Related Research Articles
WASP-4 is a G-type main sequence star approximately 891 light-years away in the constellation of Phoenix. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on close orbit.
WASP-19 is a magnitude 12.3 star located in the Vela constellation of the southern hemisphere. This star has been found to host a transiting hot Jupiter-type planet in tight orbit.
HAT-P-14b, also known as WASP-27b, is an extrasolar planet located approximately 250 parsecs (820 ly) away in the constellation of Hercules, orbiting the 10th magnitude F-type star HAT-P-14. This planet was discovered in 2010 by the HATNet Project using the transit method. It was independently detected by the SuperWASP project.
HD 15082 is a star located roughly 399 light years away in the northern constellation of Andromeda. The star is a Delta Scuti variable and a planetary transit variable. A hot Jupiter type extrasolar planet, named WASP-33b or HD 15082b, orbits this star with an orbital period of 1.22 days. It is the first Delta Scuti variable known to host a planet.
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.
HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.
WASP-26 is a yellow main sequence star in the constellation of Cetus.
HD 233731, or HAT-P-22, is a suspected multiple star system in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye, having an apparent visual magnitude of 9.732. This system is located at a distance of 267 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +13 km/s.
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 1240 light-years away. The star is older than Sun and is strongly depleted in heavy elements compared to Sun, having just 45% of solar abundance. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by giant planet on close orbit.
WASP-35 is a G-type main-sequence star about 660 light-years away. The star's age cannot be well constrained, but it is probably older than the Sun. WASP-35 is similar in concentration of heavy elements compared to the Sun.
GSC 03949-00967 is a G-type main-sequence star about 1190 light-years away. It is older than the Sun, yet is enriched by heavy elements compared to the Sun, having 160% of solar abundance.
Qatar-2 is a K-type main-sequence star about 595 light-years away. 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.
HAT-P-30, also known as WASP-51, is the primary of a binary star system about 700 light-years away. It is a G-type main-sequence star. HAT-P-30 has a similar concentration of heavy elements compared to the Sun.
References
- 1 2 Turner, Jake D.; et al. (2016). "Ground-based near-UV observations of 15 transiting exoplanets: Constraints on their atmospheres and no evidence for asymmetrical transits". Monthly Notices of the Royal Astronomical Society. 459 (1): 789–819. arXiv: 1603.02587 . Bibcode:2016MNRAS.459..789T. doi:10.1093/mnras/stw574.
- 1 2 Clark, B. J. M.; Anderson, D. R.; Madhusudhan, N.; Hellier, C.; Smith, A. M. S.; Collier Cameron, A. (2018), "Thermal emission of WASP-48b in the Ks-band", Astronomy & Astrophysics, 615: A86, arXiv: 1804.01913 , Bibcode:2018A&A...615A..86C, doi:10.1051/0004-6361/201527071, S2CID 89607391
- ↑ Enoch, B.; et al. (2011). "WASP-35b, WASP-48b, and HAT-P-30b/WASP-51b: Two New Planets and an Independent Discovery of a Hat Planet". The Astronomical Journal. 142 (3). 86. arXiv: 1104.2827 . Bibcode:2011AJ....142...86E. doi:10.1088/0004-6256/142/3/86. S2CID 63996398.
- 1 2 Ciceri, S.; Mancini, L.; Southworth, J.; Bruni, I.; Nikolov, N.; d'Ago, G.; Schröder, T.; Bozza, V.; Tregloan-Reed, J.; Henning, Th. (2015), "Physical properties of the HAT-P-23 and WASP-48 planetary systems from multi-colour photometry", Astronomy & Astrophysics, 577: A54, arXiv: 1503.00762 , Bibcode:2015A&A...577A..54C, doi:10.1051/0004-6361/201425449, S2CID 53607610
- ↑ Murgas, F.; Pallé, E.; Parviainen, H.; Chen, G.; Nortmann, L.; Nowak, G.; Cabrera-Lavers, A.; Iro, N. (2017), "The GTC exoplanet transit spectroscopy survey", Astronomy & Astrophysics, 605: A114, arXiv: 1707.03345 , doi:10.1051/0004-6361/201730937, S2CID 55003393
