what is the surface of kepler 22b like
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Kepler-22b Kepler-22b, also known by its Kepler object of interest designation KOI-087.01, is an extrasolar planet orbiting within the empirical habitable zone of the Sun-like star Kepler-22. It is located about from Earth in the constellation of Cygnus. It was discovered by NASA's "Kepler Space Telescope" in December 2011 and was the first known transiting planet to orbit within the habitable zone of a Sun-like star. Kepler-22 is too dim to be seen with the naked eye. Kepler-22b's size is roughly twice that of Earth. Its mass and surface composition are unknown. An Earth-like composition for the planet has been
Kepler-22b
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Kepler-22b Kepler-22b, also known by its Kepler object of interest designation KOI-087.01, is an extrasolar planet orbiting within the empirical habitable zone of the Sun-like star Kepler-22. It is located about from Earth in the constellation of Cygnus. It was discovered by NASA's "Kepler Space Telescope" in December 2011 and was the first known transiting planet to orbit within the habitable zone of a Sun-like star. Kepler-22 is too dim to be seen with the naked eye. Kepler-22b's size is roughly twice that of Earth. Its mass and surface composition are unknown. An Earth-like composition for the planet has been
Kepler-22b
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was announced on 5 December 2011. Kepler-22b is an extrasolar planet orbiting around the star Kepler-22. It is about from Earth in the constellation of Cygnus. It was discovered by the Kepler Space Telescope in December 2011. Kepler-22b's radius is roughly twice that of Earth. Its mass and surface composition remain unknown, with only some very rough estimates established: it has fewer than 124 Earth masses at the 3-sigma confidence limit, and fewer than 36 Earth masses at 1-sigma confidence. The adopted model in Kipping et al. (2013) does not reliably detect the mass (the best fit value is only
Kepler-22b
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of liquid water. Kepler-22b one of the first 54 candidates found by the Kepler telescope and reported is 2.4 times the size of the Earth, with an estimated temperature of 22 °C. It is described as having the potential for surface water, though its composition is currently unknown. Among the 1,235 possible extrasolar planet candidates detected by NASA's planet-hunting Kepler space telescope during its first four months of operation, 54 are orbiting in the parent star's habitable 'Goldilocks' zone where liquid water could exist. Five of these are near Earth-size. On 6 January 2015, NASA announced further observations conducted from
Extraterrestrial liquid water
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average distance from the star and a lower stellar luminosity are consistent with a moderate surface temperature at that distance, if it is assumed that the surface is not subject to extreme greenhouse heating. If Kepler-22b moves in a highly elliptical orbit, as it seems, its surface temperature variance will be very high. Scientists can estimate the possible surface conditions as follows: Recent estimates suggest that Kepler-22b has more than a 95% probability of being located in the empirical habitable zone defined by the recent Venus and early Mars limits (based on estimates of when these planets may have supported
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ruled out. It is likely to have a volatile-rich composition with a liquid or gaseous outer shell. The only parameters of the planet's orbit that are currently available are its orbital period, which is about , and its inclination, which is approximately 90°. Evidence suggests that the planet has a moderate surface temperature, assuming that the surface is not subject to extreme greenhouse heating. In the absence of an atmosphere, its equilibrium temperature (assuming an Earth-like albedo) would be approximately , compared to Earth's The planet's first transit was observed on 12 May 2009. Confirmation of the existence of Kepler-22b
Kepler-22b
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day of scientific operations, on 12 May 2009. The third transit was detected on 15 December 2010. Additional confirmation data was provided by the Spitzer Space Telescope and ground-based observations. Confirmation of the existence of Kepler-22b was announced on 5 December 2011. Kepler-22b Kepler-22b, also known by its Kepler object of interest designation KOI-087.01, is an extrasolar planet orbiting within the empirical habitable zone of the Sun-like star Kepler-22. It is located about from Earth in the constellation of Cygnus. It was discovered by NASA's "Kepler Space Telescope" in December 2011 and was the first known transiting planet to orbit
Kepler-22b
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slightly larger than the 1-sigma error bar), though the mass is below 52.8 Earth masses to 95% confidence. Kepler-22b, dubbed by scientists as a 'waterworld', might be an 'ocean-like' planet. It might also be comparable to the water-rich planet GJ 1214 b although Kepler-22b, unlike GJ 1214 b, is in the habitable zone. An Earth-like composition is ruled out to at least 1-sigma uncertainty by radial velocity measurements of the system. It is thus likely to have a more volatile-rich composition with a liquid or gaseous outer shell; this would make it similar to Kepler-11f, the smallest known gas planet.
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less than a month later, a flood of 41 new exoplanets including 10 super-Earths were announced. On 5 December 2011, the Kepler space telescope discovered its first planet within the habitable zone or "Goldilocks region" of its Sun-like star. Kepler-22b is 2.4 times the radius of the earth and occupies an orbit 15% closer to its star than the Earth to the Sun. This is compensated for however, as the star, with a spectral type G5V is slightly dimmer than the Sun (G2V), and thus the surface temperatures would still allow liquid water on its surface. On 5 December 2011,
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surface pressure of 0.56–1.32 times Earth's. Outside the Solar System, Kepler-11, GJ 1214 b, Kepler-22b, Kepler-62f, Kepler-62e and the planets of TRAPPIST-1 are some of most likely known candidates for an extrasolar ocean planet. Many more such objects are expected to be discovered by "Kepler". Although 70.8% of all Earth's surface is covered in water, water accounts for only 0.05% of Earth's mass. An extraterrestrial ocean's depth would be so deep and dense that even at high temperatures the pressure would turn the water into ice. The immense pressures in the lower regions of these oceans could lead to the
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Natalie Batalha, one of the scientists on the Kepler Space Telescope project, has speculated, "If it is mostly ocean with a small rocky core, it's not beyond the realm of possibility that life could exist in such an ocean". This possibility has spurred SETI to perform research on top candidates for extraterrestrial life. The host star, Kepler-22, is a G-type star that is 3% less massive than the Sun and 2% smaller in volume. It has a surface temperature of compared with the Sun, which has a surface temperature of . The star is about 4 billion years old. In
Kepler-22b
