GV Tauri
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Taurus |
| GV Tauri A | |
| Right ascension | 04h29m23.71056s[2] |
| Declination | +24° 32′ 58.6176″[2] |
| GV Tauri B | |
| Right ascension | 04h29m23.6868s[3] |
| Declination | +24° 33′ 01.1160″[3] |
| Characteristics | |
| GV Tauri A | |
| Evolutionary stage | pre-main-sequence star |
| Spectral type | K3[4] |
| Apparent magnitude(K) | 10.872[2] |
| Apparent magnitude(g) | 16.282[5] |
| Variable type | T Tau |
| GV Tauri B | |
| Spectral type | late G to early K[4] |
| Apparent magnitude(K) | 10.171[3] |
| Astrometry | |
| GV Tauri A | |
| Proper motion(μ) | RA:8.0±0.4mas/yr[5] Dec.:−26.7±0.3mas/yr[5] |
| Parallax(π) | 7.01 ± 0.34mas[5] |
| Distance | 470 ± 20ly (143 ± 7pc) |
| GV Tauri B | |
| Position (relative to GV Tauri A) | |
| Component | GV Tauri B |
| Angular distance | 1.2″[6] |
| Projected separation | 170AU |
| Details[4] | |
| GV Tauri A | |
| Mass | 1.8M☉ |
| Luminosity | 2.3L☉ |
| Surface gravity(logg) | 4.0cgs |
| Temperature | 4800±200K |
| Age | 0.5[6]Myr |
| GV Tauri B | |
| Luminosity | 114L☉ |
| Age | 0.5[6]Myr |
| Other designations | |
2MASSJ04292373+2433002, Haro 6-10, TIC 268217520, Elia 3-7, LEI 4, HBC 389 | |
| GV Tauri A:Gaia EDR3 149367383323435648, GV Tau S, EPIC 247820507, Haro 6-10 VLA 1, LEI 4A | |
| GV Tauri B:GV Tau N, Haro 6-10 VLA 2, LEI 4B | |
| Database references | |
| SIMBAD | data |
GK Tauriis a young binary system composed ofT Tauri-typepre-main sequence starsin the constellation ofTaurusabout466light yearsaway, belonging to theTaurus Molecular Cloud.
System
[edit]The stars GV Tauri A (GV Tauri S) and G Tauri B (GV Tauri N) form a wide binary system, with the projected separation between components being 170AU.Both are strongly shrouded by circumstellar dust - GV Tauri A by 30 magnitudes and the GV Tauri B up to 59 magnitudes in the V band.[4]Both components are suspected to be binaries themselves,[7]as they produce strongly ionized jets and molecular outflows.[8]
Properties
[edit]Both members of the binary system are medium-mass objects still contracting towards themain sequenceand accreting mass, although accretion rates remain highly uncertain as of 2009.[4]
Protoplanetary system
[edit]Both stars are surrounded byprotoplanetary disks,with the observable dust in each being about5×10−5M☉,and the gas about 0.005M☉.[6]The disk of GV Tauri B is rich incarbon monoxide,hydrogen cyanideand, unusually,methane.[8]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| protoplanetary disk | 0–17[6]AU | 65±5[6]° | — | |||
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| protoplanetary disk | 20[8]AU | 30 or 80±10[6]° | — | |||
References
[edit]- ^"MAST: Barbara A. Mikulski Archive for Space Telescopes".Space Telescope Science Institute.Retrieved8 December2021.
- ^abc"V* GV Tau A".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2021-08-03.
- ^abc"V* GV Tau B".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2021-08-03.
- ^abcdePrato, L.; Lockhart, K. E.; Johns-Krull, Christopher M.; Rayner, John T. (2009). "Stellar and Circumstellar Properties of Class I Protostars".The Astronomical Journal.137(4): 3931–3941.arXiv:0902.1289.Bibcode:2009AJ....137.3931P.doi:10.1088/0004-6256/137/4/3931.S2CID12428060.
- ^abcBrown, A. G. A.;et al. (Gaia collaboration) (2021)."GaiaEarly 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.S2CID227254300.(Erratum:doi:10.1051/0004-6361/202039657e).Gaia EDR3 record for this sourceatVizieR.
- ^abcdefgSheehan, Patrick D.; Eisner, Josh A. (2014). "CONSTRAINING THE DISK MASSES OF THE CLASS I BINARY PROTOSTAR GV Tau".The Astrophysical Journal.791(1): 19.arXiv:1405.7959.Bibcode:2014ApJ...791...19S.doi:10.1088/0004-637X/791/1/19.S2CID118437418.
- ^Wilking, Bruce A.; Marvel, Kevin B.; Claussen, Mark J.; Gerling, Bradley M.; Wootten, Alwyn; Gibb, Erika (2012). "A Proper Motion Study of the Haro 6-10 Outflow: Evidence for a Subarcsecond Binary".The Astrophysical Journal.753(2): 143.arXiv:1205.5760.Bibcode:2012ApJ...753..143W.doi:10.1088/0004-637X/753/2/143.S2CID18213612.
- ^abcFuente, A.; Treviño-Morales, S. P.; Le Gal, R.; Rivière-Marichalar, P.; Pilleri, P.; Rodríguez-Baras, M.; Navarro-Almaida, D. (2020)."Gas kinematics of key prebiotic molecules in GV Tau N revealed with an ALMA, PdBI, and Herschel synergy".Monthly Notices of the Royal Astronomical Society.496(4): 5330–5340.arXiv:2006.15065.doi:10.1093/mnras/staa1919.
