A Catalogue of Correlations Between Eclipsing Binaries and Other Categories of Double Stars", The Journal of the American Association of Variable Star Observers, 24 (2): 105–116, Bibcode:1996JAVSO..24..105H.
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