Astronomy:GSC 02620-00648
| Observation data {{#ifeq:J2000.0|J2000.0 (ICRS)|Epoch J2000.0 Equinox J2000.0 (ICRS)| Epoch J2000.0 [[Astronomy:Equinox (celestial coordinates)|Equinox J2000.0}} | |
|---|---|
| Constellation | Hercules |
| A[1] | |
| Right ascension | 17h 53m 13.0490s[2] |
| Declination | +37° 12′ 42.586″[2] |
| Apparent magnitude (V) | 11.592[3] |
| Ca | |
| Right ascension | ~ 17h 53m 13.0496s[4] |
| Declination | ~+37° 12′ 44.139″[4] |
| Apparent magnitude (V) | 13.85[1] |
| Characteristics | |
| Spectral type | F8[1]/K or M[1] |
| Apparent magnitude (B) | 12.1120005 ±0.007[5] |
| Apparent magnitude (V) | 11.592 ±0.004[5] |
| 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 | |
| A | |
| Proper motion (μ) | RA: −6.382[2] mas/yr Dec.: −20.891[2] mas/yr |
| Parallax (π) | 1.9686 ± 0.0124[2] mas |
| Distance | 1,660 ± 10 ly (508 ± 3 pc) |
| C | |
| Proper motion (μ) | RA: −6.307[4] mas/yr Dec.: −20.387[4] mas/yr |
| Parallax (π) | 1.9657 ± 0.1076[4] mas |
| Distance | 1,660 ± 90 ly (510 ± 30 pc) |
| Details | |
| A | |
| Mass | 1.18[1] M☉ |
| Radius | 1.9[2] R☉ |
| Luminosity | 4.6[2] L☉ |
| Surface gravity (log g) | 3.98[2] cgs |
| Rotational velocity (v sin i) | 8.3[6] km/s |
| B | |
| Mass | 0.59[1] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Extrasolar Planets Encyclopaedia | data |
GSC 02620-00648 is a double star in the constellation Hercules. The brighter of the pair is a magnitude 12 star located approximately 1,660 light-years away. This star is about 1.18 times as massive as the Sun.[1]
Planetary system
In 2006 the TrES program discovered exoplanet TrES-4b using the transit method.[5] This planet orbits the primary star.[1]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.919 ± 0.073[1] MJ | 0.05091 ± 0.00071[1] | 3.553945 ± 7.5e-05 | 0 | — | 1.799[7] RJ |
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
- Trans-Atlantic Exoplanet Survey
- List of extrasolar planets
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
- ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 Daemgen; Hormuth, F.; Brandner, W.; Bergfors, C.; Janson, M.; Hippler, S.; Henning, T. (2009). "Binarity of transit host stars - Implications for planetary parameters". Astronomy and Astrophysics 498 (2): 567–574. doi:10.1051/0004-6361/200810988. Bibcode: 2009A&A...498..567D.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 "NAME TrES-4 Parent Star". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=NAME+TrES-4+Parent+Star.
- ↑ 4.0 4.1 4.2 4.3 4.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 5.0 5.1 5.2 Mandushev; O'Donovan, Francis T.; Charbonneau, David; Torres, Guillermo; Latham, David W.; Bakos, Gáspár Á.; Dunham, Edward W.; Sozzetti, Alessandro et al. (2007). "TrES-4: A Transiting Hot Jupiter of Very Low Density". The Astrophysical Journal Letters 667 (2): L195–L198. doi:10.1086/522115. Bibcode: 2007ApJ...667L.195M.
- ↑ Brewer, John M.; Fischer, Debra A. (2018). "Spectral Properties of Cool Stars: Extended Abundance Analysis of Kepler Objects of Interest". The Astrophysical Journal Supplement Series 237 (2): 38. doi:10.3847/1538-4365/aad501. Bibcode: 2018ApJS..237...38B.
- ↑ Daemgen, S.; Hormuth, F.; Brandner, W.; Bergfors, C.; Janson, M.; Hippler, S.; Henning, Th (May 2009). "Binarity of Transit Host Stars - Implications on Planetary Parameters". Astronomy & Astrophysics 498 (2): 567–574. doi:10.1051/0004-6361/200810988. ISSN 0004-6361. Bibcode: 2009A&A...498..567D.
External links
- "TrES-4". Exoplanets. http://media4.obspm.fr/exoplanets/base/etoile.php?nom=TrES-4.
- Muir, Hazel (August 6, 2007). "Largest known exoplanet puzzles astronomers". NewScientist.com news service. https://www.newscientist.com/article/dn12430-largest-known-exoplanet-puzzles-astronomers.html.
Coordinates: 
17h 53m 13s, +37° 12′ 42″
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