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though little is actually known of their composition. Some scientists speculate Kepler-22b may be an "ocean-like" planet. Models have been proposed for Gliese 581 d that could include surface oceans. Gliese 436 b is speculated to have an ocean of "hot ice". Exomoons orbiting planets, particularly gas giants within their parent star's habitable zone may theoretically have surface oceans. Terrestrial planets will acquire water during their accretion, some of which will be buried in the magma ocean but most of it will go into a steam atmosphere, and when the atmosphere cools it will collapse on to the surface forming
Ocean
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as the radial velocity method, need to be used. While such methods have been performed on the planet since its discovery, these methods have not yet detected an accurate value for the eccentricity of the planet and so (as of March 2012) only an upper limit for the mass of the planet has been set by astronomers. The average distance from Kepler-22b to its host star Kepler-22 is about 15% less than the distance from Earth to the Sun but the luminosity (light output) of Kepler-22 is about 25% less than that of the Sun. This combination of a shorter
Kepler-22b
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likely alternative is the presence of a vapor atmosphere generating from its surface. Kepler-11 and its six-planet system form what NASA considers to be the most compact and flattest planetary system yet discovered. Kepler-11b and Kepler-11c orbit Kepler-11 with a phenomenon called orbital resonance, a gravitational tugging that keeps their orbit stable at a 5.4 ratio. Kepler-11c Kepler-11c is an exoplanet discovered in the orbit of the Sun-like star Kepler-11 by the Kepler spacecraft, a NASA telescope aiming to discover Earth-like planets. It is the second planet from its star, and is most likely a water planet with a thin
Kepler-11c
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habitable conditions), but less than a 5% chance of being located in the conservative habitable zone within the Circumstellar habitable zone, (estimated from a 1D cloud-free radiative-convective model). The Hunt for Exomoons with Kepler (HEK) project has studied the Kepler photometry of the planet, to find any evidence of transit timing and duration variations that may be caused by an orbiting satellite. Such variations were not found, so ruling out the existence of any satellites of Kepler-22b with a mass greater than 0.54 Earth masses. The planet's first transit in front of its host star was observed on Kepler's third
Kepler-22b
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A second paper, published in early 2013, covering the properties of seven of the planet candidates, revealed no moons but allowed the astronomers to constrain the moon-to-planet mass ratios for the planets. A third paper, accepted by the "Astrophysical Journal", analyzed the transit and radial-velocity signals of Kepler-22b, the first and only habitable-zone planet analyzed by the HEK team as of July 2013. As with previous searches, though, no moons were conclusively discovered, constraining the maximum mass of a Kepler-22b moon below 0.54 Earth masses with 95% confidence. Despite the lack of positive results in one-and-a-half years of operation, several
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b, discovered in December 2011 by the "Kepler" space probe, is the first transiting exoplanet discovered around a Sun-like star. With a radius 2.4 times that of Earth, Kepler-22b has been predicted by some to be an ocean planet. Gliese 667 Cc, discovered in 2011 but announced in 2012, is a super-Earth orbiting in the circumstellar habitable zone of Gliese 667 C. Gliese 163 c, discovered in September 2012 in orbit around the red dwarf Gliese 163 is located 49 light years from Earth. The planet has 6.9 Earth masses and 1.8–2.4 Earth radii, and with its close orbit receives
Circumstellar habitable zone
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amongst the first people to study whether planets could form in the Alpha Centauri system. Quintana was a member of the NASA Kepler Mission Team at NASA Ames Research Center from 2006-2017. She worked as a scientific programmer developing the Kepler pipeline for which she was awarded the NASA Software of the Year in 2010. She was part of the team that discovered the first rocky exoplanet Kepler-10b, the first exoplanet to orbit the habitable zone of another star Kepler-22b and the first Earth-sized exoplanet Kepler-20e. In 2014 she led the team that discovered Kepler-186f, an earth-sized exoplanet orbiting in
Elisa Quintana
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World Systems in 1632 to demonstrate that the earth tilted on its axis as it orbited the sun. In his work "Phaenomenon singulare" (1609) Kepler had described what he took to be the transit of Mercury, observed on 29 May 1607. However, after Michael Maestlin pointed out Galileo's work to him, he corrected himself in 1617 in his "Ephemerides", recognising long after the event that what he had seen was sunspots. Welser sent Kepler a copy of Scheiner's first three Apelles letters, and Kepler replied before Galileo, arguing, like him, that Sunspots must be on the surface of the sun
Letters on Sunspots
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It has a spectral type of G5V, while the luminosity class remains undetermined. This star is radiating 79% of the Sun's luminosity from its outer atmosphere at an effective temperature of 5,518 K, giving it the yellow-hued glow of a G-type star. A projected rotational velocity of 0.6 km/s suggests it has a low period of rotation. On December 5, 2011, scientists from the Kepler mission announced that a possible Earthlike world (Kepler-22b) had been discovered orbiting in the star's habitable zone by NASA's Kepler spacecraft. This was significant in that it was the first relatively Earth-sized extrasolar planet (about
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have once more become interested in funding new programs. In 2006 the European Space Agency launched COROT, the first spacecraft dedicated to the search for exoplanets, and in 2009 NASA launched the "Kepler" space observatory for the same purpose. By February 2013 "Kepler" had detected 105 of the confirmed exoplanets, and one of them, Kepler-22b, is potentially habitable. After it was discovered, the SETI Institute resumed the search for an intelligent extraterrestrial civilization, focusing on "Kepler"s candidate planets, with funding from the United States Air Force. Newly discovered planets, particularly ones that are potentially habitable, have enabled SETI and METI
Potential cultural impact of extraterrestrial contact
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of the other detection methods, it can be confirmed by determining if the possibility of a "Kepler" candidate being a real planet is significantly larger than any false-positive scenarios combined. One of the first methods was to see if other telescopes can see the transit as well. The first planet confirmed through this method was Kepler-22b which was also observed with a Spitzer space telescope in addition to analyzing any other false-positive possibilities. Such confirmation is costly, as small planets can generally be detected only with space telescopes. In 2014, a new confirmation method called "validation by multiplicity" was announced.
