Eisspeedway

42 Camelopardalis

42 Camelopardalis
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Camelopardalis
Right ascension 06h 50m 57.08877s[1]
Declination +67° 34′ 18.9814″[1]
Apparent magnitude (V) 5.14[2]
Characteristics
Spectral type B4 IV[3] or B5 V[2]
B−V color index −0.152±0.002[2]
Astrometry
Radial velocity (Rv)3.2±1.2[4] km/s
Proper motion (μ) RA: +0.55[5] mas/yr
Dec.: +5.02[5] mas/yr
Parallax (π)4.2456 ± 0.2405 mas[1]
Distance770 ± 40 ly
(240 ± 10 pc)
Absolute magnitude (MV)−2.10[2]
Details
Mass6.5±0.2[6] M☉
Radius5.6[7] R☉
Luminosity (bolometric)2,460[8] L☉
Temperature16,550[8] K
Rotational velocity (v sin i)105[9] km/s
Age50.1±11.7[6] Myr
Other designations
42 Cam, BD+67°454, FK5 2523, GC 8902, HD 48879, HIP 32864, HR 2490, SAO 13973[10]
Database references
SIMBADdata

42 Camelopardalis is a single[11] star in the constellation Camelopardalis,[10] located roughly 770 light years away from the Sun.[1] It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.14.[2] The visual magnitude of the star is diminished by an extinction of 0.22 due to interstellar dust.[12] It is moving further from the Earth with a heliocentric radial velocity of 3 km/s.[4] 42 Camelopardalis has a peculiar velocity of 24.4+1.9
−2.1 km/s and may be a runaway star.[6]

Observations made in 1933 appeared to suggest this could be a Beta Cephei variable,[13] but this was not confirmed by follow-up measurements.[14] The star has a stellar classification of B4 IV,[3] matching a B-type subgiant star. It has 6.5[6] times the mass of the Sun and about 5.6[7] times the Sun's radius. 42 Camelopardalis is 50[6] million years old with a high rotation rate, showing a projected rotational velocity of 105 km/s.[9] It is radiating 2,460[8] times the luminosity of the Sun from its photosphere at an effective temperature of 16,550 K.[8] This star is notable as demonstrating similarities between the short-period B-type variables and the Cepheid variables.[citation needed]

References

  1. ^ a b c d 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. ^ a b c d e 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 Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement, 17: 371, Bibcode:1968ApJS...17..371L, doi:10.1086/190179
  4. ^ a b Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 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.
  5. ^ a b 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 c d e 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.
  7. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (Third ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  8. ^ a b c d Hohle, M. M.; et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
  9. ^ a b Strom, Stephen E.; et al. (2005), "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?", The Astronomical Journal, 129 (2): 809–828, arXiv:astro-ph/0410337, Bibcode:2005AJ....129..809S, doi:10.1086/426748, S2CID 15059129.
  10. ^ a b "42 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-21.
  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. ^ Gontcharov, G. A. (November 2012), "Spatial distribution and kinematics of OB stars", Astronomy Letters, 38 (11): 694–706, arXiv:1606.09028, Bibcode:2012AstL...38..694G, doi:10.1134/S1063773712110035, S2CID 119108982.
  13. ^ Edwards, D. L. (1933), "Variations in the Spectrum of 42 Camelopardalis", Monthly Notices of the Royal Astronomical Society, 93 (9): 729–735, Bibcode:1933MNRAS..93..729E, doi:10.1093/mnras/93.9.729.
  14. ^ Heard, John F. (March 1949), "An Analysis of Radial-Velocity Measures of Eight Stars Formerly Assigned to the Beta Cephei Group.", Astrophysical Journal, 109: 185, Bibcode:1949ApJ...109..185H, doi:10.1086/145122.
Quelle: https://en.wikipedia.org/wiki/42_Camelopardalis