Astronomy:LS IV-14 116

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Short description: Subdwarf star in the constellation Aquarius
LS IV-14 116[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aquarius[2]
Right ascension  +20h 57m 38.875s[3]
Declination −14° 25′ 44.01″[3]
Apparent magnitude (V) +12.93[4]
Characteristics
Spectral type sdB0.5VIIHe18[5]
B−V color index −0.16[4]
Variable type sdBVr[6][7]
Astrometry
Proper motion (μ) RA: +7.409[3] mas/yr
Dec.: −128.265[3] mas/yr
Parallax (π)2.3406 ± 0.0543[3] mas
Distance1,390 ± 30 ly
(427 ± 10 pc)
Details
Mass0.38[8] M☉
Radius0.122[8] R☉
Luminosity21[8] L☉
Surface gravity (log g)5.94±0.04[9] cgs
Temperature34,950±250[9] K
Other designations
2MASS J20573887-1425437, UCAC4 378-169675, V366 Aquarii
Database references
SIMBADdata

LS IV-14 116 is a hot subdwarf located approximately 2,000 light years away on the border between the constellations Capricornus and Aquarius. It has a surface temperature of approximately 34,000 ± 500 kelvins.[10] Along with stars HE 2359-2844 and HE 1256-2738, LS IV-14 116 forms a new group of star called heavy metal subdwarfs. These are thought to be stars contracting to the extended horizontal branch after a helium flash and ejection of their atmospheres at the tip of the red giant branch.[11]

A light curve for V366 Aquarii, adapted from Jeffery (2011)[12]

Amir Ahmad and C. Simon Jeffery discovered that the star is a variable star, in 2004, and published their discovery in 2005. They detected two pulsation periods, 1950 and 2900 seconds.[13] The star's atmosphere contains 10,000 times more zirconium (per unit mass) than the Sun's; it also has between 1,000 and 10,000 times the amount of strontium, germanium and yttrium than the Sun. The heavy metals are believed to be in cloud layers in the atmosphere where the ions of each metal have a particular opacity that allows radiational levitation to balance gravitational settling.[10]

References

  1. ↑ Nassau, J. J.; Stephenson, C. B. (1963). "Luminous Stars in the Northern Milky Way". Hamburger Sternw 04. Bibcode: 1963LS....C04....0N. 
  2. ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific 99 (617): 695. doi:10.1086/132034. Bibcode: 1987PASP...99..695R  Constellation record for this object at VizieR.
  3. ↑ 3.0 3.1 3.2 3.3 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.
  4. ↑ 4.0 4.1 Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)". VizieR On-line Data Catalog: I/322A. Originally Published in: 2012yCat.1322....0Z; 2013AJ....145...44Z 1322. Bibcode: 2012yCat.1322....0Z. 
  5. ↑ Drilling, J. S.; Jeffery, C. S.; Heber, U.; Moehler, S.; Napiwotzki, R. (2013). "An MK-like system of spectral classification for hot subdwarfs". Astronomy & Astrophysics 551: A31. doi:10.1051/0004-6361/201219433. Bibcode: 2013A&A...551A..31D. 
  6. ↑ Randall, S. K.; Bagnulo, S.; Ziegerer, E.; Geier, S.; Fontaine, G. (2015). "The enigmatic He-sdB pulsator LS IV-14°116: New insights from the VLT". Astronomy & Astrophysics 576: A65. doi:10.1051/0004-6361/201425251. Bibcode: 2015A&A...576A..65R. 
  7. ↑ Ahmad, A.; Jeffery, C. S. (2005). "Discovery of pulsation in a helium-rich subdwarf B star". Astronomy and Astrophysics 437 (3): L51. doi:10.1051/0004-6361:200500136. Bibcode: 2005A&A...437L..51A. 
  8. ↑ 8.0 8.1 8.2 Dorsch, M.; Latour, M.; Heber, U.; Irrgang, A.; Charpinet, S.; Jeffery, C. S. (2020). "Heavy-metal enrichment of intermediate He-sdOB stars: The pulsators Feige 46 and LS IV-14°116 revisited". Astronomy and Astrophysics 643: A22. doi:10.1051/0004-6361/202038859. Bibcode: 2020A&A...643A..22D. 
  9. ↑ 9.0 9.1 Green, E. M.; Guvenen, B.; O'Malley, C. J.; O'Connell, C. J.; Baringer, B. P.; Villareal, A. S.; Carleton, T. M.; Fontaine, G. et al. (2011). "The Unusual Variable Hot B Subdwarf LS IV-14°116". The Astrophysical Journal 734 (1): 59. doi:10.1088/0004-637X/734/1/59. Bibcode: 2011ApJ...734...59G. 
  10. ↑ 10.0 10.1 Naslim, N.; Jeffery, C. S.; Behara, N. T.; Hibbert, A. (2011). "An extremely peculiar hot subdwarf with a 10 000-fold excess of zirconium, yttrium and strontium". Monthly Notices of the Royal Astronomical Society 412 (1): 363. doi:10.1111/j.1365-2966.2010.17909.x. Bibcode: 2011MNRAS.412..363N. 
  11. ↑ Miller Bertolami, M. M.; Córsico, A. H.; Althaus, L. G. (2011). "On the Challenging Variability of LS IV-14°116: Pulsational Instabilities Excited by the epsilon-Mechanism". The Astrophysical Journal Letters 741 (1): L3. doi:10.1088/2041-8205/741/1/L3. Bibcode: 2011ApJ...741L...3M. 
  12. ↑ Jeffery, C. Simon (January 2011). "Photometric Variability of the Chemically Peculiar Hot Subdwarf LS IV-14 d116". Information Bulletin on Variable Stars 5964. Bibcode: 2011IBVS.5964....1J. https://ibvs.konkoly.hu/pub/ibvs/5901/5964.pdf. Retrieved 25 December 2024. 
  13. ↑ Ahmad, A.; Jeffery, C. S. (July 2005). "Discovery of pulsation in a helium-rich subdwarf B star". Astronomy and Astrophysics 437 (3): L51-L54. doi:10.1051/0004-6361:200500136. Bibcode: 2005A&A...437L..51A. 



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