Astronomy:VFTS 352
280px Artist's rendering of VFTS 352 binary star Credit: ESO/L. Calçada | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Dorado |
| Right ascension | 05h 38m 28.456s[1] |
| Declination | −69° 11′ 19.18″[1] |
| Apparent magnitude (V) | 14.38[2] |
| Characteristics | |
| Evolutionary stage | Main sequence + main sequence[3] |
| Spectral type | O4.5 V(n)((fc)):z: + O5.5 V(n)((fc)):z:[4] |
| B−V color index | −0.10[2] |
| Astrometry | |
| Radial velocity (Rv) | 262.8[5] km/s |
| Distance | 164,000 ly (50,000[5] pc) |
| Orbit[5] | |
| Primary | VFTS 3521 |
| Companion | VFTS 3522 |
| Period (P) | 1.124 days |
| Semi-major axis (a) | 17.55 R☉ |
| Eccentricity (e) | 0 |
| Inclination (i) | 55.60° |
| Semi-amplitude (K1) (primary) | 324.9 km/s |
| Semi-amplitude (K2) (secondary) | 315.6 km/s |
| Details[5] | |
| VFTS 3521 | |
| Mass | 28.63±0.30 M☉ |
| Radius | 7.22±0.02 R☉ |
| Luminosity | 180,000 L☉ |
| Surface gravity (log g) | 4.18±0.01 cgs |
| Temperature | 42,540±280 K |
| Age | 1 Myr |
| VFTS 3522 | |
| Mass | 28.85±0.30 M☉ |
| Radius | 7.25±0.02 R☉ |
| Luminosity | 150,000 L☉ |
| Surface gravity (log g) | 4.18±0.01 cgs |
| Temperature | 41,120±290 K |
| Age | 1 Myr |
| Other designations | |
VFTS 352, 2MASS J05382845-6911191, IRSF J05382846-6911192 | |
| Database references | |
| SIMBAD | data |
VFTS 352 is a contact binary star system about 160,000 light years away in the Tarantula Nebula, which is part of the Large Magellanic Cloud.[6] It is the most massive and earliest spectral type overcontact system known.[5]
The discovery of this O-type binary star system made use of the European Southern Observatory's Very Large Telescope,[7] and the description was published on 13 October 2015.[5] VFTS 352 is composed of two massive stars of almost equal size that orbit each other in less than 27 hours. Both are extremely hot and luminous and are so close that their atmospheres overlap.[7] The two stars are rotating at a rate equal to their orbital period; that is, they are tidally locked.[8]
Massive stars like the two components of VFTS 352 are the primary source of oxygen in the universe,[7] produced in their interiors via the CNO cycle and then released to the interstellar environment by a supernova explosion.[9]
The future of VFTS 352 is uncertain, and there are two possible scenarios. If the two stars merge, a very rapidly rotating star will be produced. If it keeps spinning rapidly it might end its life in a long-duration gamma-ray burst. In a second hypothetical scenario, the components would end their lives in supernova explosions, forming a close binary black hole system, hence a potential gravitational wave source through black hole–black hole merger.[5]
See also
- Contact binary (small Solar System body), two asteroids gravitating toward each other until they touch
References
- ↑ 1.0 1.1 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues 2246: II/246. Bibcode: 2003yCat.2246....0C. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246.
- ↑ 2.0 2.1 Evans, C. J.; Taylor, W. D.; Hénault-Brunet, V.; Sana, H.; De Koter, A. et al. (June 2011). "The VLT-FLAMES Tarantula Survey. I. Introduction and observational overview". Astronomy & Astrophysics 530: A108. doi:10.1051/0004-6361/201116782. Bibcode: 2011A&A...530A.108E.
- ↑ Abdul-Masih, Michael; Sana, Hugues; Sundqvist, Jon; Mahy, Laurent; Menon, Athira; Almeida, Leonardo A.; De Koter, Alex; De Mink, Selma E. et al. (2019). "Clues on the Origin and Evolution of Massive Contact Binaries: Atmosphere Analysis of VFTS 352". The Astrophysical Journal 880 (2): 115. doi:10.3847/1538-4357/ab24d4. Bibcode: 2019ApJ...880..115A.
- ↑ Walborn, N. R.; Sana, H.; Simón-Díaz, S.; Maíz Apellániz, J.; Taylor, W. D.; Evans, C. J.; Markova, N.; Lennon, D. J. et al. (2014). "The VLT-FLAMES Tarantula Survey. XIV. The O-type stellar content of 30 Doradus". Astronomy & Astrophysics 564: A40. doi:10.1051/0004-6361/201323082. Bibcode: 2014A&A...564A..40W.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 Almeida, L. A.; Sana, H.; Mink, S. E. de; Tramper, F.; Soszyński, I.; Langer, N.; Barbá, R. H.; Cantiello, M. et al. (2015). "Discovery of the Massive Overcontact Binary VFTS 352: Evidence for Enhanced Internal Mixing". The Astrophysical Journal 812 (2): 102. doi:10.1088/0004-637X/812/2/102. Bibcode: 2015ApJ...812..102A.
- ↑ "Final Kiss of Two Stars Heading for Catastrophe". EPB. 15 October 2015. http://www.eso.org/public/news/eso1540/.
- ↑ 7.0 7.1 7.2 "Final kiss of two stars heading for catastrophe". Astronomy Now. 21 October 2015. http://astronomynow.com/2015/10/21/final-kiss-of-two-stars-heading-for-catastrophe/.
- ↑ Abdul-Masih, Michael; Sana, Hugues; Hawcroft, Calum; Almeida, Leonardo A.; Brands, Sarah A.; De Mink, Selma E.; Justham, Stephen; Langer, Norbert et al. (2021). "Constraining the Overcontact Phase in Massive Binary Evolution I. Mixing in V382 Cyg, VFTS 352, and OGLE SMC-SC10 108086". Astronomy & Astrophysics 651: A96. doi:10.1051/0004-6361/202040195. Bibcode: 2021A&A...651A..96A.
- ↑ Stasińska, G.; Prantzos, N.; Meynet, G.; Simón-Díaz, S.; Chiappini, C.; Dessauges-Zavadsky, M.; Charbonnel, C.; Ludwig, H.-G. et al. (2012). "Oxygen in the Universe". Eas Publications Series 54. doi:10.1051/eas/1254002. Bibcode: 2012EAS....54.....S.
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