Back T الثور Arabic T Tauri AST T del Taure Catalan T Tauri Czech T Tauri German T Tauri Spanish T Tauri Basque تی گاو Persian T Tauri French T Tauri Hungarian
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 The star T Tauri with NGC 1555 cloud nearby. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 21m 59.43445s[1] |
| Declination | +19° 32′ 06.4182″[1] |
| Apparent magnitude (V) | 10.27[2] |
| Characteristics | |
| Spectral type | G5V:e |
| U−B color index | +0.80[2] |
| B−V color index | +1.22[2] |
| Variable type | T Tauri |
| Astrometry | |
| Radial velocity (Rv) | +24.6[3] km/s |
| Proper motion (μ) | RA: +15.51[1] mas/yr Dec.: -13.67[1] mas/yr |
| Parallax (π) | 6.9290 ± 0.0583 mas[4] |
| Distance | 471 ± 4 ly (144 ± 1 pc) |
| Orbit[5] | |
| Primary | T Tau N |
| Companion | T Tau S |
| Period (P) | 4200+5000 −3400 yr |
| Semi-major axis (a) | 2.9+5.4 −1.7″ |
| Eccentricity (e) | 0.7+0.2 −0.4 |
| Inclination (i) | 52+4 −5° |
| Longitude of the node (Ω) | 156 ± 11° |
| Periastron epoch (T) | B 1967+25 −47 |
| Argument of periastron (ω) (secondary) | 48+34 −25° |
| Orbit[5] | |
| Primary | T Tau Sa |
| Companion | T Tau Sb |
| Period (P) | 27 ± 2 yr |
| Semi-major axis (a) | 85+4 −2 mas |
| Eccentricity (e) | 0.56+0.07 −0.09 |
| Inclination (i) | 20+10 −6° |
| Longitude of the node (Ω) | 92+26 −36° |
| Periastron epoch (T) | JD 2450131+208 −288 (1996 Feb 17) |
| Argument of periastron (ω) (secondary) | 48+34 −25° |
| Details | |
| T Tau Sa | |
| Mass | 2.12 ± 0.10[5] M☉ |
| Age | 0.4[6] Myr |
| T Tau Sb | |
| Mass | 0.53 ± 0.06[5] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
T Tauri is a variable star in the constellation Taurus, the prototype of the T Tauri stars. It was discovered in October 1852 by John Russell Hind. T Tauri appears from Earth amongst the Hyades cluster, not far from ε Tauri, but it is actually 420 light-years behind it and not a member of the cluster. The cloud to the west of the system is NGC 1555, known more commonly as Hind's Variable Nebula.
Although this system is considered to be the prototype of T Tauri stars, a later phase in a protostar's formation, it is a very atypical T Tauri star.[7]
- ^ a b c d Cite error: The named reference
aaa474_2_653was invoked but never defined (see the help page). - ^ a b c Cite error: The named reference
aass34_1was invoked but never defined (see the help page). - ^ Cite error: The named reference
gcsrvwas invoked but never defined (see the help page). - ^ 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.
- ^ a b c d Köhler, R.; Kasper, M.; Herbst, T. M.; Ratzka, T.; Bertrang, G. H.-M. (2016). "Orbits in the T Tauri triple system observed with SPHERE". Astronomy & Astrophysics. 587: A35. arXiv:1512.05736. Bibcode:2016A&A...587A..35K. doi:10.1051/0004-6361/201527125. S2CID 53053114.
- ^ Cite error: The named reference
mnras410_1_190was invoked but never defined (see the help page). - ^ Flores, C.; Reipurth, B.; Connelley, M. S. (2020). "Is T Tauri North a "Classical" T Tauri Star?". The Astrophysical Journal. 898 (2): 109. arXiv:2006.10139. Bibcode:2020ApJ...898..109F. doi:10.3847/1538-4357/ab9e67. S2CID 219792821.
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