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still not completely understood; possible sources include the result of impacts with icy bodies, outgassing, mineralization, leakage from hydrous minerals from the lithosphere, and photolysis. For an extrasolar system, an icy body from beyond the frost line could migrate into the habitable zone of its star, creating an ocean planet with seas hundreds of kilometers deep such as GJ 1214 b or Kepler-22b may be. Maintenance of liquid surface water also requires a sufficiently thick atmosphere. Possible origins of terrestrial atmospheres are currently theorised to outgassing, impact degassing and ingassing. Atmospheres are thought to be maintained through similar processes along
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observable from the Solar System. Like the other planets of the system, the planet has a high maximum eccentricity of 0.28, but the lowest in that system. Kepler-20e Kepler-20e is an exoplanet orbiting Kepler-20. The planet is notable as it is the first planet with a smaller radius than Earth found orbiting a Sun-like star. The planet is second-closest to the star after Kepler-20b, and at , it is far too hot to have liquid water on its surface. Along with the other four planets in the system, Kepler-20e was announced on 20 December 2011. With a semimajor axis of
Kepler-20e
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Uranus or Neptune. However, the high density of 9.9 g/cm^3 indicates a rocky composition not too different from Earth's albeit with more iron. Without a rocky surface, life may never be able to develop on a planet. Kepler-1652b has a calculated mass of about 7 times that of Earth, which could help power a strong magnetic field. Red dwarfs like Kepler-1652 can produce very strong flares, much more powerful than what the Sun produces, which could erode away the atmosphere of orbiting planets, compromising their habitability. While not all red dwarfs are this active, a strong magnetic field can still
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density at about 5.5 grams per cubic centimetre, equivalent to that of the Earth and possibly indicative of a rock-iron composition like Earth's. The iron core could build up to 40% of the planet mass. Kepler-78b is most similar to larger high-density, hot exoplanets like Kepler-10b, Kepler-36b and CoRoT-7b. Kepler-78b orbits around the parent star in an 8.5-hour orbit. It reflects 20% to 60% of the starlight it receives. Due to its extremely close solar orbit, about 40 times closer to its star than Mercury is to the Sun, the planet's surface is estimated to be at a temperature of
Kepler-78b
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comparison, the Sun is 4.6 billion years old. The apparent magnitude of Kepler-22 is 11.5, which means it is too dim to be seen with the naked eye. The only parameters of the planet's orbit that are currently available are its orbital period, which is about , and its inclination, which is approximately 90°. From Earth, the planet appears to make a transit across the disk of its host star. It has an eccentricity of 0, meaning its orbit is circular. In order to obtain further information about the details of the planet's orbit, other methods of planetary detection, such
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Given that the stellar flux of Kepler-62e is 20% more than what Earth receives from the Sun, it is possible that the surface temperature of Kepler-62e may be over , enough to trigger a runaway greenhouse effect. Such flux may reduce the habitability factors. In 2009, NASA's Kepler spacecraft was completing observing stars on its photometer, the instrument it uses to detect transit events, in which a planet crosses in front of and dims its host star for a brief and roughly regular period of time. In this last test, Kepler observed stars in the Kepler Input Catalog, including Kepler-62;
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b, which, coincidentally, orbits a stellar remnant, much like the planets of Kepler-70. The host star, Kepler-70 (also formally known as "KOI-55", "2MASS J19452546+4105339" or "KIC 5807616"), is a subdwarf B-type star that has left its red giant stage of its lifetime – according to the Extrasolar Planets Encyclopedia – about ago. It has a surface temperature of 27730 ± 270 K, nearly 6 times as hot as the surface temperature of the Sun, which has a surface temperature of 5778 K. The star has a mass of 0.496 and a radius of 0.203 It is expected to become a
Kepler-70b
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Kepler-20e Kepler-20e is an exoplanet orbiting Kepler-20. The planet is notable as it is the first planet with a smaller radius than Earth found orbiting a Sun-like star. The planet is second-closest to the star after Kepler-20b, and at , it is far too hot to have liquid water on its surface. Along with the other four planets in the system, Kepler-20e was announced on 20 December 2011. With a semimajor axis of 0.0507 AUs, Kepler-20e's orbit has a period of 6.098 days (with an extremely small margin of error). The orbit has an inclination of 87.50°, making its transits
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Kepler-41 Kepler-41 or KOI-196 is a star in the constellation Cygnus. It is a G-type main-sequence star, like the Sun, and it is located about 3,680 light-years (1130 parsecs) away. It is fairly similar to the Sun, with 115% of its mass, a radius of 129% times that of the Sun, and a surface temperature of 5,750 K. There is one known extrasolar planet orbiting Kepler-41. In 2011, the planet Kepler-41b was discovered in orbit around the star. The planet orbits extremely close to Kepler-41, completing an orbit once every 1.86 days. Despite it receiving a high amount of radiation
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region where liquid water could exist on the surface of the planet. As of 2017, with an ESI of 0.85, it is the fifth-most Earth-like planet after Kepler-438b, TRAPPIST-1 d, and two Gliese-designated planets, GJ 3323 b and GJ 273 b, which were both discovered in 2017. Kepler-296e Kepler-296e (also known by its Kepler Object of Interest designation KOI-1422.05) is a confirmed Earth-sized exoplanet orbiting within the habitable zone of Kepler-296. The planet was discovered by NASA's Kepler spacecraft using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star
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determined to some level. It is approximately 2.92 , between the size of Earth and Neptune. At that radius, most planets should be gaseous Mini-Neptunes with no solid surface. However, the mass of Kepler-277b is extremely high for its size. Transit-timing variations indicate a planetary mass of about 87.3 , comparable to Saturn's mass at 95.16 . The planet has a density of approximately 19.3 g/cm and about 10.4 times the surface gravity of Earth. Such a high density for an object of this size implies that, like its sister planet, Kepler-277b is an enormous rock-based planet. It is currently
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radius to be determined to some level. It is approximately 3.36 , close to the size of Neptune. At that radius, most planets should be gaseous Mini-Neptunes with no solid surface. However, the mass of Kepler-277c is extremely high for its size. Transit-timing variations indicate a planetary mass of about 64.2 , close to Saturn's mass at 95.16 . The planet has a density of approximately 9.33 g/cm and about 5.7 times the surface gravity of Earth. Such a high density for an object of this size implies that, like its sister planet, Kepler-277c is an enormous rock-based planet with
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planet because of its radius, which is notable as being the closest to Earth yet: 1.004 . However, although its radius is almost the same as Earth's, its surface conditions are not Earth-like in any way. The equilibrium temperature of Kepler-20f is approximately , too hot to support liquid water on its surface and hot enough to melt some types of metal. But because of its size, it can be expected to have an atmosphere of water vapor. The mass of the planet can be approximated to around 0.66–3.04 , depending on its composition. An Earth-like composition would have its
Kepler-20f
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front of its star is measured, and by a newly utilized computer tool, deep learning, a class of machine learning algorithms. Kepler-90i is a super-Earth exoplanet with a radius of 1.32 , indicating that it is small enough to be rocky. With an Earth-like composition, Kepler-90i would have a mass of about 2.5 . It has an equilibrium temperature of , similar to the average temperature of Venus. The planet orbits a (G-type) star named Kepler-90. The star has a mass of 1.2 and a radius 1.2 . It has a surface temperatures of 6080 K and has an estimated
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exist on a planet's surface. The Planetary Habitability Laboratory (PHL) has given Kepler-1652b a very high Earth Similarity Index (ESI) value of 0.85. Kepler-1652b, like almost all of Kepler's known exoplanets, was found with the transit method, where a planet blocks a tiny fraction of its host star's light when it passed between the star and our line of sight. As a result, the only well-established parameter is its radius. Based on the size of the star and the amount of light blocked, Kepler-1652b has a radius of 1.60 , within the super-Earth range between the sizes of Earth and
Kepler-1652b
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with respect to Earth. Its surface equilibrium temperature is 544 K, over twice the surface equilibrium temperature of Earth and about two-thirds the surface temperature of Venus. Kepler-11f's low density, characteristic of the outer planets of the system, suggests that a hydrogen–helium atmosphere is present on these planets, classifying it as "gas dwarf" due to its small size and mass. The gaseous content of the planet is calculated at a few percent of its total mass, but the envelope accounts for 70-80% of the planet's total volume. Kepler-11f's low density is not shared by the planets Kepler-11b and Kepler-11c because
