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Sneden's Star

From Wikipedia, the free encyclopedia
Star in the constellation Aquarius
Sneden's Star
Observation data
Epoch J2000      Equinox J2000
ConstellationAquarius[1]
Right ascension22h 17m 01.65585s[2]
Declination−16° 39′ 27.0519″[2]
Apparent magnitude (V)13.21[3]
Characteristics
Evolutionary stagegiant[4]
Spectral typeKIIvw[5]
B−Vcolor index0.78[4]
Astrometry
Radial velocity (Rv)+13.0[3] km/s
Proper motion (μ)RA: 12.321[2]mas/yr
Dec.: −6.493[2]mas/yr
Parallax (π)0.1868±0.0440 mas[2]
Distanceapprox. 17,000 ly
(approx. 5,000 pc)
Absolute magnitude (MV)−0.23[6]
Details
Mass1.13[7] M
Radius13.8[8] R
Luminosity158[9] L
Surface gravity (log g)1.15[3] cgs
Temperature4,690[3] K
Metallicity[Fe/H]−3.19[4] dex
Age14.2±3[10] Gyr
Other designations
BPS CS 22892-0052,HE 2214-1654[5]
Database references
SIMBADdata

BPS CS22892-0052 (Sneden's Star) is an oldpopulation IIstar located at a distance of 4.7kiloparsecs (15,000light-years) in theMilky Way'sgalactic halo. It belongs to a class of ultra-metal-poor stars (metallicity [Fe/H]=-3.1), specifically the very rare subclass ofneutron-capture (r-process) enhanced stars. It was discovered byTim C. Beers and collaborators with the CurtisSchmidt telescope at theCerro Tololo Inter-American Observatory inChile. Extended high-resolutionspectroscopic observations since around 1995 (withChris Sneden from theUniversity of Texas at Austin as the leading observer) allowed observers to determine the abundances of 53chemical elements in this star, as of December 2005 only second in number to the Sun.

Frombarium (Z=56) on, all elements show the pattern of the r-process contribution to theabundances of the elements in the Solar System. Comparing the observed abundances for astable element such aseuropium (Z=63) and the radioactive elementthorium (Z=90) to calculated abundances of an r-process in a type IIsupernova explosion (as from the universities atMainz andBasel groups ofKarl-Ludwig Kratz andFriedrich-Karl Thielemann) have allowed observers to determine the age of this star to be about 14 billion years. Similar ages have been derived for other ultra-metal-poor stars (CS31082-001,BD+17°3248 andHE 1523-0901) from thorium-to-uranium ratios.[citation needed]

References

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  1. ^Roman, Nancy G. (1987)."Identification of a constellation from a position".Publications of the Astronomical Society of the Pacific.99 (617): 695.Bibcode:1987PASP...99..695R.doi:10.1086/132034. Constellation record for this object atVizieR.
  2. ^abcdeBrown, 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 atVizieR.
  3. ^abcdRoederer, Ian U.; et al. (June 2014). "A Search for Stars of Very Low Metal Abundance. VI. Detailed Abundances of 313 Metal-poor Stars".The Astronomical Journal.147 (6): 57.arXiv:1403.6853.Bibcode:2014AJ....147..136R.doi:10.1088/0004-6256/147/6/136.S2CID 119249291. 136.
  4. ^abcNorris, John E.; et al. (October 1997). "Extremely Metal-poor Stars. IV. The Carbon-rich Objects".The Astrophysical Journal.488 (1):350–363.Bibcode:1997ApJ...488..350N.doi:10.1086/304695.S2CID 121307016.
  5. ^ab"BPS CS 22892-0052".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2021-03-29.
  6. ^Beers, Timothy C.; Preston, George W.; Shectman, Stephen A. (1992). "A Search for Stars of Very Low Metal Abundance. II".The Astronomical Journal.103: 1987.Bibcode:1992AJ....103.1987B.doi:10.1086/116207.S2CID 121564385.
  7. ^Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevic, G.; Monari, G.; Cantat-Gaudin, T. (2019-08-01)."Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18".Astronomy and Astrophysics.628: A94.arXiv:1904.11302.Bibcode:2019A&A...628A..94A.doi:10.1051/0004-6361/201935765.ISSN 0004-6361.
  8. ^Stassun, Keivan G.; Oelkers, Ryan J.; Paegert, Martin; Torres, Guillermo; Pepper, Joshua; De Lee, Nathan; Collins, Kevin; Latham, David W.; Muirhead, Philip S.; Chittidi, Jay; Rojas-Ayala, Bárbara (2019-10-01)."The Revised TESS Input Catalog and Candidate Target List".The Astronomical Journal.158 (4): 138.arXiv:1905.10694.Bibcode:2019AJ....158..138S.doi:10.3847/1538-3881/ab3467.hdl:1721.1/124721.ISSN 0004-6256.S2CID 166227927.
  9. ^Giribaldi, R. E.; Van Eck, S.; Merle, T.; Jorissen, A.; Krynski, P.; Planquart, L.; Valentini, M.; Chiappini, C.; Van Winckel, H. (2023). "TITANS metal-poor reference stars. II. Red giants and CEMP stars".Astronomy and Astrophysics.679: A110.arXiv:2308.10118.Bibcode:2023A&A...679A.110G.doi:10.1051/0004-6361/202347208.
  10. ^Sneden, Christopher; Cowan, John J.; Lawler, James E.; Ivans, Inese I.; Burles, Scott; Beers, Timothy C.; Primas, Francesca; Hill, Vanessa; Truran, James W.; Fuller, George M.; Pfeiffer, Bernd; Kratz, Karl-Ludwig (2003). "The Extremely Metal-poor, Neutron Capture-rich Star CS 22892-052: A Comprehensive Abundance Analysis".The Astrophysical Journal.591 (2): 936.arXiv:astro-ph/0303542.Bibcode:2003ApJ...591..936S.doi:10.1086/375491.

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