 Light curves for V773 Tauri. The upper panel shows the variability as seen by TESS.[1] The lower panel, adapted from Kenworthy et al.,[2] shows the eclipse seen in 2010. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 14m 12.926s[3] |
| Declination | 28° 12′ 12.36″[3] |
| Apparent magnitude (V) | 10.59 to 10.95[4] |
| Characteristics | |
| Spectral type | K3Ve (Li)[5] |
| Variable type | Orion variable + BY Dra[4] |
| Astrometry | |
| Proper motion (μ) | RA: 6.540 mas/yr[3] Dec.: −27.792 mas/yr[3] |
| Parallax (π) | 8.3261 ± 0.1313 mas |
| Distance | 433.1 ± 7.5 ly (132.8±2.3 pc)[6] |
| Orbit[2] | |
| Primary | V773 Tau AB |
| Companion | V773 Tau C |
| Period (P) | 624+83 −52 yr |
| Semi-major axis (a) | 1,013+93 −74 mas |
| Eccentricity (e) | 0.40+0.04 −0.05 |
| Inclination (i) | 97.3±0.6° |
| Longitude of the node (Ω) | 104.6±1.3° |
| Periastron epoch (T) | 1,740+26 −40 |
| Argument of periastron (ω) (secondary) | 107.8±4.5° |
| Orbit[2] | |
| Primary | V773 Tau A |
| Companion | V773 Tau B |
| Period (P) | 26.50±0.07 yr |
| Semi-major axis (a) | 117.7±0.86 mas |
| Eccentricity (e) | 0.104±0.009 |
| Inclination (i) | 69.25±0.40° |
| Longitude of the node (Ω) | 290.54±0.40° |
| Periastron epoch (T) | 2,010.11±0.12 |
| Argument of periastron (ω) (secondary) | 266.0±1.5° |
| Semi-amplitude (K1) (primary) | 6.50±0.50[7] km/s |
| Orbit[6] | |
| Primary | V773 Tau Aa |
| Companion | V773 Tau Ab |
| Period (P) | 51.1033±0.0018 d |
| Semi-major axis (a) | 2.809±0.033 mas |
| Eccentricity (e) | 0.2713±0.0066 |
| Inclination (i) | 68.5±1.6° |
| Longitude of the node (Ω) | 62.4±1.1° |
| Periastron epoch (T) | 53,059.75±0.28 MJD |
| Argument of periastron (ω) (secondary) | 5.6±2.2° |
| Semi-amplitude (K1) (primary) | 35.72±0.46 km/s |
| Semi-amplitude (K2) (secondary) | 42.9±1.3 km/s |
| Details | |
| Aa | |
| Mass | 1.55±0.11[6] M☉ |
| Radius | 2.22[8] R☉ |
| Luminosity | 2.56[8] L☉ |
| Surface gravity (log g) | 3.93[8] cgs |
| Temperature | 4,900[8] K |
| Age | 3±1[2] Myr |
| Ab | |
| Mass | 1.293±0.068[6] M☉ |
| Radius | 1.74[8] R☉ |
| Luminosity | 1.37[8] L☉ |
| Surface gravity (log g) | 4.08[8] cgs |
| Temperature | 4,740[8] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
V773 Tauri is a young, multiple star system in the central region[6] of Taurus, an equatorial constellation. This is a T Tauri-type variable star that ranges in apparent visual magnitude from 10.59 down to 10.95,[4] which is too faint to be viewed with the naked eye. Based on various estimates, the system is located at a distance of approximately 433 light years from the Sun. It lies near the dark cloud Lynds 1495.[6]
| Aa | |||||||||||||||
| Period = 51.1 d | |||||||||||||||
| Ab | |||||||||||||||
| Period = 26.5 yr | |||||||||||||||
| B(ab) | |||||||||||||||
| Period = 624 yr | |||||||||||||||
| C | |||||||||||||||
Hierarchy of orbits
This system was identified as a T Tauri star by A. E. Rydgren and associates in 1974.[10] Radio emission was detected from this source in 1983.[11] In 1993, it was discovered to be a double star with an angular separation of about 150 mas: the two components are designated A and B. Component A was found to be a double-lined spectroscopic binary with an orbital period of 51 days. In 2003 a third member of this group was located, component C,[6] at a separation of 256 mas from component A.
Orbital solutions for the A–B pair provide an unexpectedly high dynamic mass of 2.69±0.67 M☉ for component B, suggesting it too may be a binary system.[7] A single star with that much mass would have 17 times the luminosity of the Sun, which is inconsistent with the observed optical luminosity. Photometry of component B suggests it is experiencing extinction from dust along the line of sight. The component is variable in the K band, which is consistent with clumps or clouds of dust in orbit.[2]
In 2010, an extended eclipse was observed in the V773 Tauri system. This was interpreted as a circumbinary disk of component B passing in front of component A. The eclipse obscured 70% of the emission from component A and lasted 150 days.[2]
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