Astronomy:Y Lyncis

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Short description: Variable star in the constellation Lynx
Y Lyncis
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A visual band light curve for Y Lyncis, adapted from Percy et al. (2001).[1] The top panel shows the brightness variation over a period of several years, and the lower panel shows shorter time scale variations.
Observation data
Equinox J2000.0]] (ICRS)
Constellation Lynx
Right ascension  07h 28m 11.61657s[2]
Declination +45° 59′ 26.2295″[2]
Apparent magnitude (V) 6.2 - 8.9[3]
Characteristics
Evolutionary stage AGB[4]
Spectral type M6S Ib[5]
Variable type SRc[5]
Astrometry
Radial velocity (Rv)5.50±0.6[6] km/s
Proper motion (μ) RA: −1.278[2] mas/yr
Dec.: −4.067[2] mas/yr
Parallax (π)2.8068 ± 0.1138[2] mas
Distance1,160 ± 50 ly
(360 ± 10 pc)
Details
Mass1.5 - 2.0[3] M☉
Radius580[3] R☉
Luminosity10,765[7] L☉
Surface gravity (log g)0.0[8] cgs
Temperature3,200[8] K
Metallicity [Fe/H]−0.19[8] dex
Other designations
Y Lyn, HD 58521, BD+46°1271, HIP 36288, SAO 41784
Database references
SIMBADdata

Y Lyncis is a semiregular variable star in the constellation Lynx. It is an asymptotic giant branch star of spectral type M6S, with a luminosity class of Ib, indicating a supergiant luminosity. It is around 1,160 light years away. Y Lyncis ranges in brightness from magnitude 6.2 to 8.9. When it is at its brightest, it very faintly visible to the naked eye under excellent observing conditions.

In 1901 it was announced that Williamina Fleming had discovered that the star, then known as BD +46°1271, is a variable star.[9] It was given its variable star designation, Y Lyncis, in 1912.[10] The changes in brightness of this star are complex, with at least two different periods showing. The General Catalogue of Variable Stars lists a period of 110 days.[11] More recent studies show a primary pulsation period of 133 days, with and a long secondary period with an amplitude of 0.2 magnitudes and duration 1,300 days. The long secondary period variations are possibly caused by long-lived convection cells.[12]

Y Lyncis has a mass around 1.5-2.0 M☉ and a luminosity around 10,000 L☉. It is a thermally pulsing asymptotic giant branch star, an evolved star with a carbon-oxygen core that is fusing helium in a shell and hydrogen in a separate shell.[4] It is also an S-type star, where third dredge-ups have brought some carbon to the surface, but not enough to create a carbon star.[7]

References

  1. ↑ Percy, John R.; Wilson, Joseph B..; Henry, Gregory W. (August 2001). "Long-Term VRI Photometry of Small-Amplitude Red Variables. I. Light Curves and Periods". Publications of the Astronomical Society of the Pacific 113 (786): 983–996. doi:10.1086/322153. Bibcode: 2001PASP..113..983P. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 Szatmary, Karoly; Vinko, Jozsef (1992). "Periodicities of the light curve of the semiregular variable star Y Lyncis". Monthly Notices of the Royal Astronomical Society 256 (2): 321–28. doi:10.1093/mnras/256.2.321. Bibcode: 1992MNRAS.256..321S. 
  4. ↑ 4.0 4.1 Guandalini, R.; Busso, M. (2008). "Infrared photometry and evolution of mass-losing AGB stars". Astronomy and Astrophysics 488 (2): 675–684. doi:10.1051/0004-6361:200809932. Bibcode: 2008A&A...488..675G. 
  5. ↑ 5.0 5.1 Kiss, L. L.; Szabó, Gy. M.; Bedding, T. R. (2006). "Variability in red supergiant stars: Pulsations, long secondary periods and convection noise". Monthly Notices of the Royal Astronomical Society 372 (4): 1721–1734. doi:10.1111/j.1365-2966.2006.10973.x. Bibcode: 2006MNRAS.372.1721K. 
  6. ↑ Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G. 
  7. ↑ 7.0 7.1 Guandalini, R.; Busso, M. (2008). "Infrared photometry and evolution of mass-losing AGB stars. II. Luminosity and colors of MS and S stars". Astronomy and Astrophysics 488 (2): 675–684. doi:10.1051/0004-6361:200809932. Bibcode: 2008A&A...488..675G. 
  8. ↑ 8.0 8.1 8.2 Soubiran, Caroline; Le Campion, Jean-François; Brouillet, Nathalie; Chemin, Laurent (2016). "The PASTEL catalogue: 2016 version". Astronomy & Astrophysics 591: A118. doi:10.1051/0004-6361/201628497. Bibcode: 2016A&A...591A.118S. 
  9. ↑ Pickering, E. C.; Colson, H. R.; Fleming, W. P.; Wells, L. D. (April 1901). "Sixty-four new variable stars". Astrophysical Journal 13: 226–230. doi:10.1086/140808. Bibcode: 1901ApJ....13..226P. 
  10. ↑ Dunér; Hartwig; Müller (June 1912). "Benennung von neu entdeckten veränderlichen Sternen". Astronomische Nachrichten 191 (19): 341–358. doi:10.1002/asna.19121911902. Bibcode: 1912AN....191..341.. 
  11. ↑ Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1. Bibcode: 2009yCat....102025S. 
  12. ↑ Percy, John R.; Sato, Hiromitsu (2009). "Long Secondary Periods in Pulsating Red Supergiant Stars". Journal of the Royal Astronomical Society of Canada 103 (1): 11. Bibcode: 2009JRASC.103...11P. 



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