Which planet has a mass which is over three hundred times that of the Earth?
"the ""A"" lobe of the lensed quasar. It is predicted that a 3-Earth-mass planet in the lensing galaxy, YGKOW G1, caused the event. This was the first extragalactic planet candidate announced. This, however, is not a repeatable observation, as it was a one-time chance alignment. This predicted planet lies 4 billion light years away. A team of scientists has used gravitational microlensing to come up with a tentative detection of an extragalactic exoplanet in Andromeda, our nearest large galactic neighbor. The lensing pattern fits a star with a smaller companion, PA-99-N2, weighing just around 6.34 times the mass of Jupiter."
"estimated to have a mass approximately 7.5 times that of Earth. Gliese 876 d Gliese 876 d is an exoplanet approximately 15 light-years away in the constellation of Aquarius. The planet was the third planet discovered orbiting the red dwarf Gliese 876. At the time of its discovery, the planet had the lowest mass of any known extrasolar planet apart from the pulsar planets orbiting PSR B1257+12. Due to this low mass, it can be categorized as a super-Earth. The mass of Gliese 876 d from radial velocity has one problem, it is that only a lower limit on the"
"the surface against harmful cosmic rays. Super-Earth A super-Earth is an extrasolar planet with a mass higher than Earth's, but substantially below those of the Solar System's ice giants, Uranus and Neptune, which are 15 and 17 times Earth's, respectively. The term ""super-Earth"" refers only to the mass of the planet, and so does not imply anything about the surface conditions or habitability. The alternative term ""gas dwarfs"" may be more accurate for those at the higher end of the mass scale, as suggested by MIT professor Sara Seager, although ""mini-Neptunes"" is a more common term. In general, super-Earths are"
"which is about twice the mass of the Moon. The most massive planet listed on the NASA Exoplanet Archive is HR 2562 b, about 30 times the mass of Jupiter, although according to some definitions of a planet, it is too massive to be a planet and may be a brown dwarf instead. There are planets that are so near to their star that they take only a few hours to orbit and there are others so far away that they take thousands of years to orbit. Some are so far out that it is difficult to tell whether they"
"outer planets and extrasolar planets. It may also be used to describe the masses of brown dwarfs, as this unit provides a convenient scale for comparison. The current best known value for the mass of Jupiter can be expressed as : which is about as massive than the sun (about ): in scientific notation, Compared to the mass of Earth, Jupiter is 318 times more massive. Jupiter's mass is 2.5 times that of all the other planets in the Solar System combined—this is so massive that its barycenter with the Sun lies beyond the Sun's surface at 1.068 solar radii"
"Earth's radius, slightly larger than that of the planet Jupiter. However, it is up to 10 times more massive (about 3,180 Earth masses), based on observations of its candidate moon. This puts it just below the deuterium-fusing limit, which is around 13 Jupiter masses. Any more massive and Kepler-1625b would be a brown dwarf. Because of this high mass and radius, the planet likely has a very strong gravitational pull, with a surface gravity calculated to be up to 22.08 times that of Earth. It is also very dense at up to 10.15 g/cm. Unlike the gas giants in our"
"TRAPPIST-1c TRAPPIST-1c, also designated as 2MASS J23062928-0502285 c, is a mainly rocky, Venus-like exoplanet orbiting around the ultracool dwarf star TRAPPIST-1 approximately 40 light-years away from Earth in the constellation Aquarius. It is the most massive and third largest planet of the system, with about 116% the mass and 110% the radius of Earth. Its density indicates a primarily rocky composition with a very thick Venus-like atmosphere, although it is expected to be thinner than that of TRAPPIST-1b. TRAPPIST-1c was observed with the transit method, which enabled scientists to calculate its radius. Transit-timing variations and computer simulations were able to"
"Super-Earth A super-Earth is an extrasolar planet with a mass higher than Earth's, but substantially below those of the Solar System's ice giants, Uranus and Neptune, which are 15 and 17 times Earth's, respectively. The term ""super-Earth"" refers only to the mass of the planet, and so does not imply anything about the surface conditions or habitability. The alternative term ""gas dwarfs"" may be more accurate for those at the higher end of the mass scale, as suggested by MIT professor Sara Seager, although ""mini-Neptunes"" is a more common term. In general, super-Earths are defined by their masses, and the"
