HD 140283
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Libra[1] |
| Right ascension | 15h 43m 03.09712s[2] |
| Declination | −10° 56′ 00.5957″[2] |
| Apparent magnitude (V) | 7.205±0.02[1] |
| Characteristics | |
| Evolutionary stage | Halo subgiant[3] |
| Spectral type | G0IV-V m-5[4] |
| Astrometry | |
| Proper motion (μ) | RA: −1115.141[2] mas/yr Dec.: −303.573[2] mas/yr |
| Parallax (π) | 16.2672 ± 0.0260 mas[2] |
| Distance | 200.5 ± 0.3 ly (61.47 ± 0.10 pc) |
| Absolute magnitude (MV) | +3.377[1] |
| Details | |
| Mass | 0.81±0.05[5] M☉ |
| Radius | 2.167±0.041[6] R☉ |
| Luminosity | 4.766±0.055[6] L☉ |
| Surface gravity (log g) | 3.653±0.024[6] cgs |
| Temperature | 5,787±48[7] K |
| Metallicity [Fe/H] | −2.29±0.10[6] dex |
| Rotational velocity (v sin i) | ≤ 3.9[3] km/s |
| Age | 12±0.05[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
HD 140283 (also known as the Methuselah star) is a metal-poor subgiant star about 200 light years away from the Earth in the constellation Libra, near the boundary with Ophiuchus in the Milky Way Galaxy. Its apparent magnitude is 7.205, so it can be seen with binoculars. It is one of the oldest stars known.
HD 140283's light is somewhat blueshifted as it is moving toward rather than away from the Earth and it has been known to astronomers for over a century as a high-velocity star based on its proper motion. An early spectroscopic analysis by Joseph W. Chamberlain and Lawrence Aller revealed it to have a substantially lower metal content than the Sun.[9] Modern spectroscopic analyses find an iron content about a factor of 250 lower than that of the Sun. It is one of the closest metal-poor (population II) stars to Earth.
The star was already known by 1912 when W. S. Adams measured its astrometry using a spectrograph in the Mount Wilson Observatory.[10]
Age and significance
[edit]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 apparent 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 its age. Because of their relative scarcity, this is even rarer for a population II star such as HD 140283. A study published in 2013[11] used the Fine Guidance Sensors of NASA's Hubble Space Telescope to measure a precise parallax (and therefore distance and luminosity) for the star. This information was used 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 would possibly conflict with the calculated age of the Universe as determined by the final 2018 Planck satellite results of 13.787±0.020 billion years.[1][12] However, more recent models of its stellar evolution have suggested revision of the star's age to 13.7 billion years[13] or 12 billion years.[5]
Dubbed the "Methuselah Star" by the popular press due to its age,[14][15] the star must have formed soon after the Big Bang[1] and is one of the oldest stars known as of 2021.[5] The search for such very iron-poor stars has shown they are almost all anomalies in globular clusters and the Galactic Halo. This accords 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 put an upper limit on the date of the reionization (first star formation) phase of the Universe independently of theories and evidence of the first few million years after the Big Bang.[16] Most stars from population II and population III are no longer observable.
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 formed from existing materials in the second generation of stellar creation; their heavy-element content is believed to have come from zero-metal stars (population III stars), which have never been observed.[17] Those first stars are thought to have been formed from existing materials a few hundred million years after the Big Bang, and they died in explosions (supernovae) after only a few million years.[17] A second generation of stars, the generation in which HD 140283 is theorized to have been formed from existing materials, could not have coalesced until gas, heated from the supernova explosions of the earlier stars, cooled down.[17] 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.[17]
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 into supernovae). As with HD 122563, CS22892-0052, and CD−38 245, HD 140283 has an excess of oxygen and the alpha elements relative to iron.[1] 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, such as 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 thereby not yet having undergone the first dredge-up.[18]
See also
[edit]References
[edit]- ^ a b c d e f H. E. Bond; E. P. Nelan; D. A. VandenBerg; G. H. Schaefer; D. Harmer (2013). "HD 140283: A Star in the Solar Neighborhood that Formed Shortly After the Big Bang". The Astrophysical Journal Letters. 765 (1): L12. arXiv:1302.3180. Bibcode:2013ApJ...765L..12B. doi:10.1088/2041-8205/765/1/L12. S2CID 119247629.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b 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. S2CID 5920058.
- ^ Gray, R.O. (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.
- ^ a b c d Jiangling Tang; Meredith Joyce (2021). "Revised Best Estimates for the Age and Mass of the Methuselah Star HD 140283 Using MESA and Interferometry and Implications for 1D Convection". Research Notes of the AAS. 5 (5): 117. arXiv:2105.11311. Bibcode:2021RNAAS...5..117T. doi:10.3847/2515-5172/ac01ca. S2CID 235166094. 117.
- ^ a b c d Karovicova, I.; White, T. R.; Nordlander, T.; Casagrande, L.; Ireland, M.; Huber, D.; Jofré, P. (2020-08-01). "Fundamental stellar parameters of benchmark stars from CHARA interferometry - I. Metal-poor stars". Astronomy & Astrophysics. 640: A25. arXiv:2006.05411. Bibcode:2020A&A...640A..25K. doi:10.1051/0004-6361/202037590. ISSN 0004-6361.
- ^ 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. arXiv:1801.03274. Bibcode:2018MNRAS.475L..81K. doi:10.1093/mnrasl/sly010.
- ^ "HD 140283". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 3 September 2017.
- ^ 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.
- ^ Adams, W. S. (1912). "The three-prism stellar spectrograph of the Mount Wilson Solar Observatory". Astrophys. J. 35: 163–182. Bibcode:1912ApJ....35..163A. doi:10.1086/141924.
- ^ "Hubble finds birth certificate of oldest known star". Phys.Org. 2013-03-07. Retrieved 2013-03-07.
- ^ Planck Collaboration (2020). "Planck 2018 results. VI. Cosmological parameters (See PDF, page 15, Table 2)". Astronomy & Astrophysics. 641: A6. arXiv:1807.06209. Bibcode:2020A&A...641A...6P. doi:10.1051/0004-6361/201833910. S2CID 119335614.
- ^ 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. S2CID 18003446.
- ^ Crookes, David (16 October 2019). "How Can a Star Be Older Than the Universe? - Space Mysteries: If the universe is 13.8 billion years old, how can a star be more than 14 billion years old?". Space.com. Retrieved 18 October 2019.
- ^ "Hubble Finds 'Birth Certificate' of Oldest Known Star". Science Daily. 7 March 2013. Retrieved 11 August 2013.
- ^ D. Majaess (2013-02-23). "Nearby Ancient Star is Almost as Old as the Universe". Universe Today. Retrieved 2013-02-23.
- ^ a b c d R. Cowen (2013-01-10). "Nearby star is almost as old as the Universe". Nature. doi:10.1038/nature.2013.12196. S2CID 124435627.
- ^ F. Spite; M. Spite (1982). "Abundance of lithium in unevolved halo stars and old disk stars - Interpretation and consequences". Astronomy & Astrophysics. 115 (2): 357–366. Bibcode:1982A&A...115..357S.
