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HE0107-5240 is an extremely metal-poor Population II star, located roughly 36000 light-years away from Earth, that has a mass of approximately 80% of the mass of the Sun. It is one of the most metal-poor stars known in our Galaxy, with a metallicity [Fe/H] = −5.2±0.2; i.e. it has just 1/160000 of the metal that the Sun has. Because of its very low metallicity, it is believed to be one of the earliest Population II stars to have formed. If so, then it is also very old, with an age of roughly 13 billion years. Because the star is not completely metal-free, it does not belong to the first generation of stars (the hypothetical Population III). These stars converted the pristine hydrogen, helium, and lithium formed by the Big Bang into heavier elements, such as carbon, oxygen, and metals.

HE0107-5240

The ultra-metal-poor star HE0107-5240
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Phoenix
Right ascension 01h 09m 29.1s[1]
Declination −52° 24′ 20″
Apparent magnitude (V) 15.86
Astrometry
Distance36000 ly
Details
Mass0.8[citation needed] M☉
Metallicity [Fe/H]−5.2[citation needed] dex
Other designations
HE 0107-5240, 2MASS J01092916-5224341.
Database references
SIMBADdata

The star is relatively small for a star of the early universe, which accounts for its old age: massive stars die quickly. To help explain why this star is so small, it is hypothesized it was once part of a binary star system.[2] [3]

HE0107-5240 was found by Norbert Christlieb and colleagues at the University of Hamburg in Germany as a byproduct of the Hamburg/ESO Survey for faint quasars with the 1m ESO Schmidt telescope. Follow-up observations were made at the Siding Spring 2.3 m Telescope and high-resolution spectra were taken at the European Southern Observatory in Chile, using one of the units of the Very Large Telescope. In 2005, a second star with an even smaller iron abundance, HE 1327-2326 ([Fe/H]=-5.4), was found, also in the Hamburg/ESO survey. In 2014 an even more metal poor star was announced: SMSS J031300.36−670839.3.[4]


See also


Ultra low metallicity / ultra metal poor stars

References


  1. A. Udalski, G. Pietrzynski, M. Szymanski, M. Kubiak, K. Zebrun, I. Soszynski, O. Szewczyk, and L. Wyrzykowski (June 2003). "The Optical Gravitational Lensing Experiment. Additional Planetary and Low-Luminosity Object Transits from the OGLE 2001 and 2002 Observational Campaigns". Acta Astronomica. 53: 133–149. arXiv:astro-ph/0306444. Bibcode:2003AcA....53..133U.{{cite journal}}: CS1 maint: uses authors parameter (link)
  2. Lau, Herbert H. B.; Stancliffe, Richard J.; Tout, Christopher A. (2007). "Carbon-rich extremely metal poor stars: signatures of Population III asymptotic giant branch stars in binary systems". MNRAS. 378 (2): 563–568. arXiv:astro-ph/0703685. Bibcode:2007MNRAS.378..563L. doi:10.1111/j.1365-2966.2007.11773.x. S2CID 14996538.{{cite journal}}: CS1 maint: uses authors parameter (link)
  3. Suda, Takuma; Aikawa, Masayuki; Machida, Masahiro N.; Fujimoto, Masayuki Y.; Iben, Icko, Jr. (2004). "Is HE 0107-5240 A Primordial Star? The Characteristics of Extremely Metal-Poor Carbon-Rich Stars". Astrophysical Journal. 611 (1): 476–493. arXiv:astro-ph/0402589. Bibcode:2004ApJ...611..476S. doi:10.1086/422135. S2CID 13040221.{{cite journal}}: CS1 maint: uses authors parameter (link)
  4. S. C. Keller, M. S. Bessell, A. Frebel, A. R. Casey, M. Asplund, H. R. Jacobson, K. Lind, J. E. Norris, D. Yong, A. Heger, Z. Magic, G. S. Da Costa, B. P. Schmidt, P. Tisserand (2014). "A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3". Nature. 506 (7489): 463–466. arXiv:1402.1517. Bibcode:2014Natur.506..463K. doi:10.1038/nature12990. ISSN 0028-0836. PMID 24509711. S2CID 4457295.{{cite journal}}: CS1 maint: uses authors parameter (link)



На других языках

[de] HE 0107-5240

HE 0107-5240 ist ein von der Erde etwa 36.000 Lichtjahre entfernter Stern im südlichen Teil des Sternbildes Phönix. Wegen seiner großen Entfernung zur Erde leuchtet der Stern ungefähr 10.000mal schwächer als die Sterne, die gerade noch mit bloßem Auge am Nachthimmel erkennbar sind. Sein Alter wird auf 12 bis 15 Milliarden Jahre geschätzt, er gilt damit als ein Stern der zweiten Generation – er soll ca. 1 Milliarde Jahre nach dem Urknall entstanden sein.
- [en] HE 0107-5240

[es] HE 0107-5240

HE 0107-5240 (2MASS J01092916-5224341) es una estrella en la constelación de Fénix de magnitud aparente +15,17.[1] Es una estrella muy alejada del Sistema Solar, estando situada a unos 36.000 años luz. Descubierta en 2002 durante un sondeo de la Universidad de Hamburgo/ESO,[2] es una de las estrellas conocidas con menor contenido metálico.


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