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explanation currently being that the light represents dust from broken down comets. SETI astronomers are studying the star for signs of extraterrestrial life, because the light signatures appear to mimic the signs of what a massive extraterrestrial superstructure, such as a Dyson sphere, might look like if observed by Kepler. Kepler object of interest A Kepler object of interest (KOI) is a star observed by the "Kepler" spacecraft that is suspected of hosting one or more transiting planets. KOIs come from a master list of 150,000 stars, which itself is generated from the Kepler Input Catalog (KIC). A KOI shows
Kepler object of interest
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other than hydrogen or helium, what astronomers term the metallicity, is approximately the same as in the Sun. It may be older than the Sun, although the margin of error here is relatively large. On December 20, 2011, the Kepler Space Telescope team reported the discovery of a five-planet system containing three small gas giants and the first two Earth-sized extrasolar planets, Kepler-20e (the first known extrasolar planet smaller than Earth orbiting a main-sequence star) and Kepler-20f, orbiting a Sun-like star. Although the planets are Earth-sized, they are not Earth-like in the respect that they are much closer to their
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sunlight that Earth does. Kepler-61b is located in the inner part of the empirical habitable zone, a zone where liquid water could exist with high albedo, relatively low humidity and higher atmospheric pressure. However, the planet is likely tidally locked because of its close distance to its host star. It has an estimated average equilibrium temperature of , very close to that of Earth. If Kepler-61b is Earth-like it is a good candidate for life, because the system is about one billion years old, however because of its radius (2.24 ), it is likely gaseous, with no solid surface. However,
Kepler-61b
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Until January 2015, Kepler-37 was the smallest star to be measured via asteroseismology. Kepler-37b is the closest planet to the Kepler-37. At the time of its discovery in February 2013, it was the smallest known exoplanet. At in diameter, it is slightly larger than the Moon. It orbits Kepler-37 once every 13 days at a distance of about 0.1 astronomical units (AU). Kepler-37b has a rocky surface and is believed to be too small and too close to its star to support water or maintain an atmosphere. Surface temperature is estimated at . Kepler-37c is around three-quarters of the diameter
Kepler-37
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planet, implying it is a low mass, "Mars, Mercury, or even lunar sized bodies with surface gravities of 1/6 to 1/3 that of Earth are to be preferred." K2-22b K2-22b (also known as EPIC 201637175 b) is an exoplanet 801 ly from Earth, rapidly orbiting the red dwarf K2-22 with an orbital period of 9.145872 hours. It has a mass below 445 M and a radius below 2.5 R. The planet was not detected in the K2 photometry. K2 photometry reveals the presence of an anomalous light curve consistent with evaporation of dust from the planet. This dust forms a
K2-22b
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thus, the planet may have an axial tilt (anywhere from 14°–30°) and rotational period somewhat similar to Earth. This can further make the planet more sustainable for habitability, as it would be able to transfer heat to the night side, instead of it being a planet with its surface being half water and half ice. K-type stars like Kepler-62 can live for approximately 20–40 billion years, 2 to 4 times longer than the estimated lifetime of our Sun. The low stellar activity of orange dwarfs like Kepler-62, creates a relatively benign radiation environment for planets orbiting in their habitable zones,
Kepler-62f
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K2-22b K2-22b (also known as EPIC 201637175 b) is an exoplanet 801 ly from Earth, rapidly orbiting the red dwarf K2-22 with an orbital period of 9.145872 hours. It has a mass below 445 M and a radius below 2.5 R. The planet was not detected in the K2 photometry. K2 photometry reveals the presence of an anomalous light curve consistent with evaporation of dust from the planet. This dust forms a tail both ahead and behind the planet, similar to some comets in the Solar System. The evaporation of this dust requires a low surface gravity from the host
K2-22b
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of Kepler-39b. The discovery paper was published in a journal on June 6, 2011. Kepler-39b is a Jupiter-like planet or brown dwarf that is eighteen times more massive than Jupiter and 1.22 times Jupiter's size. For a planet of its size, Kepler-39b has a relatively cool equilibrium temperature of with respect to other inflated planets, defying most of the common models explaining inflation at the time of its discovery (including convection and the effect of stellar radiation). Although Kepler-39b and COROT-3b have similar characteristics (in terms of host star and mass), COROT-3b lies on the predicted size of what a
Kepler-39b
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astronomers extrapolate the exoplanet's parameters and prove the existence of Kepler-40b. The discovered planet was the sixth transiting planet to have been discovered in orbit around stars with a radius of more than 1.8 times that of the Sun, after planets including Kepler-5 and Kepler-7. The discovery of Kepler-40b demonstrated that smaller telescopes, such as SOPHIE, are effective when used as follow-ups to space missions like Kepler. The team of astronomers spent what amounted roughly to one night on a 1.93d-meter telescope and gathered all the data needed to establish Kepler-40b's existence and parameters. Kepler-40b was published in the journal
Kepler-40b
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80% of the Sun's luminosity every 242 days at a distance of 0.64 times that of Earth. This is very similar to that of Venus's orbital period and distance in the Solar System. The exoplanet, along with the exoplanets Kepler-62e and Kepler-62f, were announced in the media as being located within the star's "habitable zone", a region where liquid water could exist on the surface of the planet. It was described as being one of the most Earth-like planets, in terms of size and temperature yet found and, according to the scientists, a "prime candidate to host alien life". Due
Kepler-69c
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having a mass of 1.22 , a radius of 1.79 , and a surface temperature of 6210 ± 100 K. The secondary star (Kepler-1647 B), on the other hand, has a mass of 0.975 , a radius of 1.79 , and a surface temperature of 5770 K. In comparison, the Sun has a surface temperature of 5778 K. The binary star system's age is estimated to be about 4.4 billion years old, about 200 million years younger than the Sun. Kepler-1647b is in the habitable zone of the star system. Since the planet is a gas giant, it is unlikely
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radius (4600 km) for an albedo of 0.5. It has a surface temperature of , far hotter than the surface of Venus. The planet orbits a (K-type) star named Kepler-1520. The star has a mass of 0.76 and a radius of 0.71 . It has a temperature of 4677 K and is 4.47 billion years old. In comparison, the Sun is 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 16.7. Therefore, it is too dim to be seen with the naked eye. Kepler-1520b
Kepler-1520b
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exist on the surface of the planet. However it has been found that this planet is subjected to powerful radiation activity from its parent star every 100 days, much more violent storms than the stellar flares emitted by the Sun and which would be capable of sterilizing life on Earth. Researchers at the University of Warwick say that Kepler-438b is not habitable due to the large amount of radiation it receives. The question of what makes a planet habitable is much more complex than having a planet located at the right distance from its host star so that water can
Kepler-438b
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of Kepler-440, a region where liquid water could exist on the surface of the planet. Kepler-440b Kepler-440b (also known by its Kepler Object of Interest designation KOI-4087.01) is a confirmed super-Earth exoplanet orbiting within the habitable zone of Kepler-440, about from Earth. The planet was discovered by NASA's Kepler spacecraft using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. NASA announced the confirmation of the exoplanet on 6 January 2015. Kepler-440b is a super-Earth with a radius 1.86 times that of Earth. The planet orbits Kepler-440
Kepler-440b
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(G-type) star named Kepler-69, orbited by a total of two planets. The star has a mass of 0.81 and a radius of 0.93 . It has a surface temperatures of 5638 K and has an estimated age of around 400 million years, meaning it has probably finished planet formation. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.7. Therefore, Kepler-69 is too dim to be seen with the naked eye. Kepler-69c orbits its host star with about
Kepler-69c
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planet that is substantially larger than what is estimated by "Kepler". This occurs when there are sources of light other than simply the star being transited, such as in a binary system. In cases such as these, there is more surface area producing light than is assumed, so a given transit signal is larger than assumed. Since roughly 34% of stellar systems are binaries, up to 34% of KOI signals could be from planets within binary systems and, consequently, be larger than estimated (assuming planets are as likely to form in binary systems as they are in single star systems).
