GSC 02620-00648

GSC 02620-00648 is a double star in the constellation Hercules. The brighter of the pair is a magnitude 12 star located approximately 1400 light-years away.[3] This star is about 1.18 times as massive as the Sun.[1]

GSC 02620-00648
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hercules
A[1]
Right ascension 17h 53m 13.0502s[2]
Declination +37° 12′ 42.595″[2]
Apparent magnitude (V) 11.592[3]
Ca
Right ascension ~17h 53m 13s[1]
Declination ~+37° 12′ 42″[1]
Apparent magnitude (V) 13.85[1]
Characteristics
Spectral type F8[1]/K or M[1]
Apparent magnitude (B) 12.1120005 ±0.007[4]
Apparent magnitude (V) 11.592 ±0.004[4]
Apparent magnitude (J) 10.583 ±0.018[3]
Apparent magnitude (H) 10.350 ±0.015[3]
Apparent magnitude (K) 10.330 ±0.019[3]
Astrometry
Proper motion (μ) RA: −7.388±0.754[2] mas/yr
Dec.: −21.461±0.668[2] mas/yr
Parallax (π)2.31 ± 0.25[2] mas
Distanceapprox. 1,400 ly
(approx. 430 pc)
Details
Mass1.18[1]/0.59[1] M☉
Temperature6200 ± 75 K
Metallicity0.14 ± 0.09
Age4.7 ± 2 × 109 years
Other designations
TrES-4 Parent Star, 2MASS J17531304+3712426, TYC 2620-648-1[3]
Database references
SIMBADdata
Extrasolar Planets
Encyclopaedia		data

Planetary system

In 2006 the TrES program discovered exoplanet TrES-4 using the transit method.[4] This planet orbits the primary star.[1]

The GSC 02620-00648 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
TrES-4 0.919 ± 0.073[1] MJ 0.05091 ± 0.00071[1] 3.553945 ± 7.5e-05 0 — —

Binary star

In 2008 a study was undertaken of 14 stars with exoplanets that were originally discovered using the transit method through relatively small telescopes. These systems were re-examined with the 2.2M reflector telescope at the Calar Alto Observatory in Spain. This star system, along with two others, was determined to be a previously unknown binary star system. The previously unknown secondary star is a dim magnitude 14 K or M-type star separated by about 755 AU from the primary, appearing offset from the primary by about one arc second in the images. This discovery resulted in a recalculation of parameters for both the planet and the primary star.[1]

See also

Notes
  • Note b: The secondary star is identified with a "C" suffix so as to not confuse it with the planetary designation suffix "b".[1]

References
  1. Daemgen; Hormuth, F.; Brandner, W.; Bergfors, C.; Janson, M.; Hippler, S.; Henning, T. (2009). "Binarity of transit host stars - Implications for planetary parameters" (PDF). Astronomy and Astrophysics. 498 (2): 567–574. arXiv:0902.2179. Bibcode:2009A&A...498..567D. doi:10.1051/0004-6361/200810988. S2CID 9893376.
  2. Brown, A. G. A; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. 595. A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512. S2CID 1828208.Gaia Data Release 1 catalog entry
  3. "NAME TrES-4 Parent Star". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-04-23.
  4. Mandushev; O'Donovan, Francis T.; Charbonneau, David; Torres, Guillermo; Latham, David W.; Bakos, Gáspár Á.; Dunham, Edward W.; Sozzetti, Alessandro; Fernández, José M.; Esquerdo, Gilbert A.; Everett, Mark E.; Brown, Timothy M.; Rabus, Markus; Belmonte, Juan A.; Hillenbrand, Lynne A. (2007). "TrES-4: A Transiting Hot Jupiter of Very Low Density". The Astrophysical Journal Letters. 667 (2): L195–L198. arXiv:0708.0834. Bibcode:2007ApJ...667L.195M. doi:10.1086/522115. S2CID 6087170.

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