V773 Tauri

Last updated
V773 Tauri
V773TauLightCurve.png
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]
PrimaryV773 Tau AB
CompanionV773 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]
PrimaryV773 Tau A
CompanionV773 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]
PrimaryV773 Tau Aa
CompanionV773 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☉
Luminosity1.37 [8]   L☉
Surface gravity (log g)4.08 [8]   cgs
Temperature 4,740 [8]   K
Other designations
V773 Tau, HD 283447, HIP 19762, WDS J04142+2813A [9]
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]

References

  1. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 8 December 2021.
  2. 1 2 3 4 5 6 Kenworthy, M. A.; et al. (October 2022), "Eclipse of the V773 Tau B circumbinary disc", Astronomy & Astrophysics, 666: A61, arXiv: 2207.05575 , Bibcode:2022A&A...666A..61K, doi:10.1051/0004-6361/202243441, S2CID   250451004, A61.
  3. 1 2 3 4 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  4. 1 2 3 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports , 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  5. ↑ Herbig, G. H. (1977), "Radial velocities and spectral types of T Tauri stars", Astrophysical Journal, 214: 747–758, Bibcode:1977ApJ...214..747H, doi: 10.1086/155304 .
  6. 1 2 3 4 5 6 7 Torres, Rosa M.; et al. (March 2012), "VLBA Determination of the Distance to nearby Star-forming Regions. V. Dynamical Mass, Distance, and Radio Structure of V773 Tau A", The Astrophysical Journal, 747 (1): 18, arXiv: 1112.0114 , Bibcode:2012ApJ...747...18T, doi:10.1088/0004-637X/747/1/18, S2CID   494696, 18.
  7. 1 2 Boden, Andrew F.; et al. (March 2012), "A Surprising Dynamical Mass for V773 Tau B", The Astrophysical Journal, 747 (1): 17, arXiv: 1112.1018 , Bibcode:2012ApJ...747...17B, doi:10.1088/0004-637X/747/1/17, S2CID   118997621, 17.
  8. 1 2 3 4 5 6 7 8 Boden, Andrew F.; et al. (December 2007), "Dynamical Masses for Pre-Main-Sequence Stars: A Preliminary Physical Orbit for V773 Tau A", The Astrophysical Journal, 670 (2): 1214–1224, arXiv: 0706.2376 , Bibcode:2007ApJ...670.1214B, doi:10.1086/521296, S2CID   40241514.
  9. ↑ "HD 283447". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-01-22.
  10. ↑ Rydgren, A. E.; et al. (March 1976), "The nature of the objects of Joy: a study of the T Tauri phenomenon.", Astrophysical Journal Supplement Series, 30: 307–336, Bibcode:1976ApJS...30..307R, doi:10.1086/190364. See notes about HD 283447.
  11. ↑ Kutner, M. L.; et al. (October 1986), "Detection of 6 CM radio emission from late-type PMS stars with weak chromospheric emission", Astronomical Journal, 92: 895–897, Bibcode:1986AJ.....92..895K, doi: 10.1086/114223 .

Further reading


This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.