DSS image of HD 140283
Epoch J2000.0 Equinox J2000.0
|Right ascension||15h 43m 03.09706s|
|Declination||−10° 56′ 00.6036″|
|Apparent magnitude (V)||7.205 ± 0.02|
|Evolutionary stage||Halo Subgiant|
|Spectral type||G0IV-V m-5|
|Radial velocity (Rv)||−169.00 ± 0.2 km/s|
|Proper motion (μ)|| RA: −1114.93 mas/yr |
Dec.: −304.36 mas/yr
|Parallax (π)||16.114 ± 0.072 mas|
|Distance||202.4 ± 0.9 ly |
(62.1 ± 0.3 pc)
|Absolute magnitude (MV)||+3.377|
|Mass||0.780 or 0.805 M☉|
|Surface gravity (log g)||3.6 cgs|
|Metallicity [Fe/H]||±0.10−2.40 dex|
|Rotational velocity (v sin i)||≤ 3.9 km/s|
|Age||14.46 ± 0.8 (minimum 13.66) Gyr|
HD 140283, informally nicknamed the Methuselah star, is a metal-poor subgiant star about 200 light years away from the Earth in the constellation Libra, specifically toward Ophiuchus. Its apparent magnitude is 7.205. The star's light is somewhat blueshifted as it is moving more toward than away from us and it has been known to astronomers for over a century as a high-velocity star based on its other vectors (proper motion). An early spectroscopic analysis by Chamberlain and Aller revealed it to have a substantially lower metal content than the Sun. Modern spectroscopic analyses find an iron content about a factor of 250 lower than that of the Sun. It is one of the closest Population II stars to Earth.
Age and significance
Because HD 140283 is neither on the main sequence nor a red giant, its early position in the Hertzsprung-Russell diagram has been interpreted with its data and theoretical models of stellar evolution based on quantum mechanics and the observations of processes in millions of stars to infer its old age. For field stars (as opposed to stars in clusters) it is rare to know a star's luminosity, surface temperature and composition precisely enough to get a well-constrained value for their age; because of their relative scarcity, this is even rarer for a Population II star like HD 140283. A study published in 2013 used the Fine Guidance Sensors of NASA's Hubble Space Telescope to measure a precise parallax (and therefore distance and luminosity) for the star, and employ this information to estimate an age for the star of 14.46 ± 0.8 billion years. Due to the uncertainty in the value, this age for the star may or may not conflict with the calculated age of the Universe as determined by the final 2015 Planck Satellite results, 13.799 ± 0.021.
Once dubbed the "Methuselah Star" by the popular press due to its age, if the assumptions of stellar evolution are correct in the report, the star must have formed soon after the Big Bang and is one of the oldest stars known. The search for such very iron-poor stars has shown they are almost all anomalies in globular clusters and the Galactic Halo. This concords with a narrative that they are rare survivors of their generation. If so, the apparent visual data of the oldest of these enables us to longstop-date the reionization (first star formation) phase of the Universe independently of theories and evidence of first few million years after the Big Bang. Most stars from Population II and Population III are no longer observable. If it proves necessary theories exist which allow for an older age of the universe than conventionally accepted, which can still accommodate the observed redshift of early objects and earlier radiation. Some depart from the conventional big-bang/inflation model, such as the steady-state and cyclic models. To date no accurate, greater age evidence from a cosmic object has been found, to call into question the Planck Satellite results.
Studies of the star also help astronomers understand the Universe's early history. Very low but non-zero metallicities of stars like HD 140283 indicate the star was born in the second generation of stellar creation; their heavy-element content is believed to have come from truly zero-metal stars (Population III stars), which have never been seen. Those first stars are thought to have been born a few hundred million years after the Big Bang, and they died in explosions (supernovae) after only a few million years. A second generation of stars, the generation in which HD 140283 is theorized to have been born, could not have coalesced until gas, heated from the supernova explosions of the earlier stars, cooled down. This hypothesis of such stars' birth and our best models of the early universe indicate that the time it took for the gases to cool was likely only a few tens of millions of years.
The proportions of elements in such metal-poor stars is modelled to tell us much of the earlier nucleosynthetic ("metals") yield, that is of elements other than hydrogen and helium from the supernovae of the locally-extinct Population III stars. Some of the latter may be visible in gravitational lensing in looking at deepest images such as the Hubble Ultra-Deep Field (i.e. their brief existence before their turning supernova). Like HD 122563, CS22892-0052, and CD -38 245, HD 140283 has an excesses of oxygen and the alpha elements relative to iron. While the proportions of these elements is much lower in HD 140283 than in the Sun, they are not as low as is the case for iron. The implication is that the first population of stars generated the alpha elements preferentially to other groups of elements, including the iron peak and s-process. Unlike those other metal-poor stars, HD 140283 has a detectable amount of lithium, a consequence of HD 140283 having not yet evolved into a red giant and thus has not yet undergone the first dredge-up.
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- R. O. Gray (1989). "The extension of the MK spectral classification system to the intermediate population II F type stars". Astronomical Journal. 98 (3): 1049–1062. Bibcode:1989AJ.....98.1049G. doi:10.1086/115195.
- "HD 140283". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 3 September 2017.
- Brown, 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 at VizieR.
- Creevey, O. L.; Thévenin, F.; Berio, P.; Heiter, U.; von Braun, K.; Mourard, D.; Bigot, L.; Boyajian, T. S.; Kervella, P.; Morel, P.; Pichon, B.; Chiavassa, A.; Nardetto, N.; Perraut, K.; Meilland, A.; Mc Alister, H. A.; Ten Brummelaar, T. A.; Farrington, C.; Sturmann, J.; Sturmann, L.; Turner, N. (2015). "Benchmark stars for Gaia Fundamental properties of the Population II star HD 140283 from interferometric, spectroscopic, and photometric data". Astronomy and Astrophysics. 575: A26. arXiv:1410.4780. Bibcode:2015A&A...575A..26C. doi:10.1051/0004-6361/201424310.
- Karovicova, I.; White, T. R.; Nordlander, T.; Lind, K.; Casagrande, L.; Ireland, M. J.; Huber, D.; Creevey, O.; Mourard, D.; Schaefer, G. H.; Gilmore, G.; Chiavassa, A.; Wittkowski, M.; Jofré, P.; Heiter, U.; Thévenin, F.; Asplund, M. (2018). "Accurate effective temperatures of the metal-poor benchmark stars HD 140283, HD 122563, and HD 103095 from CHARA interferometry". Monthly Notices of the Royal Astronomical Society. 475 (1): L81. Bibcode:2018MNRAS.475L..81K. doi:10.1093/mnrasl/sly010.
- A. J. Gallagher; et al. (2010). "The barium isotopic mixture for the metal-poor subgiant star HD 140283". Astronomy and Astrophysics. 523: A24. arXiv:1008.3541. Bibcode:2010A&A...523A..24G. doi:10.1051/0004-6361/201014970.
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- J. W. Chamberlain; L. H. Aller (1951). "The Atmospheres of A-Type Subdwarfs and 95 Leonis". Astrophysical Journal. 114: 52. Bibcode:1951ApJ...114...52C. doi:10.1086/145451.
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