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HD 43691 is a G-type star with magnitude +8.03 located approximately 280 light-years away in the constellation Auriga. This yellow star is about to stop thermonuclear hydrogen-fusion in its core and eventually expand to become a red giant.
HAT-P-11, also designated GSC 03561-02092, 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-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.
Kepler-17 is a main-sequence yellow dwarf star that is much more active than our Sun with starspots covering roughly 6% of its surface. Starspots are long-lived, with at least one persisting for 1400 days.
Kepler-19c is an extra-solar planet orbiting the star Kepler-19 approximately 717 light years from Earth.
Kepler-36b is an exoplanet orbiting the star Kepler-36. This planet has the closest conjunction to Kepler-36c every 97 days. Its density is similar to that of iron.
Kepler-68 is a Sun-like main sequence star. It is known to have at least three planets orbiting around it. The outermost planet has a mass similar to Jupiter but orbits within the habitable zone.
Kepler-89 is a star with four confirmed planets. Kepler-89 is a possible wide binary star.
Kepler-65 is a subgiant star slightly more massive than the Sun and has at least four planets.
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 2½ 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, 218 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 that may be transiting their stars.
Kepler-27 is a star in the northern constellation of Cygnus, the swan. It is located at the celestial coordinates: Right Ascension 19h 28m 56.8195s, Declination +41° 05′ 09.141″. With an apparent visual magnitude of 15.855, this star is too faint to be seen with the naked eye.
Kepler-29 is a Sun-like star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 53m 23.6020s, Declination +47° 29′ 28.436″. With an apparent visual magnitude of 15.456, this star is too faint to be seen with the naked eye. It is a solar analog, having a close mass, radius, and temperature as the Sun. Currently the age of the star has not been determined due to its 2780 light-year distance. As of 2016 no Jovian exoplanets of 0.9–1.4 MJ have been found at a distance of 5 AU.
Kepler-421 is a yellow main sequence star, being of spectral class G7V. Orange star of spectral class K9V, projected on sky plane just 1.085″ away, is not physically associated to it. The distance to star KOI-1274 A is approximately 1150 light-years, and to KOI-1274 B is about 1900 light-years.
Kepler-1625 is a 14th-magnitude solar-mass star located in the constellation of Cygnus approximately 8,000 light years away. Its mass is within 5% of that of the Sun, but its radius is approximately 70% larger reflecting its more evolved state. A candidate gas giant exoplanet was detected by the Kepler Mission around the star in 2015, which was later validated as a likely real planet to >99% confidence in 2016. In 2018, the Hunt for Exomoons with Kepler project reported that this exoplanet has evidence for a Neptune-sized exomoon around it, based on observations from NASA’s Kepler Mission. Subsequent observations by the larger Hubble Space Telescope provided compounding evidence for a Neptune-sized satellite, with an on-going debate about the reality of this exomoon candidate.
GJ 9827 is a star in the constellation of Pisces. It is a K-type main-sequence star with an apparent magnitude of 10.250. It is 97 light-years away, based on parallax.
HD 179070 also known as Kepler-21 is a F-type subgiant star. 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.
Kepler-51 is a Sun-like star that is only about 500 million years old. It is orbited by three super-puff planets Kepler-51b, Kepler-51c and Kepler-51d which have the lowest known densities of any exoplanet. The planets are all Jupiter-sized but with masses only a few times Earth's.
HD 175289 is a binary star system. Its primary star, also known as Kepler-410A, is a F-type subgiant star, orbited by the orange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.
References
- 1 2 3 4 5 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.
- 1 2 3 4 5 6 7 8 9 Carter, J. A.; et al. (2012). "Kepler-36: A Pair of Planets with Neighboring Orbits and Dissimilar Densities". Science. 337 (6094): 556–559. arXiv: 1206.4718 . Bibcode:2012Sci...337..556C. doi:10.1126/science.1223269. PMID 22722249. S2CID 40245894.
- 1 2 Vissapragada, Shreyas; et al. (2020). "Diffuser-assisted Infrared Transit Photometry for Four Dynamically Interacting Kepler Systems". The Astronomical Journal. 159 (3). 108. arXiv: 1907.04445 . Bibcode:2020AJ....159..108V. doi:10.3847/1538-3881/ab65c8. S2CID 195874295.
- ↑ "Kepler-36". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-08-07.
- ↑ Bodenheimer, P.; Stevenson, D.; Lissauer, J.; D'Angelo, G. (2018). "New Formation Models for the Kepler-36 System". The Astrophysical Journal. 868 (2): id. 138 (17 pp.). arXiv: 1810.07160 . Bibcode:2018ApJ...868..138B. doi:10.3847/1538-4357/aae928. S2CID 59055335.
