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List Of Exoplanets Discovered In 2010
This is a List of exoplanets discovered in 2010. For exoplanets detected only by radial velocity, the mass value is actually a lower limit. (See Minimum mass for more information) {, class="wikitable plainrowheaders sortable" style="width: 100%; font-size: 83%; text-align: center;" !Name !data-sort-type="number", Mass () !data-sort-type="number", Radius () !data-sort-type="number", Period (days) !data-sort-type="number", Semi-major axis (AU) !data-sort-type="number", Temp. ( K) !Discovery method !data-sort-type="number", Distance (ly) !data-sort-type="number", Host star mass () !data-sort-type="number", Host star temp. (K) !Remarks , - , 2MASS J04414489+2301513 b , 7.5 , , , 15.0 , , style="background:#FF6CDA", imaging , 456.63 , 0.02 , , , - , 24 Sextantis b , 1.99 , , 452.8 , 1.333 , , style="background:#00FF00", radial vel. , 235.53 , 1.54 , 5098 , , - , 24 Sextantis c , 0.86 , , 883 , 2.08 , , style="background:#00FF00", radial vel. , 235.53 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Minimum Mass
In astronomy, minimum mass is the lower-bound calculated mass of observed objects such as planets, stars and binary systems, nebulae, and black holes. Minimum mass is a widely cited statistic for extrasolar planets detected by the radial velocity method or Doppler spectroscopy, and is determined using the binary mass function. This method reveals planets by measuring changes in the movement of stars in the line-of-sight, so the real orbital inclinations and true masses of the planets are generally unknown. This is a result of sin ''i'' degeneracy. If inclination ''i'' can be determined, the true mass can be obtained from the calculated minimum mass using the following relationship: M_\text = \frac Exoplanets Orientation of the transit to Earth Most stars will not have their planets lined up and orientated so that they eclipse over the center of the star and give the viewer on earth a perfect transit. It is for this reason that when we often are only able to extrapolate ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gliese 876 E
Gliese 876 e is an exoplanet orbiting the star Gliese 876 in the constellation of Aquarius. It is in a 1:2:4 Laplace resonance with the planets Gliese 876 c and Gliese 876 b: for each orbit of planet e, planet b completes two orbits and planet c completes four. This configuration is the second known example of a Laplace resonance after Jupiter's moons Io, Europa and Ganymede. Its orbit takes 124 days to complete. Gliese 876 e has a mass similar to that of the planet Uranus. Its orbit takes 124 days to complete, or roughly one third of a year. While the orbital period is longer than that of Mercury around the Sun, the lower mass of the host star relative to the Sun means the planet's orbit has a slightly smaller semimajor axis In geometry, the major axis of an ellipse is its longest diameter: a line segment that runs through the center and both foci, with ends at the two most widely separated points of the perimeter. The semi-major axis (major semiaxis) is the lo .... ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 233731
HD 233731, or HAT-P-22, is a suspected multiple star system in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye, having an apparent visual magnitude of 9.732. This system is located at a distance of 267 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +13 km/s. The stellar classification of the primary is G5V, matching an ordinary G-type main-sequence star. The star has a low level of stellar activity with an estimated age of 9 to 12 billion years old. Its metallicity is twice that of the Sun, unusual for its advanced age. HD 233731 has a similar mass and radius as the Sun, and is spinning with a rotation period of 28.7 days. It is radiating 77% of the luminosity of the Sun from its photosphere at an effective temperature of 5314 K. A faint stellar companion (2MASS J10224397+5007504) with a red hue is located at an angular separation of from the pr ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HAT-P-21
HAT-P-21 is a G-type main-sequence star about 910 light-years away. The star has amount of metals similar to solar abundance. The survey in 2015 has failed to detect any stellar companions. The star is rotating rapidly, being spun up by the tides of giant planet on close orbit. Naming In 2019, the HAT-P-21 star received the proper name Mazalaai while its planet HAT-P-21b received the name Bambaruush at an international NameExoWorlds contest. These names refer to the Mongolian name for the endangered Gobi bear subspecies, and the Mongolian term for 'bear cub', respectively. Planetary system In 2010 a transiting hot super-Jovian planet on moderately eccentric orbit was detected. Its equilibrium temperature is 1283 K. The transit-timing variation Transit-timing variation is a method for detecting exoplanets by observing variations in the timing of a transit. This provides an extremely sensitive method capable of detecting additional planets in the system with masses ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HAT-P-20