"a mass of about 4.5 times that of Earth and orbits its host star every three days. In 2017, it was found that the planet likely hosts an atmosphere. HD 219134 b is a super-Earth, an exoplanet with a radius and mass bigger than Earth, but smaller than that of the ice giants Neptune and Uranus. Using both the radial velocity and transit method, both its mass and radius have been well determined, allowing for accurate modelling of the planet's composition. HD 219134 b has a radius of 1.602 and a mass of 4.74 , giving it a density of"
"least nine times the mass of the Earth, and so may be a Neptune-like planet. But until astronomers can determine the orbital inclination or directly image the planet, there is no way to know for certain its actual mass. The second companion, HD 96700 c, is orbiting at roughly the same distance as Mercury from the Sun, with a semimajor axis of 0.42 AU and a period of around 103 days. It may have a relatively high eccentricity of 0.4. This object has at least 13 times the mass of the Earth. HD 96700 HD 96700 is the ""Henry Draper"
"now termed ice giants. Jupiter's mass is 2.5 times that of all the other planets in the Solar System combined—this is so massive that its barycenter with the Sun lies above the Sun's surface at 1.068 solar radii from the Sun's center. Jupiter is much larger than Earth and considerably less dense: its volume is that of about 1,321 Earths, but it is only 318 times as massive. Jupiter's radius is about 1/10 the radius of the Sun, and its mass is 0.001 times the mass of the Sun, so the densities of the two bodies are similar. A ""Jupiter"
"determine the mass, density, and gravity of the planet. TRAPPIST-1c is the third-largest planet of the TRAPPIST-1 system, with a radius of 1.095 . It is also the most massive of the system as well, with a mass of 1.156 , slightly higher than that of the next most massive, TRAPPIST-1g. Despite its Earth-like mass and radius, TRAPPIST-1c has a lower density (4.89 g/cm) and gravity (0.966g) than Earth. This is consistent with a rock-based composition and a thick, Venus-like atmosphere of water vapor, similar to TRAPPIST-1b. TRAPPIST-1c's atmosphere is expected to be thinner than that of its inner sibling,"
"HD 122430 b HD 122430 b is a giant planet orbiting around the giant star HD 122430. It has a mass at least 3.71 times that of Jupiter. This planet located at a distance of 1.02 astronomical units away from its star, which is very similar to the Earth’s distance from the Sun. Despite of this, the higher luminosity of the star implies it is heated much more strongly than the Earth is. Its orbit is highly eccentric, around 68%. At periastron, the orbital distance from its parent star is 0.33 AU. At apastron, the distance is 1.71 AU. If"
"and mass to Earth, with a radius of 1.13 and a mass of 1.66 . It is slightly denser than Earth with 30% more surface gravity, meaning it has a rocky composition. Despite its physical similarities to Earth, it is considered too hot to be habitable, getting 19 times more sunlight due to its 1.6 day orbital period. In April 2017, it was revealed that the planet has an atmosphere, potentially rich in water vapor and methane. Gliese 1132 c was reported by Bonfils et al. using the HARPS spectrograph on the ESO 3.6 m Telescope at the La Silla"
"XO-3b XO-3b is an exoplanet with about 11.79 times the mass of Jupiter, and an orbit around its parent star in about 3.2 days. The radius of this object is 1.217 times that of Jupiter. Astronomers announced their discovery on May 30, 2007, at the American Astronomical Society in Honolulu, Hawaii. Its discovery is attributed to the combined effort of amateur and professional astronomers working together on the XO Project using a telescope located on the Haleakala summit in Hawaii. Dubbed an ""oddball"" planet, the planet stands out from over 350 other extrasolar planets as the most massive planet found"
"this planet were in the Solar System, its orbit would range from just within Mercury’s orbit to just beyond Mars’s orbit. In Spain, Setiawan discovered this planet in 2003, using the radial velocity method. HD 122430 b HD 122430 b is a giant planet orbiting around the giant star HD 122430. It has a mass at least 3.71 times that of Jupiter. This planet located at a distance of 1.02 astronomical units away from its star, which is very similar to the Earth’s distance from the Sun. Despite of this, the higher luminosity of the star implies it is heated"
