FU Tauri is a brown dwarf binary system in the constellation of Taurus about 429 light years away. The secondary is very close to the lower limit for brown dwarfs and several databases list it as a distant massive exoplanet.
 FU Tauri and its companion (lower left) Credit: Image Credit: NASA/ESA/CSA JWST; Ya-Lin Wu et al.; processing: Meli_thev | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| A | |
| Right ascension | 04h 23m 35.3912s[1] |
| Declination | +25° 03′ 02.74″[1] |
| B | |
| Right ascension | 04h 23m 35.3912s[2] |
| Declination | +25° 03′ 02.74″[2] |
| Characteristics | |
| Spectral type | M7.25 + M9.25[3] |
| Apparent magnitude (G) | 15.2[1] + 20.5[2] |
| Variable type | T Tau[4] |
| Astrometry | |
| A | |
| Proper motion (μ) | RA: 6.895[1] mas/yr Dec.: −21.026[1] mas/yr |
| Parallax (π) | 7.5981 ± 0.1497 mas[1] |
| Distance | 429 ± 8 ly (132 ± 3 pc) |
| B | |
| Proper motion (μ) | RA: 12.450[2] mas/yr Dec.: −21.761[2] mas/yr |
| Parallax (π) | 7.4909 ± 1.2887 mas[2] |
| Distance | approx. 440 ly (approx. 130 pc) |
| Details | |
| A | |
| Mass | 0.05[5] M☉ |
| Radius | 1.8[5] R☉ |
| Luminosity | 0.2[3] L☉ |
| Temperature | 2,838[3] K |
| Age | ≤1[5] Myr |
| B | |
| Mass | 0.015[5] M☉ |
| Luminosity | 0.0039[3] L☉ |
| Temperature | 2,375[3] K |
| Age | 1[5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | A |
| B | |
System
editThe two stars of the FU Tauri system are separated by 5.7″, equivalent to 800 AU at the distance of FU Tauri.[6] The primary is a brown dwarf with a mass of 0.05 M☉, while the secondary has a mass of 0.015 M☉. The secondary mass of 15 MJ is close to the dividing line between brown dwarfs and exoplanets, and it is often treated as an exoplanet.[7]
Properties
editBoth members of the binary are low-mass objects still contracting towards the main sequence. Comparison with theoretical evolutionary tracks gives them ages of one Myr or less. However, the primary is more luminous than expected even for this age and it may be younger than the secondary.[5] The primary has a temperature of 2,838 K, a radius of 1.8 R☉, and a bolometric luminosity of 0.2 L☉. The secondary has a temperature of 2,375 K and a bolometric luminosity of 0.0039 L☉.[5]
Variability
edit
FU Tauri varies in brightness. The primary star is a T Tauri variable, a type of irregular pre-main-sequence star. Its brightness has been observed to vary from a photovisual magnitude of 16.0 to fainter than 17.0.[9] Its photographic magnitude has been measured to vary between magnitude 15.1 and below magnitude 17.6.[10]
References
edit- ^ a b c d e f 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.
- ^ a b c d e f 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.
- ^ a b c d e Luhman, K. L.; Mamajek, E. E.; Allen, P. R.; Muench, A. A.; Finkbeiner, D. P. (2009). "Discovery of a Wide Binary Brown Dwarf Born in Isolation". The Astrophysical Journal. 691 (2): 1265. arXiv:0902.0425. Bibcode:2009ApJ...691.1265L. doi:10.1088/0004-637X/691/2/1265.
- ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
- ^ a b c d e f g Stelzer, B.; Scholz, A.; Argiroffi, C.; Micela, G. (2010). "The enigmatic young brown dwarf binary FU Tau: Accretion and activity". Monthly Notices of the Royal Astronomical Society. 408 (2): 1095–1102. arXiv:1006.2717. Bibcode:2010MNRAS.408.1095S. doi:10.1111/j.1365-2966.2010.17182.x. S2CID 16358981.
- ^ Monin, J.-L.; Whelan, E. T.; Lefloch, B.; Dougados, C.; Alves De Oliveira, C. (2013). "A molecular outflow driven by the brown dwarf binary FU Tauri". Astronomy & Astrophysics. 551: L1. arXiv:1301.4387. Bibcode:2013A&A...551L...1M. doi:10.1051/0004-6361/201220973. S2CID 55550017.
- ^ "FU Tauri". Open Exoplanet Catalogue. Retrieved 2020-04-06.
- ^ Scholz, Alexander; Stelzer, Beate; Costigan, Grainne; Barrado, David; Eislöffel, Jochen; Lillo-Box, Jorge; Riviere-Marichalar, Pablo; Stoev, Hristo (January 2012). "Magnetic activity and accretion on FU Tau A: clues from variability". Monthly Notices of the Royal Astronomical Society. 419 (2): 1271–1279. arXiv:1109.3474. Bibcode:2012MNRAS.419.1271S. doi:10.1111/j.1365-2966.2011.19781.x.
- ^ Romano, G. (1975). "Observations of T Tau stars and related objects in Taurus dark cloud". Memorie della Societa Astronomica Italiana. 46: 81. Bibcode:1975MmSAI..46...81R.
- ^ Gotz, W. (1961). "Photographische Untersuchungen an RW Aurigae-Sternen in den Dunkelgebieten von Taurus und Orion". Veroeffentlichungen der Sternwarte Sonneberg. 5: 87. Bibcode:1961VeSon...5...87G.