Kepler object of interest
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stop crossing the second, brighter star in 2018. After that, Kepler-16b will remain undetectable using the transit method until around 2042. Kepler-16b orbits near the outer edge of the habitable zone, but it is probably a gas giant with surface temperatures around . Kepler-16b is a gas giant, an exoplanet that is near the same mass and radius as the planets Jupiter and Saturn. It has a temperature of . The planet has a radius of 0.77 , slightly smaller than Saturn, and has no solid surface. The planet orbits in a circumbinary orbit around a (K-type) and (M-type) binary
Kepler-16b
17895858
paper, who use Kepler-138b. This has led to the unusual situation of having one star with two "b" planets in orbit and two different base-names for the orbiting planets. Kepler-138 is a red dwarf with approximately 57% the mass of and 54% the radius of the Sun. It has a surface temperature of 3871 ± 58 K. In comparison, the Sun has a surface temperature of 5778 K. Kepler-138's apparent magnitude (bright it appears from Earth's perspective) is 12.925, too dim to be seen with the naked eye. All known planets transit the star; this means that all three planets'
Kepler-138
17402610
this does not totally destroy the chances of habitability in the Kepler-61 system. Kepler-61b may well have a substantially large enough Earth-like moon (with the proper atmospheric properties and pressure), capable of supporting surface liquid water, and potentially life. However, such moons do not form naturally, it would have to be captured. For a stable orbit the ratio between the moon's orbital period "P" around its primary and that of the primary around its star "P" must be < 1/9, e.g. if a planet takes 90 days to orbit its star, the maximum stable orbit for a moon of that
Kepler-61b
18516063
water could exist on the surface of the planet. Kepler-296f Kepler-296f (also known by its Kepler Object of Interest designation KOI-1422.04) is a confirmed super-Earth exoplanet orbiting within the habitable zone of Kepler-296. The planet was discovered by NASA's "Kepler" spacecraft using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. NASA announced the discovery of the exoplanet on 26 February 2014. Kepler296f is a super-Earth with a radius 1.79 times that of Earth. The planet orbits Kepler-296 once every 63.3 days. The planet is located within
Kepler-296f
17233940
In comparison, the Sun has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.7. Therefore, Kepler-69 is too dim to be seen with the naked eye. Kepler-69 has two known planets orbiting around it. Kepler-69b is a hot super-Earth-sized exoplanet. Kepler-69c is a super-Earth-sized exoplanet, about 70% larger than Earth. It receives a similar amount of flux from its star as Venus does from the Sun, and is thus a likely candidate for a super-Venus. Kepler-69 Kepler-69 ("KOI-172", "2MASS J19330262+4452080", "KIC 8692861") is a G-type main-sequence star similar to
Kepler-69
16123824
star than Earth, and are hence not near the habitable zone, with expected surface temperatures of and , respectively. The three other Neptune-sized planets in the system, Kepler-20b, Kepler-20c, and Kepler-20d, all orbit similarly close to the star. Kepler-20g is a non-transiting exoplanet orbiting Kepler-20. The masses of e and f are expected masses. Their masses are uncertain as they are too small to detect via radial velocity with current technology. All planets are at small near resonances; proceeding outwards, they are 3:2, 4:2, 2:1, 4:1. Kepler-20 Kepler-20 is a star 929 light-years from Earth in the constellation Lyra with
Kepler-20
16186467
Kepler-70b Kepler-70b (formerly known as its Kepler Object of Interest designation "KOI-55.01"; sometimes listed as KOI-55 b) is an exoplanet discovered orbiting the subdwarf B star (sdB) Kepler-70. It orbits its host along with another planet, Kepler-70c, both of which orbit very close to their host star. Kepler-70b completes one orbit around its star in just 5.76 hours, one of the shortest orbital periods of any exoplanetary system yet discovered, only second to the exoplanet PSR 1719-14 b with a period of 2.2 hours. It is also the hottest known exoplanet as of mid-2017, with a surface temperature of several
Kepler-70b
14168617
Kepler-4 Kepler-4 is a sunlike star located about 1610 light-years away in the constellation Draco. It is in the field of view of the Kepler Mission, a NASA operation purposed with finding Earth-like planets. Kepler-4b, a Neptune-sized planet that orbits extremely close to its star, was discovered in its orbit and made public by the Kepler team on January 4, 2010. Kepler-4b was the first discovery by the Kepler satellite, and its confirmation helped to demonstrate the spacecraft's effectiveness. Kepler-4 is named for the Kepler spacecraft, a NASA telescope tasked with finding Earth-like planets that transit their stars as seen
Kepler-4
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Kepler-11d Kepler-11d is an exoplanet discovered in the orbit of the sun-like star Kepler-11. It is named for the telescope that discovered it, a NASA spacecraft named Kepler that is designed to detect Earth-like planets by measuring small dips in the brightness of their host stars as the planets cross in front. This process, known as the transit method, was used to note the presence of six planets in orbit around Kepler-11, of which Kepler-11d is the third from its star. Kepler-11d orbits Kepler-11 well within the orbit of Mercury approximately every 23 days. The planet is approximately six times
Kepler-11d
15302744
Kepler-11b Kepler-11b is an exoplanet discovered around the star Kepler-11 by the Kepler spacecraft, a NASA-led mission to discover Earth-like planets. Kepler-11b is less than about three times as massive and twice as large as Earth, but it has a lower density (≤ 3 g/cm), and is thus most likely not of Earth-like composition. Kepler-11b is the hottest of the six planets in the Kepler-11 system, and orbits more closely to Kepler-11 than the other planets in the system. Kepler-11b, along with its five counterparts, form the first discovered planetary system with more than three transiting planets—the most densely packed
Kepler-11b
17239335
Kepler-62b Kepler-62b (also known by its Kepler Object of Interest designation "KOI-701.02") is the innermost and the second smallest discovered exoplanet orbiting the star Kepler-62, with a diameter roughly 30% larger than Earth. It was found using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. It is likely to have an equilibrium temperature slightly higher than the surface temperature of Venus (around ), high enough to melt some types of metal. Its stellar flux is 70 ± 9 times Earth's. Kepler-62b is a super-Earth, an exoplanet
Kepler-62b
17986714
five planets discovered around Kepler-186 are all expected to have a solid surface. The smallest one, Kepler-186b, is only 8% larger than Earth, while the largest one, Kepler-186d, is almost 40% larger. The four innermost planets are probably tidally locked, but Kepler-186f is further out, where the star's tidal effects are much weaker, so there may not have been enough time for its spin to slow down that much. Because of the very slow evolution of red dwarf stars, the age of the Kepler-186 system is poorly constrained, although it is likely to be greater than a few billion years.