"a Subgiant star. Kepler-277c Kepler-277c (also known by its Kepler Objects of Interest designation KOI-1215.02) is the third most massive and second-largest rocky planet ever discovered, with a mass about 64 times that of Earth. Discovered in 2014 by the Kepler Space Telescope, Kepler-277c is a Neptune-sized exoplanet with a very high mass and density for an object of its radius, suggesting a composition made mainly of rock with some amounts of water. Along with its sister planet, Kepler-277b, the planet's mass was determined using transit-timing variations (TTVs). Kepler-277c was detected using the transit method and TTVs, allowing for both"
"Kepler-277c Kepler-277c (also known by its Kepler Objects of Interest designation KOI-1215.02) is the third most massive and second-largest rocky planet ever discovered, with a mass about 64 times that of Earth. Discovered in 2014 by the Kepler Space Telescope, Kepler-277c is a Neptune-sized exoplanet with a very high mass and density for an object of its radius, suggesting a composition made mainly of rock with some amounts of water. Along with its sister planet, Kepler-277b, the planet's mass was determined using transit-timing variations (TTVs). Kepler-277c was detected using the transit method and TTVs, allowing for both its mass and"
"is about , but since the planet is so massive, the greenhouse effect may be even higher. At twice the GE of Earth, LHS 1140 b would have a comfortable surface temperature of . In addition, the host star is so inactive that atmospheric erosion will not be very high, which would allow the planet to warm up. LHS 1140 b LHS 1140 b is a massive, dense rocky planet orbiting within the conservative habitable zone of the red dwarf LHS 1140. Discovered in 2017 by the MEarth Project, LHS 1140 b is nearly 7 times the mass of Earth"
"HD 37605 b HD 37605 b is an extrasolar planet that has nearly three times more mass than Jupiter. It orbits close to the star, taking 54 days to revolve around the parent star HD 37605. Its orbit is highly eccentric, around 74%. Distance from HD 37605 ranges from 0.069 to 0.453 astronomical units. It is the first planet found by Hobby-Eberly Telescope (HET) in July 2004. In a simulation, HD 37605 b's orbit ""sweeps clean"" most test particles within 0.5 AU; leaving only asteroids ""in low-eccentricity orbits near the known planet’s apastron distance, near the 1:2 mean-motion resonance"" with"
"Gliese 3634 b Gliese 3634 b (commonly shortened to GJ 3634 b) is a super-Earth exoplanet in the orbit of the nearby red dwarf Gliese 3634 at approximately 64.5 light-years in constellation Hydra. The planet is approximately eight times the mass of Earth, and orbits its star every two and a half days at a distance of 0.0287 AU. The planet was the first to be discovered by a group of astronomers searching for exoplanets in the orbit of very-low-mass stars after the team reorganized their strategy, choosing to search for targets that they could also confirm using the transit"
"first super-Earth with a mass of a 3 to 4 times that of Earth's found in the potentially habitable zone of its star is Gliese 581g, and its star, Gliese 581, is indeed a red dwarf. Although tidally locked, it is thought possible that at its terminator liquid water may well exist. The planet is thought to have existed for approximately 7 billion years and has a large enough mass to support an atmosphere. Another possibility could come in the far future, when according to computer simulations a red dwarf becomes a blue dwarf as it is exhausting its hydrogen"
"Epsilon Tauri b Epsilon Tauri b (abbreviated ε Tauri b or ε Tau b), also named Amateru, is a super-Jupiter exoplanet orbiting the K-type giant star Epsilon Tauri approximately 155 light-years (47.53 parsecs, or nearly km) away from the Earth in the constellation of Taurus. It orbits the star further out than Earth orbits the Sun. It has moderate eccentricity. The planet orbits one of the four giant stars in the Hyades cluster that is 2.7 times the mass of our Sun, making it the most massive planet-harboring star. This provides evidence that it was an A-type star when it"
"has approximately 3.3 Earth masses and orbits a brown dwarf. It was detected by gravitational microlensing. In June 2008, European researchers announced the discovery of three super-Earths around the star HD 40307, a star that is only slightly less massive than our Sun. The planets have at least the following minimum masses: 4.2, 6.7, and 9.4 times Earth's. The planets were detected by the radial velocity method by the HARPS (High Accuracy Radial Velocity Planet Searcher) in Chile. In addition, the same European research team announced a planet 7.5 times the mass of Earth orbiting the star HD 181433. This"
