Astronomy:GV Tauri
Coordinates: 
04h 29m 23.7315s, +24° 33′ 00.2160″
| Observation data {{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0 Equinox J2000.0 (ICRS)| Epoch J2000 [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}} | |
|---|---|
| Constellation | Taurus |
| GV Tauri A | |
| Right ascension | 04h 29m 23.71056s[2] |
| Declination | +24° 32′ 58.6176″[2] |
| Apparent magnitude (V) | |
| GV Tauri B | |
| Right ascension | 04h 29m 23.6868s[3] |
| Declination | +24° 33′ 01.1160″[3] |
| Apparent magnitude (V) | |
| 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±0.4[5] mas/yr Dec.: −26.7±0.3[5] mas/yr |
| Parallax (π) | 7.01 ± 0.34[5] mas |
| Distance | 470 ± 20 ly (143 ± 7 pc) |
| GV Tauri B | |
| Position (relative to GV Tauri A) | |
| Component | GV Tauri B |
| Angular distance | 1.2″ [6] |
| Observed separation (projected) | 170 AU |
| Details[4] | |
| GV Tauri A | |
| Mass | 1.8 M☉ |
| Luminosity | 2.3 L☉ |
| Surface gravity (log g) | 4.0 cgs |
| Temperature | 4800±200 K |
| Age | 0.5[6] Myr |
| GV Tauri B | |
| Luminosity | 114 L☉ |
| Age | 0.5[6] Myr |
| Other designations | |
2MASS J04292373+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 Tauri is a young binary system composed of T Tauri-type pre-main sequence stars in the constellation of Taurus about 466 light years away, belonging to the Taurus Molecular Cloud.
In 1978, Jonathan H. Elias announced that the object, then known as Haro 6-10, is a variable star, based on near infrared observations made from 1975 through 1978.[7]
System
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 170 AU. 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,[8] as they produce strongly ionized jets and molecular outflows.[9]
Properties
Both members of the binary system are medium-mass objects still contracting towards the main sequence and accreting mass, although accretion rates remain highly uncertain as of 2009.[4]
Protoplanetary system
Both stars are surrounded by protoplanetary disks, with the observable dust in each being about 5×10−5 M☉, and the gas about 0.005 M☉.[6] The disk of GV Tauri B is rich in carbon monoxide, hydrogen cyanide and, unusually, methane.[9]
| 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[9] AU | 30 or 80±10[6]° | — | |||
References
- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
- ↑ 2.0 2.1 2.2 "V* GV Tau A". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+GV+Tau+A.
- ↑ 3.0 3.1 3.2 "V* GV Tau B". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+GV+Tau+B.
- ↑ 4.0 4.1 4.2 4.3 4.4 Prato, 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. doi:10.1088/0004-6256/137/4/3931. Bibcode: 2009AJ....137.3931P.
- ↑ 5.0 5.1 5.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 Sheehan, Patrick D.; Eisner, Josh A. (2014). "CONSTRAINING THE DISK MASSES OF THE CLASS I BINARY PROTOSTAR GV Tau". The Astrophysical Journal 791 (1): 19. doi:10.1088/0004-637X/791/1/19. Bibcode: 2014ApJ...791...19S.
- ↑ Elias, J. H. (September 1978). "A study of the Taurus dark cloud complex". Astrophysical Journal 224: 857–872. doi:10.1086/156436. Bibcode: 1978ApJ...224..857E. https://articles.adsabs.harvard.edu/pdf/1978ApJ...224..857E. Retrieved 5 September 2025.
- ↑ 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. doi:10.1088/0004-637X/753/2/143. Bibcode: 2012ApJ...753..143W.
- ↑ 9.0 9.1 9.2 Fuente, 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. doi:10.1093/mnras/staa1919.
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