La Superba

For the Italian city with that nickname, see Genoa.
La Superba

Location of Y Canum Venaticorum
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Canes Venatici
Right ascension 12h 45m 07.83s[1]
Declination +45° 26′ 24.92″[1]
Apparent magnitude (V) +4.86 to +7.32[2]
Astrometry
Radial velocity (Rv)15.30[3] km/s
Proper motion (μ) RA: -2.20[1] mas/yr
Dec.: 13.05[1] mas/yr
Parallax (π)3.12 ± 0.34[1] mas
Distanceapprox. 1,000 ly
(approx. 320 pc)
Characteristics
Spectral type C54J(N3)[4]
U−B color index 6.62[5]
B−V color index 2.54[5]
Variable type SRb[4]
Details
Mass3 (uncertain) [6] M☉
Radius390[7] R☉
Luminosity5,800[8] L☉
Temperature2,600-3,200[9] K
Other designations
La Superba,[10] Y Canum Venaticorum, HR 4846, HD 110914, BD+46°1817, FK5 1327, HIP 62223, SAO 44317, GC 17342, 152 Schjellerup[11]
Database references
SIMBADdata

La Superba (Y CVn, Y Canum Venaticorum) is a variable star in the constellation Canes Venatici, well known for its strikingly red appearance.

Y CVn and simulation from Celestia

Visibility

La Superba is a semiregular variable star, varying by about a magnitude over a roughly 160-day cycle, but with slower variation over a larger range. Periods of 194 and 186 days have been suggested, with a resonance between the periods.[9]

Y CVn is one of the reddest stars in the sky, and it is among the brightest of the giant red carbon stars. It is the brightest J-star in the sky, a very rare category of carbon stars that contain large amounts of carbon-13 (carbon atoms with 7 neutrons instead of the usual 6). The 19th century astronomer Angelo Secchi, impressed with its beauty, gave the star its common name.[10]

Properties

The angular diameter if La Superba has been measured at 13.81 mas.[12] It is expected to be pulsating but this has not been seen in the measurements. At 320pc, this corresponds to a radius of 2.2 astronomical units (473 R☉). If it were placed at the position of the Sun, the star's surface would extend beyond the orbit of Mars.

La Superba's temperature is believed to be about 2800 K, making it one of the coolest true stars known. It is faintly visible to the naked eye, and the red colour is very obvious in binoculars.[10] When infrared radiation is included, Y CVn has a luminosity several thousand times that of the Sun.

Outlook

After stars up to a few times the mass of the sun have finished fusing hydrogen to helium in their core, they start to burn hydrogen in a shell outside a degenerate helium core, and expand dramatically into the red giant state. Once the core reaches a high enough temperature, it ignites violently in the helium flash, which begins helium core burning on the horizontal branch. Once even the core helium is exhausted, a degenerate carbon-oxygen core remains. Fusion continues in both hydrogen and helium shells at different depths in the star, and the star increases luminosity on the asymptotic giant branch (AGB). L Superba is currently an AGB star.

On the AGB, fusion products are moved outwards from the core by strong deep convection known as a dredge-up, thus creating a carbon abundance in the outer atmosphere where carbon monoxide and other compounds are formed. These molecules tend to absorb radiation at shorter wavelengths, resulting in a remarkable spectrum with even less blue and violet compared to ordinary red giants, giving the star its distinguished red color.[13]

La Superba is most likely in the final stages of fusing its remaining secondary fuel (helium) into carbon and shedding its mass at the rate of about a million times that of the Sun's solar wind. It is also surrounded by a 2.5 light year-wide shell of previously ejected material, implying that at one point it must have been losing mass as much as 50 times faster than it is now. La Superba thus appears almost ready to eject its outer layers to form a planetary nebula, leaving behind its core in the form of a vanishing white dwarf.[14]

References

  1. 1 2 3 4 5 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. ↑ Samus, N. N.; Durlevich, O. V.; 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: 02025. Bibcode:2009yCat....102025S.
  3. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065.
  4. 1 2 Shenavrin, V. I.; Taranova, O. G.; Nadzhip, A. E. (2011). "Search for and study of hot circumstellar dust envelopes". Astronomy Reports. 55: 31. Bibcode:2011ARep...55...31S. doi:10.1134/S1063772911010070.
  5. 1 2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  6. ↑ Jim Kaler. "La Superba". Retrieved 2015-11-21.
  7. ↑ Luttermoser, Donald G.; Brown, Alexander (1992). "A VLA 3.6 centimeter survey of N-type carbon stars". Astrophysical Journal. 384: 634. Bibcode:1992ApJ...384..634L. doi:10.1086/170905.
  8. ↑ Ramstedt, S.; Olofsson, H. (2014). "The 12CO/13CO ratio in AGB stars of different chemical type. Connection to the 12C/13C ratio and the evolution along the AGB". Astronomy & Astrophysics. 566: A145. arXiv:1405.6404Freely accessible. Bibcode:2014A&A...566A.145R. doi:10.1051/0004-6361/201423721.
  9. 1 2 Neilson, Hilding R.; Ignace, Richard; Smith, Beverly J.; Henson, Gary; Adams, Alyssa M. (2014). "Evidence of a Mira-like tail and bow shock about the semi-regular variable V CVn from four decades of polarization measurements". Astronomy & Astrophysics. 568: A88. arXiv:1407.5644Freely accessible. Bibcode:2014A&A...568A..88N. doi:10.1051/0004-6361/201424037.
  10. 1 2 3 "50 Deep Sky Objects for 50mm Binoculars". Binocular Astronomy. Patrick Moore’s Practical Astronomy Series. 2007. p. 107. doi:10.1007/978-1-84628-788-6_9. ISBN 978-1-84628-308-6.
  11. ↑ McCarthy, M. F. (1994). "Angelo Secchi and the Discovery of Carbon Stars". The MK process at 50 years. A powerful tool for astrophysical insight Astronomical Society of the Pacific Conference Series. 60: 224. Bibcode:1994ASPC...60..224M.
  12. ↑ Quirrenbach, A.; Mozurkewich, D.; Hummel, C. A.; Buscher, D. F.; Armstrong, J. T. (1994). "Angular diameters of the carbon stars UU Aurigae, Y Canum Venaticorum, and TX PISCIUM from optical long-baseline interferometry". Astronomy and Astrophysics. 285: 541. Bibcode:1994A&A...285..541Q.
  13. ↑ Abia, C.; Dominguez, I.; Gallino, R.; Busso, M.; Masera, S.; Straniero, O.; De Laverny, P.; Plez, B.; Isern, J. (2002). "S‐Process Nucleosynthesis in Carbon Stars". The Astrophysical Journal. 579 (2): 817. arXiv:astro-ph/0207245Freely accessible. Bibcode:2002ApJ...579..817A. doi:10.1086/342924.
  14. ↑ Libert, Y.; Gérard, E.; Le Bertre, T. (2007). "The formation of a detached shell around the carbon star Y CVn". Monthly Notices of the Royal Astronomical Society. 380 (3): 1161. arXiv:0706.4211Freely accessible. Bibcode:2007MNRAS.380.1161L. doi:10.1111/j.1365-2966.2007.12154.x.

External links

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