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GSC 03089-00929 is a magnitude 12 star located approximately 757 light-years away in the constellation of Hercules. This star is a G type main sequence star that is similar to but slightly cooler than the Sun. This star is identified in SIMBAD as a variable star per the 1SWASP survey.
HAT-P-3, is a metal-rich K5 dwarf star located about 441 light-years away in the constellation Ursa Major. At a magnitude of about 11.5 it is not visible to the naked eye but is visible in a small to medium-sized amateur telescope. It is believed to be a relatively young star and has a slightly enhanced level of chromospheric activity.
WASP-48b is an extrasolar planet orbiting the star WASP-48 in the constellation Cygnus. The planet was detected using the transit method by the SuperWASP team, which published its discovery in 2011. It orbits its host star in just 2.14 days with a semi-major axis of 0.034 AU and has an equilibrium temperature of 1956±54 K. The dayside temperature was measured to be around 2300 K in 2018.
WASP-21 is a G-type star that is reaching the end of its main sequence lifetime approximately 850 light years from Earth in the constellation of Pegasus. The star is relatively metal-poor, having 40% of heavy elements compared to the Sun. Kinematically, WASP-21 belongs to the thick disk of the Milky Way. It has an exoplanet named WASP-21b.
WASP-26 is a yellow main sequence star in the constellation of Cetus.
WASP-36 is a yellow main sequence star in the Hydra constellation.
Qatar-1 is an orange main sequence star in the constellation of Draco.
HAT-P-23 is a G-type main-sequence star 1192 light-years away. It has a rapid rotation for its advanced age of 4 billion years, and exhibits a strong starspot activity. The star may be in the process of being spun up by the giant planet on close orbit. The star is enriched in heavy elements, having about 140% amount of metals compared to solar abundance.
HAT-P-16 is a F-type main-sequence star about 725 light-years away. The star has a concentration of heavy elements slightly higher than solar abundance, and low starspot activity. The survey in 2015 have failed to find any stellar companions to it. The spectral analysis in 2014 have discovered the HAT-P-16 has a carbon to oxygen molar ratio of 0.58±0.08, close to Sun`s value of 0.55.
WASP-50 is a G-type main-sequence star about 594 light-years away. The star is older than the Sun and slightly depleted in heavy elements compared to the Sun, and has a close to average starspot activity. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by giant planet on close orbit.
WASP-48 is a subgiant star about 1400 light-years away. The star is likely older than Sun and slightly depleted in heavy elements. It shows an infrared excess noise of unknown origin, yet has no detectable ultraviolet emissions associated with the starspot activity. The discrepancy may be due to large interstellar absorption of light in interstellar medium for WASP-48. The measurements are compounded by the emission from eclipsing contact binary NSVS-3071474 projected on sky plane nearby, although no true stellar companions were detected by survey in 2015.
WASP-46 is a G-type main-sequence star about 1,210 light-years away. The star is older than the Sun and is strongly depleted in heavy elements compared to the Sun, having just 45% of the solar abundance. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on a close orbit.
WASP-45 is a K-type main-sequence star about 701 light-years away. The star's age cannot be well constrained, but it is probably older than the Sun. Yet, WASP-45 is enriched in heavy elements compared to the Sun, having 240% of the solar abundance.
Qatar-2 is a K-type main-sequence star about 595 light-years away in the constellation of Virgo. The star is much older than Sun, and has a concentration of heavy elements similar to solar abundance. The star features a numerous and long-lived starspots, and belongs to a peculiar variety of inflated K-dwarfs with strong magnetic activity inhibiting internal convection.
WASP-64 is a star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. It is younger than the Sun at 3.6±1.6 billion years, and it has a metal abundance similar to the Sun. The star is rotating rapidly, being spun up by the giant planet in a close orbit.
WASP-67 is a K-type main-sequence star about 620 light-years away. The stars age is poorly constrained, but is likely older than the Sun`s at approximately 8.7+5.5
−8.6 billion years. WASP-67 is slightly depleted in heavy elements, having 85% of the solar abundance of iron.
WASP-55 is a G-type main-sequence star about 980 light-years away. The star is much younger than the Sun at approximately 1.1+0.8
−0.6 billion years. WASP-55 is similar to the Sun in concentration of heavy elements.
