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HD 38529 is a binary star approximately 138 light-years away in the constellation of Orion.
HD 28185 b is an extrasolar planet 128 light-years away from Earth in the constellation of Eridanus. The planet was discovered orbiting the Sun-like star HD 28185 in April 2001 as a part of the CORALIE survey for southern extrasolar planets, and its existence was independently confirmed by the Magellan Planet Search Survey in 2008. HD 28185 b orbits its sun in a circular orbit that is at the inner edge of its star's habitable zone.
MACHO-1997-BLG-41, commonly abbreviated as 97-BLG-41 or MACHO-97-BLG-41, was a gravitational microlensing event located in Sagittarius which occurred in July 1999. The source star is likely a giant or subgiant star of spectral type K located at a distance of around 8 kiloparsecs. The lens star is a binary system approximately 10,000 light-years away in the constellation Sagittarius. The two stars are separated from each other by about 0.9 AU and have an orbital period of around 1.5 years. The most likely mass of the system is about 0.3 times that of the Sun. Star A and star B are both red dwarfs.
HD 17092 is a star in the constellation of Perseus. It has an orange hue but is visible only with binoculars or better equipment, having an apparent visual magnitude of 7.73. The distance to this star is approximately 750 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +5.5 km/s.
HD 118203 is a star with an orbiting exoplanet located in the northern circumpolar constellation of Ursa Major. It has the proper name Liesma, which means flame, and it is the name of a character from the Latvian poem Staburags un Liesma. The name was selected in the NameExoWorlds campaign by Latvia, during the 100th anniversary of the IAU.
HD 13189 is a star with an orbiting companion in the northern constellation of Triangulum constellation. With an apparent visual magnitude of +7.57, it is too faint to be visible to the normal human eye. The distance to this system is approximately 1,590 light years based on parallax measurements, and it is drifting further away with a radial velocity of 25.39 km/s. In 2005, a planetary companion or brown dwarf was announced in orbit around this star.
HD 17092 b is an extrasolar planet located approximately 750 light years away in the constellation Perseus, orbiting the giant star HD 17092.
HD 102272 is a star in the equatorial constellation of Leo. With an apparent visual magnitude of 8.69, it is too faint to be visible to the naked eye. The star is located at a distance of approximately 1,140 light years based on parallax measurements, but is drifting closer to the Sun with a radial velocity of −12 km/s. As of 2008, two extrasolar planets are known to orbit the star.
BD-17°63 b, formally named Finlay, is an exoplanet located approximately 112.5 light-years away in the constellation of Cetus, orbiting the 10th magnitude K-type main sequence star BD−17 63. This planet has a minimum mass of 5.1 MJ and orbits at a distance of 1.34 astronomical units from the star. The distance ranges from 0.62 AU to 2.06 AU, corresponding to the eccentricity of 0.54. One revolution takes about 656 days.
HD 153950 b, also known as Trimobe, is an extrasolar planet located approximately 162 light-years away. This planet was discovered on October 26, 2008 by Moutou et al. using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile.
HD 20868 b is an extrasolar planet located approximately 156 light-years away in the constellation of Fornax, orbiting the 10th magnitude K-type subgiant star HD 20868. This planet has a minimum mass of 1.99 times more than Jupiter and orbits at a distance of 0.947 AU. This planet takes 380.85 days or 12.5 months to revolve around the star with an eccentricity of 0.75, one of the most eccentric of any known extrasolar planets. At periastron, the distance is 0.237 AU and at apastron, the distance is 1.66 AU.
HD 139357 b is a very massive extrasolar planet or brown dwarf located approximately 390 light years away, orbiting the 6th magnitude K-type giant star HD 139357 in the constellation of Draco. The detection occurred on March 20, 2009, which was the first day of spring.
BD−17 63 is a K-type main-sequence star in the southern constellation Cetus. It is a 10th magnitude star at a distance of 113 light-years from Earth. The star is rotating slowly with a negligible level of magnetic activity and an age of over 4 billion years.
HD 240210 is a star in the northern constellation of Cassiopeia. It has an orange hue but is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.33. Parallax measurements provide an estimate of its distance from the Sun as approximately 1,230 light years. It is drifting further away with a radial velocity of +8.6 km/s.
BD+14 4559 b, named Pirx, is an exoplanet orbiting the K-type main sequence star BD+14 4559 about 161 light-years (49 parsecs, or nearly 1.5×1015 km) from Earth in the constellation Pegasus. It orbits its star within the habitable zone at a distance of 0.777 AU, close to that of Venus, but its star is less energetic, thus its habitable zone is closer to it than Earth. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star.
BD+14 4559 is a star with an exoplanetary companion in the northern constellation of Pegasus. During the 2019 NameExoWorlds campaign, the star was named Solaris by Poland after a 1961 science fiction novel about an ocean-covered exoplanet by Polish writer Stanisław Lem. With an apparent visual magnitude of 9.78, the star is too faint to be viewed with the naked eye. The system is located at a distance of 161 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −44 km/s. It is a high proper motion star, traversing the celestial sphere at an angular rate of 0.234″ yr−1.
BD+20 2457 is a 10th-magnitude K-type bright giant star located approximately 4,800 light-years away in the constellation of Leo. The name refers to the Bonner Durchmusterung star catalog. This star contains a very small amount of metals, containing only 10% as enriched with elements heavier than hydrogen and helium as the Sun. On June 10, 2009, two planets were announced to be orbiting the star, with minimum masses 21.4 and 12.5 times the mass of Jupiter and orbital periods of 380 and 622 days for the inner and outer planets, respectively. A dynamical analysis reveals that the proposed system is unstable on astronomically short timescales and so the suggested planetary configuration is unlikely to be correct: further data is needed to determine a physically plausible explanation for the radial velocity variations. This conclusion of a dynamical unstable system depends on the planets masses. A later study found lower masses, which could increase the long-term stability. A study from 2021 using Gaia identified BD+20 2457 as a halo star on a retrograde orbit around the Milky Way with a highly eccentric orbit. The researchers constrain the minimum age and the stars upper mass to ≥8 billion years and ≤1 M☉. This decreases the mass of the planets to 13 MJ and 7 MJ. The chemical abundances also suggest that the star formed from the Milky Ways protodisk. As an alternative it could have formed from debris of the Gaia-Enceladus galaxy as it merged with the Milky Way. If BD+20 2457 formed from the Gaia-Enceladus debris, then the star and its planets could have an extragalactic origin.
HD 28254 is a binary star system located 180 light-years away in the constellation Dorado. The primary component is an 8th magnitude G-type main-sequence star. This star is larger, cooler, brighter, and more massive than the Sun, and its metal content is 2.3 times as much as the Sun. In 2009, a gas giant exoplanet was found in orbit around the star.
BD+48 740 is a giant star suspected of having recently engulfed one of its planets. The star's atmosphere has an overabundance of lithium, a metal that is destroyed by nuclear reactions in stars.
HD 240237 b is a super-Jupiter exoplanet orbiting the K-type giant star HD 240237 about 4,900 light-years (1,500 parsecs, or nearly 4.6×1016 km) away from Earth in the constellation Cassiopeia. It orbits outside of the habitable zone of its star at a distance of 1.9 AU. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star. The planet has a mildly eccentric orbit.
References
- ↑ Niedzielski, A.; et al. (2009). "Substellar-mass Companions to the K-dwarf BD+14 4559 and the K-giants HD 240210 and BD+20 2457". The Astrophysical Journal. 707 (1): 768–777. arXiv: 0906.1804 . Bibcode:2009ApJ...707..768N. doi:10.1088/0004-637X/707/1/768. S2CID 16877069.
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