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List Of Exoplanets Discovered In 2017
This is a List of exoplanets discovered in 2017. 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 , - , BD+03 2562 b , 6.4 , , 481.9 , 1.3 , , style="background:#00FF00", radial vel. , 8540 , 1.14 , 4095 , , - , CoRoT-30 b , 2.90 , 1.009 , 9.06005 , 0.0844 , , style="background:#FFFF00", transit , 3100 , 0.98 , 5650 , , - , CoRoT-31 b , 0.84 , 1.46 , 4.62941 , 0.0586 , , style="background:#FFFF00", transit , 7000 , 1. ... [...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 3323 C
GJ 3323 (also known as LHS 1723) is a nearby single star located in the equatorial constellation Eridanus, about 0.4° to the northwest of the naked eye star Psi Eridani. It is invisible to the naked eye with an apparent visual magnitude 12.20. Parallax measurements give a distance estimate of from the Sun. It is drifting further away with a radial velocity of +42.3 km/s. Roughly 104,000 years ago, the star is believed to have come to within of the Solar System. The stellar classification of GJ 3323 is M4.0Ve, indicating that it is a red dwarf, with emission lines appearing in its spectrum. It is fully convective and a source of X-ray emission. The star has 17% of the Sun's mass, 19% of the radius of the Sun, and just 0.4% of the Sun's luminosity. History of observations The discovery name of this star is LP 656-38, which indicates that its discovery was published between 1963 and 1981 in University of Minnesota, Minneapolis.Dictionary of Nomencl ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 20781 D
HD 20781 d is an extrasolar planet orbiting the K-type main-sequence star HD 20781 away in the southern constellation Fornax. It was discovered in 2011 during a survey for southern exoplanets conducted with HARPS using doppler spectroscopy, the radial velocity variations caused by the gravitational pull of the planet. Its existence was confirmed in another survey during 2017. Naming This planet was initially reported in a 2011 preprint, which referred to it as HD 20781 b. However, the 2017 paper (published in a journal in 2019) that confirmed the planet designated it HD 20781 d, using the b designation for a different, shorter-period planet. Properties Orbit HD 20781 d takes only 29 days to orbit its host star, classifying it as a hot Neptune. However, its orbit is slightly eccentric, carrying it as close as and as far as . HD 20781 d is the second outermost planet in its system after HD 20781 e. Characteristics With a minimum mass 10.6 times that of Earth, it is proba ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 3167
HD 3167 is a single, orange-hued star in the zodiac constellation of Pisces that hosts a system with three exoplanets. The star is too faint to be seen with the naked eye, having an apparent visual magnitude of 8.97. The distance to HD 3167 can be determined from its annual parallax shift of as measured by the Gaia space observatory, yielding a range of 154 light years. It has a relatively high proper motion, traversing the celestial sphere at the rate of per year. Since it was first photographed during the Palomar observatory sky survey in 1953, it had moved over by 2017. The star is moving away from the Earth with an average heliocentric radial velocity of +19.5 km/s. This is an ordinary K-type main-sequence star with a stellar classification of K0 V and no significant variability. The star has 86% of the mass of the Sun and 86% of the Sun's radius. It is a chromospherically inactive star and is radiating 56% of the Sun's luminosity from its ph ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
