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G 196-3 is a young low-mass M dwarf type star which is about 100 million years old. The star is located within the Ursa Major constellation about 71.1 light years away[1] from the Earth. During observations by Instituto de Astrofísica de Canarias in Tenerife, Spain in 1998, a substellar-mass object was discovered to orbit approximately 300 astronomical units (AU) from the star. It was detected using direct imaging.[2][3][4][5]

G 196-3
Observation data
Epoch J2000      Equinox J2000
Constellation Ursa Major
Right ascension 10h 04m 21.4629s[1]
Declination 50° 23′ 13.3872″[1]
Apparent magnitude (V) 13.3
Characteristics
Spectral type M3V
U−B color index +1.67
B−V color index +1.16
Astrometry
Radial velocity (Rv)11.7 km/s
Proper motion (μ) RA: −141.177±0.055[1] mas/yr
Dec.: −202.394±0.053[1] mas/yr
Parallax (π)45.8611 ± 0.0388 mas[1]
Distance71.12 ± 0.06 ly
(21.80 ± 0.02 pc)
Absolute magnitude (MV)13.33
Other designations
TYC 3440-13-1, NLTT 23293
Database references
SIMBADdata

Substellar companion


Observations of the substellar object were performed on January 25, 1998 where a faint red companion was present 16.2 arc seconds southwest of the star. A comparison of images taken at different wavelengths was done using low-intermediate-resolution spectroscopy confirmed the presence of a substellar object which was named G 196-3B. The Further observations confirmed the discovery when the team of Rafael Rebolo obtained R & I broadband photometry on March 19, 1998. The TCS Telescope showed its very cool nature in near-infrared (K Band). The comparison of the optical and infrared magnitudes including dust condensation has allowed astronomers to conclude that the substellar object was 25–10+15 Jupiter masses or simply 25 masses that of the Jovian-planet Jupiter. This was the second[6][7] discovery of a brown dwarf that was found around a low-mass star whose age[8] was relatively young. The separation of the star and the substellar object has suggested that both were parts of a fragment from a collapsing cloud although another possible scenario suggests that it originated from a dissipated protoplanetary disk.[9][2][10][11][12][13]

The G 196-3 planetary system[14]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
B 15+30
−4 MJ		 390 — — — —

See also



References


  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Rafael Rebolo; et al. (1998). "Discovery of a Low-Mass Brown Dwarf Companion of the Young Nearby Star G 196-3". Science. 282 (5392): 1309–1312. arXiv:astro-ph/9811413. Bibcode:1998Sci...282.1309R. doi:10.1126/science.282.5392.1309. PMID 9812893. S2CID 10595230.
  3. Kirkpatrick, J. Davy; Gizis, John E.; Burgasser, Adam J.; Wilson, John C.; Dahn, Conard C.; Monet, David G.; Reid, I. Neill; Liebert, James (2001). "Low-Luminosity Companions to Nearby Stars: Status of the 2MASS Data Search". In Jones, Hugh R. A.; Steele, Iain A. (eds.). Ultracool Dwarfs: New Spectral Types L and T. Berlin/Heidelberg: Springer. p. 125. Bibcode:2001udns.conf..125K. doi:10.1007/978-3-642-56672-1_12. ISBN 978-3-642-56672-1.
  4. "G 196-3". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-18.
  5. "Lowell Proper Motion Survey 8991 Northern Stars (Giclas 1971) ReadMe". Centre de Donnes Astronomiques. Retrieved 2010-02-09.
  6. "G196-3B : the second discovery of a brown dwarf around a low-mass star". Instituto de Astrofísica de Canarias (IAC). Retrieved 2010-02-22.
  7. R. Rebolo (2000). "Lithium in Brown Dwarfs". The Light Elements and Their Evolution, Proceedings of IAU Symposium 198, Held 22-26 Nov 1999, Natal, Brazil. Edited by L. Da Silva, R. De Medeiros, & M Spite, 2000. 198: 299. Bibcode:2000IAUS..198..299R.
  8. "ING Scientific Highlights in 1998". Isaac Newton Group of Telescopes. Retrieved 2010-02-18.
  9. "Resultados más relevantes". IAC. Retrieved 2010-02-18.
  10. "196-3B". ExtraSolar.net. Archived from the original on 2010-09-21. Retrieved 2010-02-18.
  11. McGovern, Mark R.; Kirkpatrick, J. Davy; McLean, Ian S.; Burgasser, Adam J.; Prato, L.; Lowrance, Patrick J. (2004). "Identifying Young Brown Dwarfs Using Gravity-Sensitive Spectral Features". The Astrophysical Journal. 600 (2): 1020–1024. arXiv:astro-ph/0309634. Bibcode:2004ApJ...600.1020M. doi:10.1086/379849. S2CID 475796.
  12. Allers; Liu; Dupuy; Cushing (2009). "Discovery of Young Dwarf L Binary". Astrophysical Journal. 715 (561): 561–571. arXiv:0912.4687. Bibcode:2010ApJ...715..561A. doi:10.1088/0004-637X/715/1/561. S2CID 116058913.
  13. "2MASSW J1004207+502300". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-18.
  14. Zakhozhay, Olga; Zapatero Osorio, María Rosa; Béjar, Víctor J. S.; Boehler, Yann (2017), "Spectral energy distribution simulations of a possible ring structure around the young, red brown dwarf G 196-3 B", Monthly Notices of the Royal Astronomical Society, 464 (1): 1108–1118, doi:10.1093/mnras/stw2308

На других языках

[de] G 196-3

G 196-3 ist ein Roter Zwerg mit einer scheinbaren Helligkeit von 11,8 mag im Sternbild Großer Bär. Im Jahre 1998 entdeckten Rebolo et al. ein substellares Objekt (vermutlich ein Brauner Zwerg) der Spektralklasse L2, das sehr wahrscheinlich gravitativ an diesen Stern gebunden ist und mit G 196-3 B bezeichnet wird. Grob geschätzt dürfte seine Masse im Bereich von 25 Jupitermassen liegen. Der Winkelabstand der beiden Objekte beträgt 16" bei einem Positionswinkel von 209°.
- [en] G 196-3

[es] G 196-3

G 196-3 (NLTT 23293 / GSC 03440-00013)[1] es una estrella de magnitud aparente +11,77 situada en la constelación de la Osa Mayor. Aunque inicialmente se estimó que se encontraba a 68 años luz, hoy se piensa que su distancia respecto al Sistema Solar es de 49 ± 9 años luz.[2] En 1998 se descubrió un objeto de masa subestelar —una enana marrón— en órbita alrededor de esta estrella.[3]


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