Summary
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]
| Observation data Epoch J2000.0 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 mas[2] |
| 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 mas[4] |
| 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 |
| Temperature | 6,200±75[citation needed] K |
| Metallicity [Fe/H] | +0.14±0.09[citation needed] dex |
| Rotational velocity (v sin i) | 8.3[6] km/s |
| Age | 4.7±2[citation needed] Gyr |
| B | |
| Mass | 0.59[1] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
Planetary system edit
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 edit
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 edit
Notes edit
References edit
- ^ a b c d e f g h i j k l 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. arXiv:0902.2179. Bibcode:2009A&A...498..567D. doi:10.1051/0004-6361/200810988. S2CID 9893376.
- ^ a b c d e f g h Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e "NAME TrES-4 Parent Star". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-04-23.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ 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.; 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.
- ^ 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. arXiv:1804.00673. Bibcode:2018ApJS..237...38B. doi:10.3847/1538-4365/aad501. S2CID 119431797.
- ^ 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. arXiv:0902.2179. Bibcode:2009A&A...498..567D. doi:10.1051/0004-6361/200810988. ISSN 0004-6361. S2CID 9893376.
External links edit
- "TrES-4". Exoplanets. Archived from the original on 2009-11-25. Retrieved 2009-04-28.
- Muir, Hazel (August 6, 2007). "Largest known exoplanet puzzles astronomers". NewScientist.com news service. Retrieved 2007-08-07.