Kepler-186
10065288
the width of which corresponds to the lifetime of the mode: the faster it decays, the broader is the Lorentzian. All stars with surface convection zones are expected to show solar-like oscillations, including cool main-sequence stars (up to surface temperatures of about 7000K), subgiants and red giants. Because of the small amplitudes of the oscillations, their study has advanced tremendously thanks to space-based missions (mainly COROT and Kepler). Solar-like oscillations have been used, among other things, to precisely determine the masses and radii of planet-hosting stars and thus improve the measurements of the planets' masses and radii. In red giants,
Solar-like oscillations
19669322
has a temperature of . It has a mass of 2.5 and a radius of 0.96 . The planet orbits an (F-type) star named Kepler-419. The star has a mass of 1.39 and a radius 1.75 . It has a surface temperatures of 6430 K and is 2.8 billion years old. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13. It is too dim to be seen with the naked eye. Kepler-419c orbits its host star with
Kepler-419b
16578354
confirmed planets. The designation "b", derive from the order of discovery. The designation of "b" is given to the first planet orbiting a given star, followed by the other lowercase letters of the alphabet. In the case of Kepler-1520, there was only one planet detected, so only the letter b is used. Kepler-1520 is a K-type star that is approximately 76% the mass of and 71% the radius of the Sun. It has a surface temperature of 4677 K and is about 4.47 billion years old. In comparison, the Sun is about 4.6 billion years old and has a surface
Kepler-1520
18918026
its lifetime due to increased volcanic activity on Kepler-452b. This could allow any potential life on the surface to inhabit the planet for another 500–900 million years before the habitable zone is pushed out of Kepler-452b's orbit. In 2009, NASA's Kepler spacecraft was observing stars on its photometer, the instrument it uses to detect transit events, in which a planet crosses in front of and dims its host star for a brief and roughly regular period of time. In this last test, Kepler observed stars in the Kepler Input Catalog, including Kepler-452; the preliminary light curves were sent to the
Kepler-452b
15302753
Kepler-11c Kepler-11c is an exoplanet discovered in the orbit of the Sun-like star Kepler-11 by the Kepler spacecraft, a NASA telescope aiming to discover Earth-like planets. It is the second planet from its star, and is most likely a water planet with a thin hydrogen–helium atmosphere. Kepler-11c orbits Kepler-11 every 10 days, and has an estimated density twice that of pure water. It is estimated to have a mass thirteen times that of Earth and a radius three times that of Earth. Kepler-11c and its five sister planets form the first discovered system with more than three transiting planets. The
Kepler-11c
17115740
Moon. Due to its small size, it is very likely Kepler-37b is a rocky planet with a solid surface. Furthermore, it is too hot to support liquid water on its surface. The planet orbits a (G-type) star similar to the Sun, named Kepler-37, orbited by a total of four planets. The star has a mass of 0.80 and a radius of 0.79 . It has a temperature of 5417 K and is 5.66 billion years old. In comparison, the Sun is 4.6 billion years old and has a temperature of 5778 K. The star's apparent magnitude, or how bright it
Kepler-37b
17641133
"h", and "i" derives from the order of discovery. The designation of "b" is given to the first planet orbiting a given star, followed by the other lowercase letters of the alphabet. In the case of Kepler-90, there are eight planets discovered, so designations up to "i" are used. Kepler-90 is a G-type star that is approximately 120% the mass and radius of the Sun. It has a surface temperature of 6080 K, and an estimated age of around 2 billion years. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K.
