Astronomy:V1094 Tauri
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Short description: Eclipsing binary in the constellation Taurus
| Observation data {{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0 Equinox J2000.0 (ICRS)| Epoch J2000 [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}} | |
|---|---|
| Constellation | Taurus |
| A | |
| Right ascension | 04h 12m 03.59s[1] |
| Declination | +21° 56′ 50.6″[1] |
| Apparent magnitude (V) | 8.95 to 9.43[2] |
| B | |
| Right ascension | 04h 12m 05.10s[3] |
| Declination | +21° 56′ 49.7″[3] |
| Apparent magnitude (V) | 14.24[4] |
| Characteristics | |
| A | |
| Spectral type | G0 + G3[5] |
| Variable type | Algol[2] |
| Astrometry | |
| A | |
| Proper motion (μ) | RA: +89.201[1] mas/yr Dec.: −84.886[1] mas/yr |
| Parallax (π) | 8.2523 ± 0.0203[1] mas |
| Distance | 395.2 ± 1.0 ly (121.2 ± 0.3 pc) |
| B | |
| Radial velocity (Rv) | +5.67±2.98[3] km/s |
| Proper motion (μ) | RA: +88.757[3] mas/yr Dec.: −84.665[3] mas/yr |
| Parallax (π) | 8.2126 ± 0.0166[3] mas |
| Distance | 397.1 ± 0.8 ly (121.8 ± 0.2 pc) |
| Orbit[6] | |
| Primary | eclipsing primary |
| Companion | eclipsing secondary |
| Period (P) | 8.988 d |
| Semi-major axis (a) | 0.091—0.092 AU |
| Eccentricity (e) | 0.2697 |
| Inclination (i) | 90° |
| Semi-amplitude (K1) (primary) | 65.30 km/s |
| Semi-amplitude (K2) (secondary) | 70.98 km/s |
| Details[5] | |
| Eclipsing primary | |
| Mass | 1.0965±0.0040 M☉ |
| Radius | 1.4109±0.0058 R☉ |
| Temperature | 5,850±100 K |
| Metallicity | −0.09±0.11 dex |
| Age | ≈6 Gyr |
| Eclipsing secondary | |
| Mass | 1.0120±0.0028 M☉ |
| Radius | 1.1063±0.0066 R☉ |
| Temperature | 5,700±100 K |
| Metallicity | −0.09±0.11 dex |
| Age | ≈6 Gyr |
| B | |
| Mass | 0.616[7] M☉ |
| Radius | 0.636[7] R☉ |
| Luminosity | 0.088[7] L☉ |
| Surface gravity (log g) | 4.62[7] cgs |
| Temperature | 3,944[7] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
| B | |
V1094 Tauri is a system of at least three stars in the constellation of Taurus. Two stars are resolved 21″ apart; the brighter is an eclipsing binary.[8] In 2015, the parameters for the eclipsing pair were precisely measured.[5] Radial velocity data also revealed apsidal motion with a period of 14,500±3,700 years, which may indicate a third star.[9]
The star system was included in a 2003 study that featured GK Draconis and V1094 Tauri. The study suggested a mass of 1.10 M☉ for the primary star and a mass of 1.01 M☉ for the secondary.[6] The two stars orbit each other at a distance of around 0.091—0.092 AU and have an orbital period of around 9 days.
System structure
V1094 Tauri consists of three stars, a bright Algol-type eclipsing binary, and a faint companion farther out. It is an approximately 6 billion year old hierarchical triple star system around 400 light years away from Earth.
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)". Vizier Online Data Catalog. Bibcode: 2012yCat.1322....0Z.
- ↑ 5.0 5.1 5.2 Maxted, P. F. L.; Hutcheon, R. J.; Torres, G.; Lacy, C. H. S.; Southworth, J.; Smalley, B.; Pavlovski, K.; Marschall, L. A. et al. (2015). "Precise mass and radius measurements for the components of the bright solar-type eclipsing binary star V1094 Tauri". Astronomy and Astrophysics 578: A25. doi:10.1051/0004-6361/201525873. Bibcode: 2015A&A...578A..25M.
- ↑ 6.0 6.1 Griffin, R. F.; Boffin, H. M. J. (2003). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 171: HD 152028 and HDE 284195 (GK Dra and V1094 Tau)". The Observatory 123: 203. Bibcode: 2003Obs...123..203G.
- ↑ 7.0 7.1 7.2 7.3 7.4 Stassun, Keivan G. et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. Bibcode: 2019AJ....158..138S.
- ↑ "DEBCat: John Southworth's catalogue of well-studied detached eclipsing binaries". https://www.astro.keele.ac.uk/jkt/debcat/.
- ↑ Wolf, M.; Claret, A.; Kotková, L.; Kučáková, H.; Kocián, R.; Brát, L.; Svoboda, P.; Šmelcer, L. (2010). "Relativistic apsidal motion in eccentric eclipsing binaries". Astronomy and Astrophysics 509: A18. doi:10.1051/0004-6361/200911671. Bibcode: 2010A&A...509A..18W.
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