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HD 114729 is a 7th magnitude star approximately 118 ly (36.1 pc) away in the constellation of Centaurus. Like the Sun (G2V), it is a yellow dwarf. It is about the same mass as the Sun, but twice as luminous. That indicates a much greater age, perhaps over 10 billion years. HD 114729 has a co-moving companion designated HD 114729 B, with the latter having 25.3% of the Sun's mass and a projected separation of 282±10 AU.
HD 217107 is a yellow subgiant star approximately 65 light-years away from Earth in the constellation of Pisces. Its mass is very similar to the Sun's, although it is considerably older. Two planets have been discovered orbiting the star: one is extremely close and completes an orbit every seven days, while the other is much more distant, taking fourteen years to complete an orbit.
HD 28185 is a yellow dwarf star similar to the Sun located 128 light-years away from Earth in the constellation Eridanus. The designation HD 28185 refers to its entry in the Henry Draper catalogue. The star is known to possess one long-period extrasolar planet.
HD 108874 is a yellow dwarf star in the constellation of Coma Berenices. It is 195 light years from Earth and has two extrasolar planets that are possibly in a 9:2 orbital resonance.
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.
HD 217107 c is an extrasolar planet approximately 64 light-years away from Earth in the constellation of Pisces. The planet was the second planet to be discovered orbiting the star HD 217107. HD 217107 c's existence was hypothesized in 1998 due to the eccentricity of the inner planet's orbit and confirmed in 2005 when radial velocity studies of the star indicated another, more distant and massive companion orbiting the star. The planet has an eccentric orbit lasting on order of a decade.
HD 11964 is a binary star system located 110 light-years away from the Sun in the equatorial constellation of Cetus. It is visible in binoculars or a telescope but is too faint to be seen with the naked eye, having an apparent visual magnitude of 7.51. The system is drifting closer to the Sun with a radial velocity of −9 km/s. Two extrasolar planets have been confirmed to orbit the primary.
HD 11964 c is an extrasolar planet approximately 110 light-years away in the constellation of Cetus. The planet was discovered in a close-orbit around the yellow subgiant star HD 11964. The planet has a minimum mass 35 times the mass of Earth and is located in a mildly eccentric orbit which takes almost 38 days to complete. HD 11964 c was a possible planet discovered on the same day as HD 11964 b in 2005. HD 11964 c was first proposed in a paper published in 2007, and finally confirmed with new data presented in a review of multi-planet systems which appeared on the arXiv preprint website in 2008.
HD 17156, named Nushagak by the IAU, is a yellow subgiant star approximately 255 light-years away in the constellation of Cassiopeia. The apparent magnitude is 8.17, which means it is not visible to the naked eye but can be seen with good binoculars. A search for a binary companion star using adaptive optics at the MMT Observatory was negative.
HD 183263 b is an extrasolar planet orbiting the star HD 183263. This planet has a minimum mass of 3.6 times more than Jupiter and takes 625 days to orbit the star. The planet was discovered on January 25, 2005 using multiple Doppler measurements of five nearby FGK main-sequence stars and subgiants obtained during the past 4–6 years at the Keck Observatory in Mauna Kea, Hawaii. These stars, namely, HD 183263, HD 117207, HD 188015, HD 45350, and HD 99492, all exhibit coherent variations in their Doppler shifts consistent with a planet in Keplerian motion, and the results were published in a paper by Geoffrey Marcy et al. Photometric observations were acquired for four of the five host stars with an automatic telescope at Fairborn Observatory. The lack of brightness variations in phase with the radial velocities supports planetary-reflex motion as the cause of the velocity variations. An additional planet in the system was discovered later.
HD 108874 b is a gas giant announced in 2003. The orbit lies in the star's habitable zone. It is expected that any moons orbiting this planet are enriched in carbon, and are thus quite different from the silicate-rich bodies in the Solar System. The planet is possibly in a 4 : 1 orbital resonance with HD 108874 c.
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 syat 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.
HD 102272 b is an extrasolar planet approximately 1,200 light-years away in the constellation of Leo. The planet was discovered orbiting the K-type giant star HD 102272 in 2008. The planet was discovered by the radial velocity method, using the Hobby-Eberly Telescope. Another planet, HD 102272 c, was also discovered orbiting the same star. The discovery was announced in June 2008. HD 102272 b orbits at an average of 0.614 astronomical units away from its star, with a mass at least 5.9 ± 0.2 times that of Jupiter.
HD 102272 c is an extrasolar planet approximately 1,200 light-years away in the constellation of Leo. The planet is orbiting the K-type giant star HD 102272. The planet was discovered by the radial velocity method, using the Hobby-Eberly Telescope. Another planet, HD 102272 b, was also discovered orbiting the same star. Although there is evidence for the existence of this planet, data is insufficient to unambiguously determine its orbit. The discovery was announced in June 2008. It's thought to have at least 2.6 times the mass of Jupiter.
BD-17°63 b, formally named Finlay, is an extrasolar planet 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 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 143361 b is an exoplanet located approximately 224 light-years away in the constellation of Norma, orbiting the 9th magnitude G-type main sequence star HD 143361. This planet has a minimum mass of 3.0 times that of Jupiter. Because the inclination was initially unknown, the true mass was not known. This planet orbits at a distance of 2.0 AU with an orbital eccentricity of 0.18.
HD 48265 is the Henry Draper Catalogue designation for a star in the southern constellation Puppis. It has an apparent visual magnitude of 8.07, which makes it too faint to be seen with the naked eye. Based upon parallax measurements made during the Hipparcos mission, it is located at a distance of roughly 293 light-years from Earth.
HD 143361 is a star in the southern constellation Norma. With an apparent visual magnitude of 9.20, this star is too dim to be seen with the naked eye. It is close enough to the Earth that its distance can be determined using parallax measurements, yielding a value of 224 light-years.
The Magellan Planet Search Program is a ground-based search for extrasolar planets that makes use of the radial velocity method. It began gathering data in December 2002 using the MIKE echelle spectrograph mounted on the 6.5m Magellan II "Clay" telescope located within the Las Campanas Observatory in Chile. In 2010, the program began using the newly commissioned Planet Finder Spectrograph (PFS), an instrument purpose-built for precise radial velocity measurement.
References
- 1 2 3 4 5 Jenkins, J. S.; et al. (2017). "New planetary systems from the Calan–Hertfordshire Extrasolar Planet Search". Monthly Notices of the Royal Astronomical Society. 466 (1): 443–473. arXiv: 1603.09391 . Bibcode:2017MNRAS.466..443J. doi:10.1093/mnras/stw2811.
- ↑ Minniti, Dante; et al. (2009). "Low-Mass Companions for Five Solar-Type Stars From the Magellan Planet Search Program". The Astrophysical Journal. 693 (2): 1424–1430. arXiv: 0810.5348 . Bibcode:2009ApJ...693.1424M. doi:10.1088/0004-637X/693/2/1424. S2CID 119224845.
- ↑ Salas, Javier (17 December 2019). "Rosalía de Castro ya tiene su estrella | Ciencia | EL PAÍS". El País.
