External links
- "HD 173416 b". Exoplanets. Archived from the original on 2012-03-18. Retrieved 2009-02-01.
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| Discovery | |
|---|---|
| Discovered by | Liu et al. |
| Discovery date | January 10, 2009 |
| radial velocity | |
| Orbital characteristics | |
| Apastron | 1.40 AU (209,000,000 km) |
| Periastron | 0.92 AU (138,000,000 km) |
| 1.16 ± 0.06 AU (173,500,000 ± 9,000,000 km) | |
| Eccentricity | 0.21 ± 0.04 |
| 323.6 ± 2.2 d 0.8860 ± 0.0060 y | |
Average orbital speed | 39.13 |
| 3465.8 ± 8.3 | |
| 254 ± 11 | |
| Star | HD 173416 |
HD 173416 b, also named Wangshu, is an extrasolar planet located approximately 440 light years away in the constellation of Lyra, orbiting the 6th magnitude G-type giant star HD 173416. This is planet has at least 2.7 times the mass of Jupiter and was discovered on January 10, 2009 by Liu et al. HD 173416 b orbits at 1.16 AU from the star. However, despite the fact that the planet orbits 16% further from the star than Earth does from the Sun, it has orbital period of only 323.6 days, compared to 365.25 days for Earth. This inverse relationship is caused by the parent star having twice the mass of the Sun, which increases the strength of its gravitational field. This evidence implies that when this star was on the main sequence, it was an A-type star.
The planet HD 173416 b is named Wangshu (望舒). The name was selected in the NameExoWorlds campaign by Nanjing, during the 100th anniversary of the IAU. Wangshu is the goddess who drives for the Moon and also represents the Moon in Chinese mythology. [1] [2]
Mu Arae, often designated HD 160691, officially named Cervantessur-VAN-teez, is a main sequence G-type star approximately 50 light-years away from the Sun in the constellation of Ara. The star has a planetary system with four known extrasolar planets, three of them with masses comparable with that of Jupiter. Mu Arae c, the innermost, was the first hot Neptune or super-Earth discovered.
HD 83443 is an orange dwarf star approximately 134 light-years away in the constellation of Vela. As of 2000, at least one extrasolar planet has been confirmed to be orbiting the star. The star HD 83443 is named Kalausi. The name was selected in the NameExoWorlds campaign by Kenya, during the 100th anniversary of the IAU. The word Kalausi means a very strong whirling column of wind in the Dholuo language.
HD 149026, also named Ogma, is a yellow subgiant star approximately 250 light-years from the Sun in the constellation of Hercules. An extrasolar planet is believed to orbit the star.
HD 102195 is an orange-hued star in the zodiac constellation of Virgo with a confirmed exoplanet companion. With an apparent visual magnitude of 8.07, the star is too faint to be seen with the naked eye. The distance to HD 102195 can be estimated from its annual parallax shift of 34.06 mas, yielding a separation of 95.8 light years. It is moving further away from the Earth with a heliocentric radial velocity of 1.85 km/s. This is a high proper motion star and a possible member of the η Cha stellar kinematic group.
Upsilon Andromedae d, formally named Majriti, is a super-Jupiter exoplanet orbiting within the habitable zone of the Sun-like star Upsilon Andromedae A, approximately 44 light-years away from Earth in the constellation of Andromeda. Its discovery made it the first multiplanetary system to be discovered around a main-sequence star, and the first such system known in a multiple star system. The exoplanet was found by using the radial velocity method, where periodic Doppler shifts of spectral lines of the host star suggest an orbiting object.
HD 147506 is a magnitude 8.7 F8 dwarf star that is somewhat larger and hotter than the Sun. The star is approximately 419 light years from Earth and is positioned near the keystone of Hercules. It is estimated to be 2 to 3 billion years old. There is one known transiting extrasolar planet.
HD 104985, formally named Tonatiuh, is a solitary star with a exoplanetary companion in the northern constellation of Camelopardalis. The companion is designated HD 104985 b and named Meztli. This star has an apparent visual magnitude of 5.78 and thus is dimly visible to the naked eye under favorable seeing conditions. It is located at a distance of approximately 329 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −20 km/s.
HD 192699 b is an exoplanet located approximately 214 light-years away in the constellation of Aquila, orbiting the star HD 192699. This planet was discovered in April 2007, massing at least 2.5 times the mass of Jupiter (MJ). Despite its orbital distance more than that of Earth, the orbital period is less than a year, because the parent star is more massive than the Sun.
HD 175541 b, also named Kavian, is a jovian planet located approximately 424 light-years away in the constellation of Serpens, orbiting the star HD 175541. This planet was discovered in April 2007. Despite the distance of planet to star slightly more than Earth to the Sun, the period is less than 300 days that orbits in an eccentric orbit, because the parent star is 65% more massive than the Sun.
HD 8574 b is an extrasolar planet discovered in 2001 by a team of European astronomers using Doppler spectroscopy as part of the ELODIE Planet Search Survey, and was published in a paper with five other planets. HD 8574 b is in the orbit of host star HD 8574. The planet is at most two times the mass of Jupiter, orbiting every 227 days at three quarters of the distance between the Earth and Sun. HD 8574 b has a very elliptical orbit, far more than that of Jupiter.
HD 104985 b, also named Meztli, is an extrasolar planet approximately 97 parsecs (317 lys) from the SunThe 198-day period planet orbits the yellow giant star HD 104985 (Tonatiuh) at a distance of 0.78 AU. With a mass 61/3 times Jupiter it is a gas giant.
41 Lyncis, also designated HD 81688 and named Intercrus, is a fifth-magnitude star located in the northern constellation of Ursa Major. An extrasolar planet is thought to be orbiting the star.
HD 205739 b is an extrasolar planet located approximately 350 light-years away.
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 173416, also named Xihe, is an intermediate-mass giant star in the constellation Lyra. It is a 6th magnitude star, relatively bright for its distance of about 440 light years from Earth.
HD 20868 is a star in the southern constellation Fornax. With an apparent visual magnitude of 9.92, it is much too dim to be visible to the naked eye. Parallax measurements give a distance estimate of 156 light years from the Sun. It is drifting further away with a radial velocity of +46.2 km/s, having come to within about 124 ly around 312,000 years ago.
BD−17 63 is a low-mass K type star in the southern constellation Cetus. It is a 9th magnitude star at a distance of 113 light years from Earth.
HD 63765 is an 8th-magnitude G-type main sequence star located approximately 106 light years away in the constellation Carina. This star is smaller, cooler, dimmer, and less massive than the Sun, and has a lower iron content with approximately 69% of the Sun's iron-to-hydrogen ratio. In 2009, a gas giant planet was found in orbit around the star.
HD 212771 b is an extrasolar planet orbiting the G-type star HD 212771 approximately 364 light years away in the constellation Aquarius.
Yanyan, originally named HD 38283 b, is an extrasolar planet, orbiting the 7th magnitude F-type main-sequence star Bubup, 123 light years away in the constellation Mensa. It is a Saturn-like planet orbiting at Earth-like distance, though slightly inwards of its star's habitable zone. Its eccentricity is 0.41, much higher than the Earth's eccentricity of 0.017. The planet's distance ranges from about 0.60 AU and 1.44 AU. This planet takes 363.2 days to orbit the star, just two days less compared to the Earth's orbital period of 365.256366 days. Its mass is one-third that of Jupiter but its size and density are not known. Since inclination is not known, its actual mass is unknown, either slightly greater or much greater than its lower limit.
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