"mass of at least 1.3 times that of the Earth. Its habitability has not been established, though it is unlikely to be habitable since the planet is subject to stellar wind pressures of more than 2,000 times those experienced by Earth from the solar wind. The discovery of the planet was announced in August 2016 by the European Southern Observatory. The planet was found using the radial velocity method, where periodic Doppler shifts of spectral lines of the host star suggest an orbiting object. From these readings, the radial velocity of the parent star relative to the Earth is varying"
"gas giants Jupiter and Saturn. It has a temperature of , around that of the surface temperature of Venus. It has an estimated mass of around 5.3 and a potential radius of around 9% larger than Jupiter (1.11 , or 12.2 ) based on its mass, since it is more massive than the jovian planet. The planet orbits a (K-type) giant star named HD 240237. It has exhausted the hydrogen supply in its core and is currently fusing helium. The star has a mass of 1.69 and a radius of around 32 . It has a surface temperature of 4361K"
"from Earth with the naked eye. Kepler-11c has a mass of 13.5 M and a radius of 3.15 R, making it over 13.5 times the mass of earth, but approximately 3.15 times its radius. Neptune, in comparison, has a radius approximately 3.9 times that of Earth. With a density of 2.3 grams/cm, Kepler-11c has a mass over double of that of pure water at 0 °C; it is also denser than all the Sun's gas giants, but less dense than any of its rocky planets. Its density is closest to the dwarf planet Pluto. Due in part to its proximity"
"massive enough it could remain in such a state for billions of years despite having lost the atmospheric mass. Solid planets up to thousands of Earth masses may be able to form around massive stars (B-type and O-type stars; 5–120 solar masses), where the protoplanetary disk would contain enough heavy elements. Also, these stars have high UV radiation and winds that could photoevaporate the gas in the disk, leaving just the heavy elements.<ref name=""mass/radius sold""></ref> For comparison, Neptune's mass equals 17 Earth masses, Jupiter has 318 Earth masses, and the 13-Jupiter-mass limit used in the IAU's working definition of an"
"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"
"super-Earth, meaning it has a mass and radius bigger than Earth's, but smaller than that of the ice giants Uranus and Neptune. It has a surface temperature of and a radius of 1.51 . Normally, a planet of this size would be a mini-Neptune, with no solid surface. However, its unusual density when fit for a radius of K2-3d's size would make it an exception to this rule, giving it a solid surface: its density is 11.7±6.7 g/cm, but may be as high as 17.5±6.3 g/cm. This is far greater than the density of iron. Because of this, a composition"
"oscillating eccentricity up to 0.06, and also at 1:3 with oscillating eccentricity up to 0.4. HD 37605 b HD 37605 b is an extrasolar planet that has nearly three times more mass than Jupiter. It orbits close to the star, taking 54 days to revolve around the parent star HD 37605. Its orbit is highly eccentric, around 74%. Distance from HD 37605 ranges from 0.069 to 0.453 astronomical units. It is the first planet found by Hobby-Eberly Telescope (HET) in July 2004. In a simulation, HD 37605 b's orbit ""sweeps clean"" most test particles within 0.5 AU; leaving only asteroids"
"its short period. Kepler-78b is 69% more massive than Earth and 20% larger. Two independent teams were involved in pioneering work to estimate the mass of the planet. The estimates were made possible because Kepler-78b's gravity causes a ""wobble"" in the orbit of the host star. While the method has been used to characterize gas giants, ordinarily it is hard to estimate the mass of Earth-sized exoplanets because their gravity is too weak to produce a visible influence on their stars. In this case, the planet's orbit is so close to its star that its gravitational influence has a detectable"
"with a radius and mass bigger than Earth, but smaller than that of the ice giants Neptune and Uranus. It has an equilibrium temperature of . This is hot enough to melt some types of metal. It has a radius of 1.3 , placing it below the estimated radius of ≤1.6 where it would otherwise be a mini-Neptune with a volatile composition, with no solid surface. However, the mass is currently not known, estimates place an upper limit of <9 , the real mass is expected to be significantly lower than this. The planet orbits a (K-type) star named Kepler-62,"