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Theta Persei is a star system 37 light years away from Earth, in the constellation Perseus. It is one of the closest naked-eye stars.
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.
Kepler-17 is a main-sequence yellow dwarf star that is much more active than the Sun with starspots covering roughly 6% of its surface. Starspots are long-lived, with at least one persisting for 1400 days.
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-18 is a star with almost the same mass as the Sun in the Cygnus constellation.
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-65 is a subgiant star slightly more massive than the Sun and has at least four planets.
Kepler-66 is a star with slightly more mass than the Sun in the NGC 6811 open cluster in the Cygnus constellation. It has one confirmed planet, slightly smaller than Neptune, announced in 2013.
Kepler-56 is a red giant in constellation Cygnus roughly 3,060 light-years (940 pc) away with slightly more mass than the Sun.
YBP 1194 is a G-type main-sequence star, class G5V, in the open cluster M67 in the constellation Cancer. It is the best solar twin found to date, having the near exact temperature and mass as the Sun. YBP 1194 has a higher metallicity than the Sun and is 0.5 billion years younger at an age of 4.2 billion years old, but due to the distance, the error bar is high at ±1.6 billion years. On December 19, 2013, it was announced to have an extrasolar planet with a period of 6.9 days and a high eccentricity of 0.24 with a mass of 0.34 MJ. It is about 2,772 light-years from the Sun. It is packed in a small cluster, Messier 67, with a radius of 10 ly, with over 500 other stars. For comparison, the Sun has 17 stars at a distance of 10 ly and about 134 stars at a distance of 20 ly.
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.
HIP 41378 is a star located 346 light-years away in the constellation of Cancer. The star has an apparent magnitude of 8.92. This F-type main sequence dwarf has a mass of 1.15 M☉ and a radius of 1.25 R☉. It has a surface temperature of about 6,251 K.
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.
Kepler-1625b is a super-Jupiter exoplanet orbiting the Sun-like star Kepler-1625 about 2,500 parsecs away. The large gas giant is approximately the same radius as Jupiter and orbits its star every 287.4 days. In 2017, hints of a Neptune-sized exomoon in orbit of the planet was found using photometric observations collected by the Kepler Mission. Further evidence for a Neptunian moon was found the following year using the Hubble Space Telescope, where two independent lines of evidence constrained the mass and radius to be Neptune-like. The mass-signature has been independently recovered by two other teams. However, the radius-signature was independently recovered by one of the teams but not the other. The original discovery team later showed that this latter study appears affected by systematic error sources that may influence their findings.
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, c, and d—which have the lowest known densities of any exoplanet. The planets are all Jupiter-sized but with masses only a few times Earth's.
BD+00 316, also known as WASP-71 since 2019, is an F-class main sequence star about 1200 light-years away. The star is younger than the Sun at approximately 3.6 billion years, yet is already close to leaving the main sequence. BD+00 316 is enriched in heavy elements, having 140% of the solar abundance of iron.
HD 189567 is a G3V star located 58.5 light years away, in the constellation of Pavo. The star HD 189567 is also known as Gliese 776, CD-67 2385, and HR 7644.
Kepler-411 is a binary star system. Its primary star Kepler-411 is a K-type main-sequence star, orbited by the red dwarf star Kepler-411B on a wide orbit, discovered in 2012.
Kepler-635 is an F7V star with an extrasolar planetary system discovered by the Kepler space telescope. The star was first thought to be variable, but later determined to be static.
Kepler-63 is a G-type main-sequence star about 638 light-years away. The star is much younger than the Sun, at 0.21 billion years. Kepler-63 is similar to the Sun in its concentration of heavy elements.
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.
- ↑ McQuillan, A.; Mazeh, T.; Aigrain, S. (2013). "Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators". The Astrophysical Journal Letters. 775 (1). L11. arXiv: 1308.1845 . Bibcode:2013ApJ...775L..11M. doi:10.1088/2041-8205/775/1/L11. S2CID 118557681.
- ↑ "Kepler-67". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 15 January 2018.
- ↑ Maliuk, A.; Budaj, J. (2020), "Spatial distribution of exoplanet candidates based on Kepler and Gaia data", Astronomy & Astrophysics, 635: A191, arXiv: 2002.10823 , Bibcode:2020A&A...635A.191M, doi:10.1051/0004-6361/201936692, S2CID 211296456
- ↑ Meibom, Søren; Torres, Guillermo; Fressin, Francois; Latham, David W.; Rowe, Jason F.; Ciardi, David R.; Bryson, Steven T.; Rogers, Leslie A.; Henze, Christopher E.; Janes, Kenneth; Barnes, Sydney A.; Marcy, Geoffrey W.; Isaacson, Howard; Fischer, Debra A.; Howell, Steve B.; Horch, Elliott P.; Jenkins, Jon M.; Schuler, Simon C.; Crepp, Justin (2013). "The same frequency of planets inside and outside open clusters of stars". Nature. 499 (7456): 55–58. doi:10.1038/nature12279. PMID 23803764. S2CID 4356893.