HAT-P-20 is a K-type main-sequence star about 232 light-years away. The star has a strong starspot Starspots are stellar phenomena, so-named by analogy with sunspots. Spots as small as sunspots have not been detected on other stars, as they would cause undetectably small fluctuations in brightness. The commonly observed starspots are in gene ... activity, and its equatorial plane is misaligned by 36° with the planetary orbit. Although star with a giant planet on close orbit is expected to be spun-up by tidal forces, only weak indications of tidal spin-up were detected. Planetary system In 2010 a transiting hot super-Jovian planet was detected. Its equilibrium temperature is 996 K. References Gemini (constellation) K-type main-sequence stars Planetary systems with one confirmed planet Planetary transit variables J07273995+2420118 {{extrasolar-planet-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HAT-P-19
HAT-P-19 is a K-type main-sequence star about 650 light-years away. The star is old yet metal enriched, having amount of heavy elements 250% of solar abundance. The survey in 2012 have failed to find any stellar companions to HAT-P-19. Planetary system In 2010 a transiting hot Saturn-sized planet was detected. Its equilibrium temperature is 984 K, and it is grey in color. The transit-timing variation Transit-timing variation is a method for detecting exoplanets by observing variations in the timing of a transit. This provides an extremely sensitive method capable of detecting additional planets in the system with masses potentially as small a ... measurements in 2015 and 2018 did not detect additional planets in the system. References Andromeda (constellation) K-type main-sequence stars Planetary systems with one confirmed planet Planetary transit variables J07273995+2420118 {{extrasolar-planet-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HAT-P-18
HAT-P-18 is a K-type main-sequence star about 530 light-years away. The star is very old and has a concentration of heavy elements similar to solar abundance. A survey in 2015 detected very strong starspot activity on HAT-P-18. Planetary system In 2010 a transiting hot Saturn-sized planet was detected. Its equilibrium temperature is 841 K. In 2014, observations utilizing the Rossiter–McLaughlin effect detected an exoplanet, HAT-P-18b, on a retrograde orbit, with an angle between orbital plane of the planet and the parent star equatorial plane equal to 132°. Transit-timing variation measurements in 2015 did not detect additional planets in the system. In 2016, the transmission optical spectra of the planet indicated that the atmosphere is lacking detectable clouds or hazes, and is blue in color due to Rayleigh scattering Rayleigh scattering ( ), named after the 19th-century British physicist Lord Rayleigh (John William Strutt), is the predominantly elastic scat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HAT-P-16
HAT-P-16 is a F-type main-sequence star about 740 light-years away. The star has a concentration of heavy elements slightly higher than solar abundance, and low starspot activity. The survey in 2015 have failed to find any stellar companions to it. The spectral analysis in 2014 have discovered the HAT-P-16 has a carbon to oxygen molar ratio of 0.58, close to Sun`s value of 0.55. Planetary system In 2010 a transiting hot superjovian planet was detected. Transit-timing variation analysis in 2016 have failed to detect an additional planets in the system. In 2011 the observation utilizing a Rossiter–McLaughlin effect was performed, and the orbit of HAT-P-16b was found to be probably aligned with the equatorial plane of the star, misalignment angle equal to 10°. The planet HAT-P-16b equilibrium temperature was found to be equal to 1567 K in 2013. The multiband photometry have failed to find any Rayleigh scattering Rayleigh scattering ( ), named after the 19th-centu ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HAT-P-14b
HAT-P-14b, also known as WASP-27b, is an extrasolar planet located approximately away in the constellation of Hercules, orbiting the 10th magnitude F-type star HAT-P-14. This planet was discovered in 2010 by the HATNet Project using the transit method. It was independently detected by the SuperWASP project. History The planet HAT-P-14b was named Sissi. The name was selected by Austria as part of the NameExoWorlds campaign for the 100th anniversary of the IAU. The planet was named after the character Sissi in the movie '' Sissi'', who is married to Franz. The role is played by the actress Romy Schneider. The star HAT-P-14 is named Franz. Orbit HAT-P-14b is located very close orbit to its star, taking only 4.6 days to complete one orbit. Observations of the Rossiter–McLaughlin effect The Rossiter–McLaughlin effect is a spectroscopic phenomenon observed when an object moves across the face of a star. Description The Rossiter–McLaughlin effect is a spectroscopic p ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
