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WASP-8 is a binary star system 294 light-years away. The star system is much younger than the Sun at 300 million to 1.2 billion years age, and is heavily enriched in heavy elements, having nearly twice the concentration of iron compared to the Sun.
WASP-11/HAT-P-10 is a binary star. It is a primary main-sequence orange dwarf star. Secondary is M-dwarf with a projected separation of 42 AU. The system is located about 424 light-years away in the constellation Aries.
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 a close orbit.
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.
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-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-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.
BD+00 316 is an ordinary star with a close-orbiting planetary companion in the equatorial constellation of Cetus. It is also known as WASP-71 since 2019; BD+00 316 is the stellar identifier from the Bonner Durchmusterung catalogue. With an apparent visual magnitude of 10.56, it is too faint to be visible to the naked eye. This star is located at a distance of 1,160 light-years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 7.7 km/s.
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-59 is a K-type main-sequence star about 379 light-years away. The star's age is essentially unconstrained by observations. WASP-59 is slightly depleted in heavy elements, having 70% of the solar abundance of iron. The star produces extremely low levels of ultraviolet light, indicating an absence of flare activity.
WASP-54, also known as BD+00 3088, is a binary star system about 825 light-years away. The primary, WASP-54A, is a F-type main-sequence star, accompanied by the red dwarf WASP-54B on a wide orbit. WASP-54 is depleted in heavy elements, having 55% of the solar abundance of iron. The age of WASP-54 is slightly older than the Sun's at 6.9+1.0
−1.9 billion years.
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.
WASP-75 is a F-type main-sequence star about 980 light-years away. The star is much younger than the Sun at approximately 2.9±0.2 billion years. WASP-75 is similar to the Sun in its concentration of heavy elements.
WASP-88 is a F-type main-sequence star. Its surface temperature is 6450±61 K. WASP-88 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.03±0.04, and is younger at an age of 3.0±1.3 billion years.
WASP-84, also known as BD+02 2056, is a G-type main-sequence star 327 light-years away in the constellation Hydra. Its surface temperature is 5350±31 K and is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.05±0.02. It is rich in carbon and depleted of oxygen. WASP-84's age is probably older than the Sun at 8.5+4.1
−5.5 billion years. The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.
References
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- ↑ Ginski, C.; Mugrauer, M.; Seeliger, M.; Löhne, T. (November 2013), "The multiplicity status of three exoplanet host stars", Astronomy & Astrophysics , 559: 6, Bibcode:2013A&A...559A..71G, doi: 10.1051/0004-6361/201322274
- 1 2 3 4 5 6 7 Bai, Lu; Gu, Shenghong; Wang, Xiaobin; Sun, Leilei; Kwok, Chi-Tai; Hui, Ho-Keung (2022), "WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry", The Astronomical Journal, 163 (5): 208, arXiv: 2203.02866 , Bibcode:2022AJ....163..208B, doi: 10.3847/1538-3881/ac5b6a , S2CID 247292453
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- ↑ "BD+06 1909", SIMBAD , Centre de données astronomiques de Strasbourg
- ↑ Wöllert, Maria; Brandner, Wolfgang (2015), "A Lucky Imaging search for stellar sources near 74 transit hosts", Astronomy & Astrophysics, 579: A129, arXiv: 1506.05456 , Bibcode:2015A&A...579A.129W, doi:10.1051/0004-6361/201526525, S2CID 118903879
- 1 2 Johnson, John Asher; Winn, J. N.; Bakos, G. Á.; Hartman, J. D.; Morton, T. D.; Torres, G.; Kovács, Géza; Latham, D. W.; Noyes, R. W.; Sato, B.; Esquerdo, G. A.; Fischer, D. A.; Marcy, G. W.; Howard, A. W.; Buchhave, L. A.; Fűrész, G.; Quinn, S. N.; Béky, B.; Sasselov, D. D.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P. (2011), "HAT-P-30b: A transiting hot Jupiter on a highly oblique orbit", The Astrophysical Journal, 735 (1): 24, arXiv: 1103.3825 , Bibcode:2011ApJ...735...24J, doi:10.1088/0004-637X/735/1/24, S2CID 53689766