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HD 38529 is a binary star approximately 138 light-years away in the constellation of Orion.
HD 142 is a wide binary star system in the southern constellation of Phoenix. The main component has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.7. The system is located at a distance of 85.5 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +6 km/s.
HAT-P-1b is an extrasolar planet orbiting the Sun-like star HAT-P-1, also known as ADS 16402 B. HAT-P-1 is the dimmer component of the ADS 16402 binary star system. It is located roughly 521 light years away from Earth in the constellation Lacerta. HAT-P-1b is among the least dense of any of the known extrasolar planets.
HAT-P-6 also named Sterrennacht is a star in the constellation Andromeda, located approximately 895 light years or 274 parsecs away from the Earth. It is an F-type star, implying that it is hotter and more massive than the Sun. The apparent magnitude of the star is +10.54, which means that it can only be visible through the telescope. The absolute magnitude of +3.36 is brighter than the Sun's +4.83, meaning that the star itself is brighter than the Sun. A search for a binary companion star using adaptive optics at the MMT Observatory turned out negative.
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.
HAT-P-9 is a magnitude 12 F star approximately 1500 light years away in the constellation Auriga. A search for a binary companion star using adaptive optics at the MMT Observatory was negative.
HAT-P-4 is a wide binary star consisting of a pair of G-type main-sequence stars in the constellation of Boötes. It is also designated BD+36°2593.
XO-2 is a binary star. It consists of two components: XO-2S and XO-2N, both of which has two known exoplanets.
HAT-P-11, also designated GSC 03561-02092 and Kepler-3, is an orange dwarf metal rich star about 123 light-years away in the constellation Cygnus. This star is notable for its relatively large rate of proper motion. The magnitude of this star is about 9, which means it is not visible to the naked eye but can be seen with a medium-sized amateur telescope on a clear dark night. The age of this star is about 6.5 billion years.
HAT-P-7 is a F-type main sequence star located about 1088 light-years away in the constellation Cygnus. The apparent magnitude of this star is 10.5, which means it is not visible to the naked eye but can be seen with a small telescope on a clear dark night.
HAT-P-8 is a magnitude 10 star located 700 light-years away in Pegasus. It is a F-type star about 28% more massive than the Sun. Two red dwarf companions have been detected around HAT-P-8. The first has a spectral type of M5V and has a mass of 0.22 M☉. The second is even less massive, at 0.18 M☉, and its spectral type is M6V.
HAT-P-12 is a magnitude 13 low-metallicity K dwarf star approximately 463 light years away in the constellation Canes Venatici, which hosts one known exoplanet.
HAT-P-33 is a late-F dwarf star. It is orbited by a planet called HAT-P-33b. A search for a binary companion star using adaptive optics at the MMT Observatory was negative.
HAT-P-17 is a K-type main-sequence star about 92.6 parsecs (302 ly) away. It has a mass of about 0.857 ± 0.039 M☉. It is the host of two planets, HAT-P-17b and HAT-P-17c, both discovered in 2010. A search for a binary companion star using adaptive optics at the MMT Observatory was negative. A candidate companion was detected by a spectroscopic search of high-resolution K band infrared spectra taken at the Keck observatory.
HD 179070, also known as Kepler-21, is a F-type subgiant star 354 light-years away in the constellation Lyra. A transiting exoplanet was discovered orbiting this star by the Kepler spacecraft. At a magnitude of 8.25 this was the brightest star observed by Kepler to host a validated planet until the discovery of an exoplanet orbiting HD 212657 in 2018.
K2-19 is an early K-type or late G-type main sequence star that is magnetically active, and has a light curve that exhibits variations in brightness of ~1%. It is located approximately 976 light-years away in the constellation Virgo. Three confirmed transiting exoplanets are known to orbit this star.
HAT-P-36, also referred to as Tuiren is a 12th magnitude G-type main-sequence star estimated to be approximately 958 light-years away from Earth in the constellation Canes Venatici. HAT-P-36 is too faint to be seen with the naked eye, but it is possible to view it with binoculars or a small telescope. In 2012 a hot Jupiter-type exoplanet was discovered orbiting HAT-P-36 with an orbital period of about 1.3 Earth days. In December 2019, HAT-P-36 was named Tuiren and its planetary companion, HAT-P-36b, was named Bran as a result of Ireland's contribution to the 2019 NameExoWorlds campaign. Bran has a mass approximately 1.8 times that of Jupiter and a radius 1.2 times larger.
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.
WASP-58 is a binary star system comprising a G-type main-sequence star and a red dwarf about 955 light-years away. WASP-58 is slightly depleted in heavy elements, having 80% of the solar abundance of iron. WASP-58 is much older than the Sun at 12.80+0.20
−2.10 billion years.
HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.
References
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- ↑ Faedi, F.; et al. (2013). "Lucky imaging of transiting planet host stars with LuckyCam". Monthly Notices of the Royal Astronomical Society. 433 (3): 2097–2106. arXiv: 1305.3795 . Bibcode: 2013MNRAS.433.2097F . doi: 10.1093/mnras/stt885 .
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- ↑ Aguilar, David A.; Pulliam, Christine (September 14, 2006). "Strange New Planet Baffles Astronomers" (Press release). Cambridge, Massachusetts: Harvard–Smithsonian Center for Astrophysics . Retrieved November 18, 2016.
- ↑ 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 .
