GSC 02620-00648
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Hercules |
| A[1] | |
| Right ascension | 17h 53m 13.058s[2] |
| Declination | +37° 12′ 42.36″[2] |
| Apparent magnitude (V) | 11.592[2] |
| 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[3] |
| Apparent magnitude (V) | 11.592 ±0.004[3] |
| Apparent magnitude (J) | 10.583 ±0.018[2] |
| Apparent magnitude (H) | 10.350 ±0.015[2] |
| Apparent magnitude (K) | 10.330 ±0.019[2] |
| Astrometry | |
| Proper motion (μ) | RA: -8.1[2] mas/yr Dec.: -33.0[2] mas/yr |
| Distance | 1400 ± 200 ly (430 ± 60 pc) |
| Details | |
| Mass | 1.18[1]/0.59[1] M☉ |
| Temperature | 6200 ± 75 K |
| Metallicity | 0.14 ± 0.09 |
| Age | 4.7 ± 2 × 109 years |
| Other designations | |
| Database references | |
| SIMBAD | data |
GSC 02620-00648 A is a magnitude 12 star located approximately 1400 light-years away in the constellation of Hercules.[2] This star is about 1.18 times as massive as the Sun.[1]
Planetary system
In 2006 the TrES program discovered exoplanet TrES-4 using the transit method.[3] This planet orbits the primary star.[1]
| 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 fourteen 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]
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]
See also
References
- ^ a b c d e f g h i j k l m n Daemgen; Hormuth, F.; Brandner, W.; Bergfors, C.; Janson, M.; Hippler, S.; Henning, T.; et al. (2009). "Binarity of transit host stars - Implications for planetary parameters" (PDF). Astronomy and Astrophysics. 498: 567–574. arXiv:0902.2179. Bibcode:2009A&A...498..567D. doi:10.1051/0004-6361/200810988.
{{cite journal}}: Explicit use of et al. in:|author=(help) - ^ a b c d e f g h i j "SIMBAD query result: NAME TrES-4 Parent Star -- Star". Centre de Données astronomiques de Strasbourg. Retrieved 2009-04-23.
- ^ a b c Mandushev; O'Donovan, Francis T.; Charbonneau, David; Torres, Guillermo; Latham, David W.; Bakos, Gáspár Á.; Dunham, Edward W.; Sozzetti, Alessandro; Fernández, José M.; et al. (2007). "TrES-4: A Transiting Hot Jupiter of Very Low Density". The Astrophysical Journal Letters. 667: L195–L198. arXiv:0708.0834. Bibcode:2007ApJ...667L.195M. doi:10.1086/522115.
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External links
- "TrES-4". Exoplanets. Retrieved 2009-04-28.
- Muir, Hazel (August 6, 2007). "Largest known exoplanet puzzles astronomers". NewScientist.com news service. Retrieved 2007-08-07.
