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Hot Jupiters are a class of gas giant exoplanets that are inferred to be physically similar to Jupiter but that have very short orbital periods. The close proximity to their stars and high surface-atmosphere temperatures resulted in their informal name "hot Jupiters".
The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.
This page describes exoplanet orbital and physical parameters.
A circumbinary planet is a planet that orbits two stars instead of one. The two stars orbit each other in a binary system, while the planet typically orbits farther from the center of the system than either of the two stars. In contrast, circumstellar planets in a binary system have stable orbits around one of the two stars, closer in than the orbital distance of the other star. Studies in 2013 showed that there is a strong hint that a circumbinary planet and its stars originate from a single disk.
Transit-timing variation is a method for detecting exoplanets by observing variations in the timing of a transit. This provides an extremely sensitive method capable of detecting additional planets in the system with masses potentially as small as that of Earth. In tightly packed planetary systems, the gravitational pull of the planets among themselves causes one planet to accelerate and another planet to decelerate along its orbit. The acceleration causes the orbital period of each planet to change. Detecting this effect by measuring the change is known as transit-timing variations. "Timing variation" asks whether the transit occurs with strict periodicity or if there's a variation.
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.
Kepler-32 is an M-type main sequence star located about 1070 light years from Earth, in the constellation of Cygnus. Discovered in January 2012 by the Kepler spacecraft, it shows a 0.58 ± 0.05 solar mass (M☉), a 0.53 ± 0.04 solar radius (R☉), and temperature of 3900.0 K, making it half the mass and radius of the Sun, two-thirds its temperature and 5% its luminosity.
Kepler-23 is a star in the northern constellation of Cygnus, the swan. It is orbited by three known exoplanets. With an apparent visual magnitude of 14.0, this star is too faint to be seen with the naked eye.
Kepler-24 is a star in the northern constellation of Lyra. It is located at the celestial coordinates: Right Ascension 19h 21m 39.0s, Declination +38° 20′ 37″. With an apparent visual magnitude of 15.5, this star is too faint to be seen with the naked eye.
Kepler-91b is a giant planet orbiting Kepler-91, a star slightly more massive than the Sun. Kepler-91 has left the main sequence and is now a red giant branch star.
Kepler-30 is a star in the northern constellation of Lyra. It is located at the celestial coordinates: Right Ascension 19h 01m 08.0747s Declination +38° 56′ 50.219″. With an apparent visual magnitude of 15.5, this star is too faint to be seen with the naked eye. Kepler-30 is exhibiting a strong starspot activity.
Kepler-24b is an exoplanet orbiting the star Kepler-24, located in the constellation Lyra. It was discovered by the Kepler telescope in January 2012. It orbits its parent star at only 0.08 astronomical units away, and at its distance it completes an orbit once every 8.145 days.
Kepler-24c is an exoplanet orbiting the star Kepler-24, located in the constellation Lyra. It was discovered by the Kepler telescope in January 2012. It orbits its parent star at only 0.106 astronomical units away, and at its distance it completes an orbit once every 12.3335 days.
Kepler-13 or KOI-13 is a stellar triple star system consisting of Kepler-13A, around which an orbiting hot Jupiter exoplanet was discovered with the Kepler spacecraft in 2011, and Kepler-13B a common proper motion companion star which has an additional star orbiting it.
Kepler-167 is a K-type main-sequence star located about 1,119 light-years (343 pc) away from the Solar System in the constellation of Cygnus. The star has about 78% the mass and 75% the radius of the Sun, and a temperature of 4,884 K. It hosts a system of four known exoplanets. There is also a companion red dwarf star at a separation of about 700 AU, with an estimated orbital period of over 15,000 years.
References
- 1 2 3 Ford, Eric B.; Fabrycky, Daniel C.; Steffen, Jason H.; Carter, Joshua A.; Fressin, Francois; Holman, Matthew J.; Lissauer, Jack J.; Moorhead, Althea V.; Morehead, Robert C.; Ragozzine, Darin; Rowe, Jason F.; Welsh, William F.; Allen, Christopher; Batalha, Natalie M.; Borucki, William J.; Bryson, Stephen T.; Buchhave, Lars A.; Burke, Christopher J.; Caldwell, Douglas A.; Charbonneau, David; Clarke, Bruce D.; Cochran, William D.; Désert, Jean-Michel; Endl, Michael; Everett, Mark E.; Fischer, Debra A.; Gautier, Thomas N.; Gilliland, Ron L.; Jenkins, Jon M.; et al. (2012). "Transit Timing Observations Fromkepler. Ii. Confirmation of Two Multiplanet Systems Via a Non-Parametric Correlation Analysis". The Astrophysical Journal. 750 (2): 113. arXiv: 1201.5409 . Bibcode:2012ApJ...750..113F. doi:10.1088/0004-637X/750/2/113. S2CID 4528963.
- 1 2 3 4 Van Eylen, Vincent; Albrecht, Simon (2015). "Eccentricity from Transit Photometry: Small Planets in Kepler Multi-Planet Systems Have Low Eccentricities". The Astrophysical Journal. 808 (2): 126. arXiv: 1505.02814 . Bibcode:2015ApJ...808..126V. doi:10.1088/0004-637X/808/2/126. S2CID 14405731.
- 1 2 3 "Kepler-23 c". Extrasolar Planets Encyclopaedia . Retrieved 26 June 2017.
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