 The exoplanet HD 12661 c (min mass ~1.57 MJ) | |
| Discovery | |
|---|---|
| Discovered by | Fischer et al. [1] |
| Discovery site | California & Carnegie Planet Search  USA |
| Discovery date | April 1, 2003 |
| Radial velocity | |
| Orbital characteristics | |
| 2.56 AU (383,000,000 km) | |
| Eccentricity | 0.031 ± 0.022 |
| 1708 ± 14 d | |
| 2,452,130 ± 330 | |
| 38 | |
| Semi-amplitude | 29.27 ± 0.88 |
| Star | HD 12661 |
HD 12661 c is a giant exoplanet one and a half times the mass of Jupiter orbiting around HD 12661. [1]
HD 12661 is a G-type main sequence star in the northern constellation of Aries. The star is slightly larger and more massive than the Sun, with an estimated age of seven billion years. It has two known extrasolar planets.
HD 37124 is a star in the equatorial constellation of Taurus, positioned about a half degree to the SSW of the bright star Zeta Tauri. The apparent visual magnitude of this star is 7.68, which is too dim to be visible to the naked eye. It is located at a distance of 103 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −23 km/s. Three extrasolar planets have been found to orbit the star.
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 eight years to complete an orbit.
HD 38529 is a binary star approximately 138 light-years away in the constellation of Orion.
692 Hippodamia, provisional designation 1901 HD, is a stony asteroid from the outer region of the asteroid belt, about 45 kilometers in diameter. It was discovered on 5 November 1901, by the German astronomers Max Wolf and August Kopff at Heidelberg Observatory in southern Germany. Nine years later, the body was rediscovered by August Kopff at its apparition in 1910.
HD 40979 is a triple star system in the northern constellation of Auriga. The combined brightness of this group lies below the typical limit of visibility to the naked eye at an apparent visual magnitude of 6.74. It is located at a distance of approximately 108 light years from the Sun based on parallax. The system is receding with a radial velocity of +32 km/s. It has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 0.182″ per year.
HD 217107 b is an extrasolar planet approximately 65 light-years away from Earth in the constellation of Pisces. The planet was discovered orbiting the star HD 217107 approximately every seven days, classifying the planet as a hot Jupiter. Because of the planet's somewhat eccentric orbit, scientists were able to confirm another planet within the system.
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 12661 b is a giant exoplanet two and a half times the mass of Jupiter orbiting around the star HD 12661.
HD 167042 is a 6th magnitude K-type subgiant star located approximately 164 light-years away in Draco constellation. It has mass of 1.88 times that of the Sun and the age is only 1.8 billion years old. When this star was a main sequence, it was white mid to late A-type star based on its mass.
HD 92788 is a star in the equatorial constellation of Sextans. It has a yellow hue but is too dim to be visible to the naked eye, having an apparent visual magnitude of 7.31. The star is located at a distance of 113 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −4.5 km/s. Two planets have been found in orbit around the star.
HD 37124 b is an extrasolar planet approximately 103 light-years away in the constellation of Taurus. The planet was discovered in 1999 orbiting the star HD 37124. Based on its mass, it is most likely that this planet is a Jovian planet.
HD 37124 c is an extrasolar planet approximately 103 light-years away in the constellation of Taurus. The planet was discovered in 2002 orbiting the star HD 37124. The planet is most likely to be a gas giant.
HD 37124 d is an extrasolar planet approximately 103 light-years away in the constellation of Taurus. The planet was discovered in 2005 orbiting the star HD 37124 in a long-period orbit. Based on its mass, it is considered to be a gas giant. An alternative solution to the radial velocities gives a period of 29.92 days and a minimum mass 17% that of Jupiter.
HD 40979 b is an extrasolar planet orbiting the star HD 40979, was detected from the Lick and Keck observatories and photometric observations at Fairborn Observatory reveal low-amplitude brightness variations in HD 40979. It is thought to be a large gas giant planet. It was discovered in 2002 by Debra Fischer.
HD 92788 b is an exoplanet located approximately 113 light-years away in the constellation of Sextans, orbiting the star HD 92788. The semimajor axis of this 3.68 Jupiter mass planet is 0.97 astronomical units, taking approximately 326 days to revolve.
A circumbinary planet is a planet that orbits two stars instead of one. Planets in stable orbits around one of the two stars in a binary are known. New studies showed that there is a strong hint that the planet and stars originate from a single disk.
HD 106906 b is a directly imaged planetary-mass companion and candidate exoplanet orbiting the star HD 106906, in the constellation Crux at about 336 ± 13 light-years (103 ± 4 pc) from Earth. It is estimated to be about eleven times the mass of Jupiter and is located about 738 AU away from its host star. HD 106906 b is rare in astronomy; while its mass estimate is nominally consistent with identifying it as an exoplanet, it appears at a much wider separation from its parent star than thought possible for in-situ formation from a protoplanetary disk.
HD 106906 is a binary star system in the southern constellation of Crux. It is too faint to be visible to the naked eye, having a combined apparent visual magnitude of 7.80. The distance to this system is approximately 337 light years based on parallax, and it is receding from the Sun with a radial velocity of +10 km/s. It is a member of the Lower Centaurus Crux group of the Scorpius–Centaurus OB association of co-moving stars.
HD 136138, or HR 5692, is a binary star system in the Serpens Caput segment of the Serpens constellation. It has a golden hue like the Sun and is dimly visible to the naked eye with an apparent visual magnitude of 5.68; the light contribution from the companion is effectively negligible. This system is located at a distance of approximately 317 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −7.7 km/s and has a proper motion of 23.5 mas yr−1.
Coordinates: 
02h 04m 34.36s, +25° 24′ 53″
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