Kepler-90
18513148
smaller than that of the ice giants Uranus and Neptune. It has an equilibrium temperature of . It has a radius of 1.34 . Because of its radius, it is likely to be a rocky planet with a solid surface. The mass of the exoplanet is estimated to be 2.34 . The surface gravity on Kepler-442b would be 30% stronger than that of Earth, assuming a rocky composition similar to that of Earth. The planet orbits a (K-type) star named Kepler-442. The star has a mass of 0.61 and a radius of 0.60 . It has a temperature of 4402
Kepler-442b
210210
can produce higher magnification than Galileo's combination of convex and concave lenses. Around 1611, Kepler circulated a manuscript of what would eventually be published (posthumously) as "Somnium" [The Dream]. Part of the purpose of "Somnium" was to describe what practicing astronomy would be like from the perspective of another planet, to show the feasibility of a non-geocentric system. The manuscript, which disappeared after changing hands several times, described a fantastic trip to the moon; it was part allegory, part autobiography, and part treatise on interplanetary travel (and is sometimes described as the first work of science fiction). Years later, a
Johannes Kepler
16748582
naked eye. The binary system is known to host three planets, all larger than Earth with no solid surface. The innermost planet, Kepler-47b, is a gas giant and resides close to its parent stars and therefore is inhospitable to life. It is thought to be smaller than Kepler-47c and is roughly three times the radius of Earth. The second planet, Kepler-47c, is also a gas giant and the outermost planet. It is situated within the habitable zone and its radius is 4 times the Earth's. Although it is assumed Kepler-47c is not capable of harboring life, it is marginally larger
Kepler-47
17115739
Kepler-37b Kepler-37b is an extrasolar planet (exoplanet) orbiting Kepler-37 in the constellation Lyra. it is the smallest planet discovered around a main-sequence star, with a radius slightly greater than that of the Moon. The measurements do not constrain its mass, but masses above a few times that of the Moon give unphysically high densities. Kepler-37b is a sub-Earth, an exoplanet with a radius and mass smaller than Earth. Its surface temperature is . Because of this, it is not expected to have an atmosphere. Its radius is approximately 0.34 (about a diameter of ), about a little larger than the
Kepler-37b
7059477
Operation INHERENT RESOLVE, assisted with the evacuation of US Embassies in Yemen in both San'na and Aden, supported multiple US Ambassador visits to Aden, Yemen, and served as an airborne deterrence force against surface ships delivering lethal weapons to Huthi rebels in Yemen. In the seven-month deployment, the squadron flew more than 3,500 hours and maintained the highest overall aircraft readiness rate of any Aviation Combat Element since deploying with the MV-22B Osprey. VMM-365 Marine Medium Tiltrotor Squadron 365 (VMM-365) is a United States Marine Corps tiltrotor squadron consisting of MV-22B Osprey transport aircraft. The squadron, known as the "Blue
VMM-365
17115743
Jack Lissauer, a scientist at NASA's Ames Research Center, to conjecture that "such little planets are common". Kepler-37b Kepler-37b is an extrasolar planet (exoplanet) orbiting Kepler-37 in the constellation Lyra. it is the smallest planet discovered around a main-sequence star, with a radius slightly greater than that of the Moon. The measurements do not constrain its mass, but masses above a few times that of the Moon give unphysically high densities. Kepler-37b is a sub-Earth, an exoplanet with a radius and mass smaller than Earth. Its surface temperature is . Because of this, it is not expected to have an
Kepler-37b
16222182
Kepler-42 Kepler-42, formerly known as KOI-961, is a red dwarf located in the constellation Cygnus and approximately 131 light years from the Sun. It has three known extrasolar planets, all of which are smaller than Earth in radius, and likely also in mass. Kepler-42's mass is estimated to be 0.13 times that of the Sun, and to have a radius 0.17 times that of the Sun, that is, just 1.7 times that of the gas giant Jupiter. Due to its small radius and hence surface area, the luminosity of Kepler-42 is only 0.24% of that of the Sun. Its metallicity
Kepler-42
14168638
Kepler-6 Kepler-6 is a yellow giant situated in the constellation Cygnus. The star lies within the field of view of the Kepler Mission, which discovered it as part of a NASA-led mission to discover Earth-like planets. The star, which is slightly larger, more metal-rich, slightly cooler, and more massive than the Sun, is orbited by at least one extrasolar planet, a Jupiter-sized planet named Kepler-6b that orbits closely to its star. Kepler-6 was named for the Kepler Mission, a NASA project launched in 2009 that aims to discover Earth-like planets that transit, or cross in front of, their home stars
Kepler-6
18513140
a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 14.467. Therefore, it is too dim to be seen with the naked eye. Kepler-438b orbits its parent star once every 35.2 days. It is likely tidally locked due to its close distance to its star. A search for exomoons by the Hunt for Exomoons with Kepler project around Kepler-438b placed a maximum mass on a hypothetical moon at 29% that of the planet. The planet was announced as orbiting within the habitable zone of Kepler-438, a region where liquid water could
Kepler-438b
15302779
further distance. Kepler-11e, which formed within the first few million years of the star system's formation, has a mass 8.4 times that of Earth's, and radius 4.52 times that of Earth's. With a density of 0.5 grams/cm, Kepler-11e has a density that is half of that of pure water at standard temperature and pressure and slightly less than the density of Saturn. Kepler-11e has a surface equilibrium temperature of 617 K, and is thus has an equilibrium temperature approximately 2.4 times hotter than Earth's. Kepler-11e orbits its star at a mean distance of .194 AU, making it the fourth planet
Kepler-11e
16578352
and is expected to disintegrate in about 100-200 million years. The planet orbits its star in just 15.7 hours, at a distance only two stellar diameters away from the star's surface, and has an estimated effective temperature of about 2255 K. The orbital period of the planet is one of the shortest ever detected in the history of the extrasolar planet search. In 2016, the planet was confirmed as part of a data release by the "Kepler" spacecraft. Prior to Kepler observation, Kepler-1520 had the 2MASS catalogue number 2MASS J19235189+5130170. In the Kepler Input Catalog it has the designation of
Kepler-1520
15228790
and that the planet "will go into every textbook worldwide." Marcy also described Kepler-10b as "a bridge between the gas giant planets we've been finding and the Earth itself." Diana Valencia at the University of Côte d'Azur in Nice, France considered the planet more of a "super-Mercury" than a super-Earth, granted its physical characteristics. Kepler-10b is most noted for its rocky surface. It has a diameter 1.4 times that of the Earth, and a mass of 3.33±0.49 times that of Earth. The density of Kepler-10b is 5.8±0.8 g cm. It orbits its star, Kepler-10, in less than a day, at
Kepler-10b
20267430
Solar System, Kepler-1625b orbits near the habitable zone of its host star. The planet takes 287 days, or about 0.786 years, to orbit Kepler-1625. This places it at 0.811 AU, similar to Venus' distance from the Sun. At this distance Kepler-1625b has an equilibrium temperature of , which is slightly lower than the boiling point of water. However, as the planet has no solid surface, bodies of liquid water are impossible. The exact size of the host star Kepler-1625 is not fully known. The most accepted model puts it at 1.79 solar radii and 1.08 solar masses with a temperature
Kepler-1625b
17878255
super-Earth with a radius 2.15 times that of Earth, and orbits near the inner edge of the habitable zone. It has an eccentric orbit that takes it in and out and thus experiences temperature swings, which may hinder it's habitability. Also because of its radius, it may be a mini-Neptune, without a solid surface. Kepler-61 Kepler-61 is a K-type main-sequence star approximately 1,100 light years from Earth in the constellation Cygnus. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets that may be transiting their stars. On
Kepler-61
15302798