WASP-42 is a K-type main-sequence star. Its surface temperature is 5315±79 K. WASP-42 is similar to the Sun in concentration of heavy elements, with metallicity ([Fe/H]) of 0.05±0.13, and is much older than the Sun at 11.3+1.5
−4.8 billion years. The star does exhibit starspot activity as is typical for its spectral class.
WASP-41 is a G-type main-sequence star. Its surface temperature is 5450±150 K. WASP-41 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of −0.080±0.090, but is much younger at an age of 2.289±0.077 billion years. The star does exhibit strong starspot activity, with spots covering 3% of the stellar surface.
References
- 1 2 3 4 5 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.
- 1 2 3 Maciejewski, G.; Dimitrov, D.; Mancini, L.; Southworth, J.; Ciceri, S.; D'Ago, G.; Bruni, I.; Raetz, St.; Nowak, G.; Ohlert, J.; Puchalski, D.; Saral, G.; Derman, E.; Petrucci, R.; Jofre, E.; Seeliger, M.; Henning, T. (2016), "New Transit Observations for HAT-P-30 b, HAT-P-37 b, TrES-5 b, WASP-28 b, WASP-36 b and WASP-39 b", Acta Astronomica, 66 (1): 55, arXiv: 1603.03268 , Bibcode:2016AcA....66...55M
- 1 2 3 Skrutskie, Michael F.; et al. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode: 2006AJ....131.1163S . doi: 10.1086/498708 . Vizier catalog entry
- 1 2 3 Mandushev, Georgi; Quinn, Samuel N.; Buchhave, Lars A.; Dunham, Edward W.; Rabus, Markus; Oetiker, Brian; Latham, David W.; Charbonneau, David; Brown, Timothy M.; Belmonte, Juan A.; O'Donovan, Francis T. (2011), "TrES-5: A Massive Jupiter-sized Planet Transiting A Cool G-dwarf", The Astrophysical Journal, 741 (2): 114, arXiv: 1108.3572 , Bibcode:2011ApJ...741..114M, doi:10.1088/0004-637X/741/2/114, S2CID 118671116
- 1 2 Mislis, D.; Mancini, L.; Tregloan-Reed, J.; Ciceri, S.; Southworth, J.; d'Ago, G.; Bruni, I.; Baştürk, Ö.; Alsubai, K. A.; Bachelet, E.; Bramich, D. M.; Henning, Th.; Hinse, T. C.; Iannella, A. L.; Parley, N.; Schroeder, T. (2015), "High-precision multiband time series photometry of exoplanets Qatar-1b and TrES-5b", Monthly Notices of the Royal Astronomical Society, 448 (3): 2617–2623, arXiv: 1503.02246 , Bibcode:2015MNRAS.448.2617M, doi: 10.1093/mnras/stv197 , S2CID 53561305
- ↑ "GSC 03949-00967". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2022-01-06.
- 1 2 Sokov, Eugene N.; Sokova, Iraida A.; Dyachenko, Vladimir V.; Rastegaev, Denis A.; Burdanov, Artem; Rusov, Sergey A.; Benni, Paul; Shadick, Stan; Hentunen, Veli-Pekka; Salisbury, Mark; Esseiva, Nicolas; Garlitz, Joe; Bretton, Marc; Ogmen, Yenal; Karavaev, Yuri; Ayiomamitis, Anthony; Mazurenko, Oleg; Alonso, David; Velichko, Sergey F. (2018), "Transit timing analysis of the exoplanet TrES-5 b. Possible existence of the exoplanet TrES-5 c", Monthly Notices of the Royal Astronomical Society, 480 (1): 291–301, arXiv: 1806.03503 , Bibcode:2018MNRAS.480..291S, doi: 10.1093/mnras/sty1615 , S2CID 53665645
- ↑ Maciejewski, G.; et al. (December 2021). "Revisiting TrES-5 b: departure from a linear ephemeris instead of short-period transit timing variation". Astronomy & Astrophysics. 656. A88. arXiv: 2110.14294 . Bibcode: 2021A&A...656A..88M . doi: 10.1051/0004-6361/202142424 .
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