Wikipedia

GV Tauri

GV Tauri

A light curve for GV Tauri, plotted from Kepler data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
GV Tauri A
Right ascension 04h 29m 23.71056s[2]
Declination +24° 32′ 58.6176″[2]
GV Tauri B
Right ascension 04h 29m 23.6868s[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±0.4 mas/yr[5]
Dec.: −26.7±0.3 mas/yr[5]
Parallax (π)7.01±0.34 mas[5]
Distance470 ± 20 ly
(143 ± 7 pc)
GV Tauri B
Position (relative to GV Tauri A)
ComponentGV Tauri B
Angular distance1.2″ [6]
Projected separation170 AU
Details[4]
GV Tauri A
Mass1.8 M☉
Luminosity2.3 L☉
Surface gravity (log g)4.0 cgs
Temperature4800±200 K
Age0.5[6] Myr
GV Tauri B
Luminosity114 L☉
Age0.5[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
SIMBADdata

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

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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

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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

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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]

The GV Tauri A planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
protoplanetary disk 0–17[6] AU 65±5[6]° —
The GV Tauri B planetary system
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

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  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c "V* GV Tau A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-08-03.
  3. ^ a b c "V* GV Tau B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-08-03.
  4. ^ a b c d e 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. arXiv:0902.1289. Bibcode:2009AJ....137.3931P. doi:10.1088/0004-6256/137/4/3931. S2CID 12428060.
  5. ^ a b c 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.
  6. ^ a b c d e f g 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. arXiv:1405.7959. Bibcode:2014ApJ...791...19S. doi:10.1088/0004-637X/791/1/19. S2CID 118437418.
  7. ^ Elias, J. H. (September 1978). "A study of the Taurus dark cloud complex". Astrophysical Journal. 224: 857–872. Bibcode:1978ApJ...224..857E. doi:10.1086/156436. Retrieved 5 September 2025.
  8. ^ 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. S2CID 18213612.
  9. ^ a b c 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. arXiv:2006.15065. doi:10.1093/mnras/staa1919.