limit, gravitational effects on the other planets would be observed. Nonetheless, tighter constraints were placed on Kepler-11g's mass by formation and evolution calculations, which indicated that the planet mass is not much greater than about 7 M. Its radius is estimated to be 3.33 times that of Earth, somewhat smaller than Neptune's radius. According to formation models, the planet has a gaseous envelope comprising about 10% of its mass. Kepler-11g has an estimated surface equilibrium temperature of 400 K, over 1.5 times (50% higher) that of Earth's equilibrium temperature. Kepler-11g orbits Kepler-11 every 118.37774 days (over 2.5 times that of
Kepler-11g
15321337
"Kepler" followed by a hyphen and an integer number. The associated planet(s) have the same designation, followed by a letter in the order each was discovered. For all 150,000 stars being watched for transits by "Kepler", there are estimates of each star's surface temperature, radius, surface gravity and mass. These quantities are derived from photometric observations taken prior to Kepler's launch at the 1.2 m reflector at Fred Lawrence Whipple Observatory. For KOIs, there is, additionally, data on each transit signal: the depth of the signal, the duration of the signal and the periodicity of the signal (although some signals
Kepler object of interest
18513142
be liquid on its surface: various geophysical and geodynamical aspects, the radiation, and the host stars plasma environment can influence the evolution of planets and life, if it originated. The planet is more likely to resemble a larger and cooler version of Venus. In 2009, NASA's Kepler spacecraft was completing observing stars on its photometer, the instrument it uses to detect transit events, in which a planet crosses in front of and dims its host star for a brief and roughly regular period of time. In this last test, Kepler observed stars in the Kepler Input Catalog, including Kepler-62; the
Kepler-438b
18918022
the planet would be thick and misty, covering much of the surface as viewed from space. The planet takes 385 Earth days to orbit its star. Its radius is 50% bigger than Earth's, and lies within the conservative habitable zone of its parent star. It has an equilibrium temperature of , a little warmer than Earth. The host star, Kepler-452, is a G-type star that is about the same mass of the Sun, only 3.7% more massive and 11% larger. It has a surface temperature of 5757 K, nearly the same as the Sun, which has a surface temperature of
Kepler-452b
16186468
thousand Kelvin. Its density is 5500 kg/m which is not much different from Earth. Kepler-70b is likely a rocky exoplanet with a mass of 0.44 and a radius of 0.76 . It has a surface temperature of several thousand Kelvin, one of the hottest known surface temperatures on any exoplanet. While the precise temperature is not known, it is expected to be hotter than the surface of the Sun. The exoplanet has an orbit period shorter than any exoplanet known to date, with an orbital period of 5.76 hours (345 minutes). This comes in second to the exoplanet PSR 1719-14
Kepler-70b
3480249
zones of Sun-like stars and red dwarfs within the Milky Way. It is estimated that 11 billion of these planets may be orbiting Sun-like stars. The nearest such planet may be away, according to the scientists. On January 6, 2015, NASA announced the 1,000th confirmed exoplanet discovered by the "Kepler" space telescope. Four of the newly confirmed exoplanets were found to orbit within habitable zones of their related stars: three of the four, Kepler-438b, Kepler-442b and Kepler-452b, are almost Earth-size and likely rocky; the fourth, Kepler-440b, is a super-Earth. On May 10, 2016, NASA verified 1,284 new exoplanets found by
Kepler (spacecraft)
19669292
from the fact that the star is the catalogued 419th star discovered by "Kepler" to have confirmed planets. The designation "b" and "c", derive from the order of discovery. The designation of "b" is given to the first planet orbiting a given star, and "c" to the furthest. In the case of Kepler-419, there were two planets detected, so the letters "b" and "c" are used. Kepler-419 is an F-type star that is approximately 139% the mass of and 175% the radius of the Sun. It has a surface temperature of 6430 K and is 2.8 billion years old. In
Kepler-419
15302773
Kepler-11e Kepler-11e is an exoplanet (extrasolar planet) discovered in the orbit of the sunlike star Kepler-11. It is the fourth of six planets around Kepler-11 discovered by NASA's Kepler spacecraft. Kepler-11e was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. Kepler-11e is most likely a gas giant like Neptune, having a density that is less than that of Saturn, the least dense planet in the Solar System. Its low density can probably be attributed to a large hydrogen and helium atmosphere. Kepler-11e has
Kepler-11e
15302752
of light-element envelope acquired during formation. The observed low density does require the presence of a gaseous envelope though, which was most likely produced via outgassing of hydrogen or evaporation of HO from the condensed core. Kepler-11b and Kepler-11c orbit Kepler-11 with a strong orbital resonance, which gravitationally tugs the planets into stable orbits at a set ratio. The ratio of the resonance between Kepler-11b and c is 5:4. Kepler-11b Kepler-11b is an exoplanet discovered around the star Kepler-11 by the Kepler spacecraft, a NASA-led mission to discover Earth-like planets. Kepler-11b is less than about three times as massive and
Kepler-11b
15843222
confirmed by the Kepler spacecraft after Kepler-10b. Kepler-14b completes an orbit every 6.79 days with a slightly irregular orbit indicated by its orbital eccentricity of 0.035. Kepler-14 Kepler-14 is a binary star system targeted by the Kepler spacecraft. It is host to one known planet: the Jupiter-like Kepler-14b. The star system was identified by Kepler as a possible planetary host, but when imaging revealed that Kepler-14 was a binary star system and not a single star, the confirmation process became protracted. The stars are separated by at least 280 AU, and the stars complete an orbit around a common center
Kepler-14
14168666
Sun at .3871 AU, and takes approximately 87.97 days to complete one orbit. Kepler-7b's eccentricity is assumed to be 0, which would give Kepler-7b a circular orbit by definition. Kepler-7 Kepler-7 is a star located in the constellation Lyra in the field of view of the Kepler Mission, a NASA operation in search of Earth-like planets. It is home to the fourth of the first five planets that Kepler discovered; this planet, a Jupiter-size gas giant named Kepler-7b, is as light as styrofoam. The star itself is more massive than the Sun, and is nearly twice the Sun's radius. It
Kepler-7
15302769
an orbit every 22.68719 days, making it the third planet from Kepler-11. In comparison, planet Mercury orbits the Sun every 87.97 days at a distance of .387 AU. Kepler-11d has an orbital inclination of 89.3°. Thus, Kepler-11d is almost exactly edge on with respect to Earth. The presence of large quantities of hydrogen and helium on Kepler-11d, Kepler-11e, and Kepler-11f suggest that these planets formed within the first few million years of the system's existence, when gas could still be captured from the forming protoplanetary disc. Kepler-11d Kepler-11d is an exoplanet discovered in the orbit of the sun-like star Kepler-11.
Kepler-11d
15302782
Kepler-11f Kepler-11f is an exoplanet (extrasolar planet) discovered in the orbit of the sun-like star Kepler-11 by NASA's Kepler spacecraft, which searches for planets that transit (cross in front of) their host stars. Kepler-11f is the fifth planet from its star, orbiting one quarter of the distance (.25 AU) of the Earth from the Sun every 47 days. It is the furthest of the first five planets in the system. Kepler-11f is the least massive of Kepler-11's six planets, at nearly twice the mass of Earth; it is about 2.6 times the radius of Earth. Along with planets "d" and
Kepler-11f
15302781
20% of it total mass, which account for ≈60% of its radius (or ≈90% of its volume). Kepler-11e Kepler-11e is an exoplanet (extrasolar planet) discovered in the orbit of the sunlike star Kepler-11. It is the fourth of six planets around Kepler-11 discovered by NASA's Kepler spacecraft. Kepler-11e was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. Kepler-11e is most likely a gas giant like Neptune, having a density that is less than that of Saturn, the least dense planet in the Solar
Kepler-11e