26 Camelopardalis

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26 Camelopardalis
Observation data
Epoch J2000      Equinox J2000
Constellation Camelopardalis
Right ascension 05h 46m 30.39025s[1]
Declination +56° 06′ 56.0726″[1]
Apparent magnitude (V) +5.93[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A4Vn[4]
B−V color index +0.164±0.004[2]
Astrometry
Radial velocity (Rv)+21.0±4.3[2] km/s
Proper motion (μ) RA: +19.337±0.133[1] mas/yr
Dec.: −58.838±0.134[1] mas/yr
Parallax (π)16.5077 ± 0.0696[1] mas
Distance197.6 ± 0.8 ly
(60.6 ± 0.3 pc)
Absolute magnitude (MV)2.01[2]
Details
Mass1.80±0.02[3] M☉
Luminosity12.88+0.75
−0.71[3] L☉
Surface gravity (log g)4.12[5] cgs
Temperature7,798±36[3] K
Metallicity [Fe/H]−0.08[6] dex
Rotational velocity (v sin i)249[3] km/s
Age345[5] Myr
Other designations
NSV 2615, BD+56°1058, GC 7191, HD 38091, HIP 27249, HR 1969, SAO 25362[7]
Database references
SIMBADdata

26 Camelopardalis is a single[8] star in the northern constellation of Camelopardalis, positioned next to the southern constellation boundary with Auriga. It is a suspected variable star[9] that is dimly visible to the naked eye with a peak apparent visual magnitude of +5.93.[2] This object is located at a distance of 197 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +21 km/s.[2]

This is a white-hued A-type main-sequence star with a stellar classification of A4Vn,[4] where the 'n' notation indicates "nebulous" absorption lines due to rapid rotation. It is an estimated 345[5] million years old and is spinning with a projected rotational velocity of 249 km/s.[3] The star has 1.80[3] times the mass of the Sun and is radiating 13 times the Sun's luminosity from its photosphere at an effective temperature of 7,798 K.[3]

References[]

  1. ^ a b c d e f 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 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 c d e f g h Zorec, J.; et al. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  4. ^ a b Cowley, A.; et al. (1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
  5. ^ a b c David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  6. ^ Netopil, Martin (August 2017), "Metallicity calibrations for dwarf stars and giants in the Geneva photometric system", Monthly Notices of the Royal Astronomical Society, 469 (3): 3042–3055, arXiv:1705.00883, Bibcode:2017MNRAS.469.3042N, doi:10.1093/mnras/stx1077, S2CID 119034918.
  7. ^ "HD 38091". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-10.
  8. ^ De Rosa, R. J.; Patience, J.; Wilson, P. A.; Schneider, A.; Wiktorowicz, S. J.; Vigan, A.; Marois, C.; Song, I.; MacIntosh, B.; Graham, J. R.; Doyon, R.; Bessell, M. S.; Thomas, S.; Lai, O. (2014), "The VAST Survey - III. The multiplicity of A-type stars within 75 pc", Monthly Notices of the Royal Astronomical Society, 437 (2): 1216, arXiv:1311.7141, Bibcode:2014MNRAS.437.1216D, doi:10.1093/mnras/stt1932, S2CID 88503488.
  9. ^ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
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