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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.
Kepler-4b, initially known as KOI 7.01, is an extrasolar planet first detected as a transit by the Kepler spacecraft. Its radius and mass are similar to that of Neptune; however, due to its proximity to its host star, it is substantially hotter than any planet in the Solar System. The planet's discovery was announced on January 4, 2010, in Washington, D.C., along with four other planets that were initially detected by the Kepler spacecraft and subsequently confirmed by telescopes at the W.M. Keck Observatory.
A Kepler object of interest (KOI) is a star observed by the Kepler space telescope that is suspected of hosting one or more transiting planets. KOIs come from a master list of 150,000 stars, which itself is generated from the Kepler Input Catalog (KIC). A KOI shows a periodic dimming, indicative of an unseen planet passing between the star and Earth, eclipsing part of the star. However, such an observed dimming is not a guarantee of a transiting planet, because other astronomical objects—such as an eclipsing binary in the background—can mimic a transit signal. For this reason, the majority of KOIs are as yet not confirmed transiting planet systems.
Kepler-39 is an F-type main sequence star located in the constellation Cygnus. It is located about 3,560 light-years away. One known substellar companion orbits it, Kepler-39b.
Kepler-16 is an eclipsing binary star system in the constellation of Cygnus that was targeted by the Kepler spacecraft. Both stars are smaller than the Sun; the primary, Kepler-16A, is a K-type main-sequence star and the secondary, Kepler-16B, is an M-type red dwarf. They are separated by 0.22 AU, and complete an orbit around a common center of mass every 41 days. The system is host to one known extrasolar planet in circumbinary orbit: the Saturn-sized Kepler-16b.
Kepler-18 is a star with almost the same mass as the Sun in the Cygnus constellation.
Kepler-80, also known as KOI-500, is a red dwarf star of the spectral type M0V. This stellar classification places Kepler-80 among the very common, cool, class M stars that are still within their main evolutionary stage, known as the main sequence. Kepler-80, like other red dwarf stars, is smaller than the Sun, and it has both radius, mass, temperatures, and luminosity lower than that of our own star. Kepler-80 is found approximately 1,223 light years from the Solar System, in the stellar constellation Cygnus, also known as the Swan.
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-65 is a subgiant star slightly more massive than the Sun and has at least four planets.
Kepler-69 is a G-type main-sequence star similar to the Sun in the constellation Cygnus, located about 2,430 ly (750 pc) from Earth. On April 18, 2013 it was announced that the star has two planets. Although initial estimates indicated that the terrestrial planet Kepler-69c might be within the star's habitable zone, further analysis showed that the planet very likely is interior to the habitable zone and is far more analogous to Venus than to Earth and thus completely inhospitable.
Kepler-88 is a Sun-like star in the constellation of Lyra, with three confirmed planets. In April 2012, scientists discovered that a Kepler candidate known as KOI-142.01 (Kepler-88b) exhibited very significant transit-timing variations caused by a non-transiting planet. Timing variations were large enough to cause changes to transit durations to Kepler-88b as well. Large transit-timing variations helped to put tight constraints to masses of both planets. The non-transiting planet was further confirmed through the radial velocity method in November 2013.
Kepler-25 is a star in the northern constellation of Lyra. It is slightly larger and more massive than the sun with a luminosity 21⁄2 times that of the sun. With an apparent visual magnitude of 10.6, this star is too faint to be seen with the naked eye.
Kepler-138, also known as KOI-314, is a red dwarf located in the constellation Lyra, 219 light years from Earth. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets transiting their stars.
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-43,formerly known as KOI-135, is a star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 00m 57.8034s, Declination +46° 40′ 05.665″. With an apparent visual magnitude of 13.996, this star is too faint to be seen with the naked eye. The Kepler-43 has a very strong starspot activity.
KOI-256 is a double star located in the constellation Cygnus approximately 575 light-years (176 pc) from Earth. While observations by the Kepler spacecraft suggested the system contained a gas giant exoplanet orbiting a red dwarf, later studies determined that KOI-256 was a binary system composed of the red dwarf orbiting a white dwarf.
Kepler-419 is an F-type main-sequence star located about 3,400 light years from Earth in the constellation Cygnus. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets that may be transiting their stars. In 2012, a potential planetary companion in a very eccentric orbit was detected around this star, but its planetary nature was not confirmed until 12 June 2014, when it was named Kepler-419b. A second planet was announced orbiting further out from the star in the same paper, named Kepler-419c.
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.
References
- 1 2 3 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
- ↑ "Planet Kepler-89 b". Extrasolar Planets Encyclopaedia . Retrieved 26 April 2018.
- 1 2 3 Hirano, Teruyuki; et al. (2012). "Planet-Planet Eclipse and the Rossiter-McLaughlin Effect of a Multiple Transiting System: Joint Analysis of the Subaru Spectroscopy and the Kepler Photometry". The Astrophysical Journal. 759 (2). L36. arXiv: 1209.4362 . Bibcode: 2012ApJ...759L..36H . doi: 10.1088/2041-8205/759/2/L36 .
- ↑ "Kepler-89". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-08-07.
- ↑ Takahashi, Yasuhiro H.; Norio Narita; Teruyuki Hirano; Masayuki Kuzuhara; et al. (2013). "A Discovery of a Candidate Companion to a Transiting System KOI-94: A Direct Imaging Study for a Possibility of a False Positive". arXiv: 1309.2559 [astro-ph.EP].
- ↑ Weiss, Lauren M.; et al. (2013). "The Mass of KOI-94d and a Relation for Planet Radius, Mass, and Incident Flux". The Astrophysical Journal. 768 (1). 14. arXiv: 1303.2150 . Bibcode: 2013ApJ...768...14W . doi: 10.1088/0004-637X/768/1/14 .
- 1 2 Masuda, Kento; et al. (2013). "Characterization of the KOI-94 System with Transit Timing Variation Analysis: Implication for the Planet-Planet Eclipse". The Astrophysical Journal. 778 (2). 185. arXiv: 1310.5771 . Bibcode: 2013ApJ...778..185M . doi: 10.1088/0004-637X/778/2/185 .
- ↑ "First ever discovery of planet-planet eclipse | UTokyo Research". u-tokyo.ac.jp. Archived from the original on 2013-11-04. Retrieved 2014-01-20.
- ↑ Kane, Stephen R. (2019). "Orbital Stability and Precession Effects in the Kepler-89 System". The Astronomical Journal. 158 (2). 72. arXiv: 1906.07193 . Bibcode: 2019AJ....158...72K . doi: 10.3847/1538-3881/ab2a09 .
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