Jump to content

36 Lyncis

From Wikipedia, the free encyclopedia
36 Lyncis

A light curve for EI Lyncis, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Lynx
Right ascension 09h 13m 48.21318s[2]
Declination +43° 13′ 04.1940″[2]
Apparent magnitude (V) 5.30[3]
Characteristics
Spectral type B9IVpHgMn[4]
B−V color index −0.130±0.003[3]
Variable type SX Ari[5]
Astrometry
Radial velocity (Rv)21.3±1.7[3] km/s
Proper motion (μ) RA: –30.236[2] mas/yr
Dec.: −32.032[2] mas/yr
Parallax (π)5.2687 ± 0.1577 mas[2]
Distance620 ± 20 ly
(190 ± 6 pc)
Absolute magnitude (MV)−0.95[3]
Details
Mass4.2[2] M☉
Radius4.21[6] R☉
Luminosity505[2] L☉
Surface gravity (log g)3.65[7] cgs
Temperature13,700[7] K
Metallicity [Fe/H]+0.60[7] dex
Rotation3.83476±0.00004 d[8]
Rotational velocity (v sin i)49±1[8] km/s
Other designations
36 Lyn, EI Lyn, BD+43°1893, FK5 346, HD 79158, HIP 45290, HR 3652, SAO 42759[9]
Database references
SIMBADdata

36 Lyncis is a solitary[10] variable star located around 620 light years away from the Sun in the northern constellation of Lynx. It has the variable star designation of EI Lyncis, while 36 Lyncis is the Flamsteed designation. This object is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of 5.30.[3] It is moving further away from the Earth with a heliocentric radial velocity of 21 km/s.[3]

This is a magnetic, helium-weak Bp star[11][12] with a stellar classification of B9IVpHgMn,[4] although the spectral peculiarities have led to alternate classifications such as B8 IIImnp.[8] It is sometimes classified as a mercury-manganese star.[13] It is also an 'sn' star, displaying a spectrum with generally sharp lines for most elements in combination with broad, diffuse lines of helium.[14] 36 Lyncis has been classified as an SX Arietis variable[15] with an amplitude of 0.03 in visual magnitude and a rotationally-modulated period of 3.834 days.[5] The star is spinning with a projected rotational velocity of 49 km/s[8] and a rotation rate of 3.83476 days.[8] It has 4.21[6] times the Sun's radius and is radiating 505 times the luminosity of the Sun from its photosphere at an effective temperature of 13,700 K.[7]

References

[edit]
  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e f g 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 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.
  4. ^ a b Abt, Helmut A.; Morrell, Nidia I. (July 1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". The Astrophysical Journal Supplement Series. 99: 135. Bibcode:1995ApJS...99..135A. doi:10.1086/192182. ISSN 0067-0049.
  5. ^ a b 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.
  6. ^ a b Shulyak, D.; et al. (2014). "Interferometry of chemically peculiar stars: Theoretical predictions versus modern observing facilities". Monthly Notices of the Royal Astronomical Society. 443 (2): 1629. arXiv:1406.6093. Bibcode:2014MNRAS.443.1629S. doi:10.1093/mnras/stu1259. S2CID 96452769.
  7. ^ a b c d Ghazaryan, S.; et al. (November 2018). "New catalogue of chemically peculiar stars, and statistical analysis". Monthly Notices of the Royal Astronomical Society. 480 (3): 2953–2962. arXiv:1807.06902. Bibcode:2018MNRAS.480.2953G. doi:10.1093/mnras/sty1912. S2CID 119062018.
  8. ^ a b c d e Cowley, A. (November 1972). "Spectral classification of the bright B8 stars". Astronomical Journal. 77: 750–755. Bibcode:1972AJ.....77..750C. doi:10.1086/111348.
  9. ^ "36 Lyncis". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-06-06.
  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.
  11. ^ Oksala, M. E.; Silvester, J.; Kochukhov, O.; Neiner, C.; Wade, G. A.; MiMeS Collaboration (January 2018). "Mixed poloidal-toroidal magnetic configuration and surface abundance distributions of the Bp star 36 Lyn". Monthly Notices of the Royal Astronomical Society. 473 (3): 3367–3376. arXiv:1709.08361. Bibcode:2018MNRAS.473.3367O. doi:10.1093/mnras/stx2487. S2CID 4158836.
  12. ^ Adelman, Saul J. (May 2000). "UVBY photometry of the magnetic CP stars HD 36668, 36 Lyncis, HD 86592, and HR 8861". Astronomy and Astrophysics. 357: 548–552. Bibcode:2000A&A...357..548A.
  13. ^ Ghazaryan, S.; Alecian, G.; Hakobyan, A. A. (2018). "New catalogue of chemically peculiar stars, and statistical analysis". Monthly Notices of the Royal Astronomical Society. 480 (3): 2953–2962. arXiv:1807.06902. Bibcode:2018MNRAS.480.2953G. doi:10.1093/mnras/sty1912. S2CID 119062018.
  14. ^ Shore, Steven N.; et al. (September 1987). "The SN Stars: Magnetically Controlled Stellar Winds Among the Helium-Weak Stars". Astronomical Journal. 94: 737. Bibcode:1987AJ.....94..737S. doi:10.1086/114512.
  15. ^ Watson, Christopher (4 January 2010). "EI Lyncis". AAVSO Website. American Association of Variable Star Observers. Retrieved 21 October 2022.
Retrieved from "https://en.wikipedia.org/w/index.php?title=36_Lyncis&oldid=1235039112"