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 mass" ( or ) is often used as a unit to describe masses of other objects, particularly extrasolar planets and brown dwarfs.
Mass and size
Jupiter
Jupiter | Mass and size
Jupiter's radius is about 1/10 the radius of the Sun It's mass is 2.5 times that of all the other planets in the Solar System combined. It is the largest in the solar system with a radius being about 1/10 that of the Sun. 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.
what are the alternating dark and light bands in jupiter’s atmosphere called
user
Lightly colored "zones" and relatively dark "belts."
assistant
what is the atmosphere like in jupiter?
user
It is mostly made of molecular hydrogen and helium in roughly solar proportions; other chemical compounds are present only in small amounts and include methane, ammonia, hydrogen sulfide, and water.
assistant
how can you describe its structure vertically?
user
The atmosphere of Jupiter is classified into four layers, by increasing altitude: the troposphere, stratosphere, thermosphere and exosphere
assistant
what is the definition of the first mentioned layer?
user
The troposphere is the lowest layer of Earth's atmosphere, and is also where nearly all weather conditions take place.
assistant
what is the flow here like?
user
The flow of the atmosphere generally moves in a west to east direction.
assistant
are there different types of flow?
user
Yes, Zonal flow, Meridional flow and Atmospheric flow
assistant
how do you explain the first type of flow?
user
A zonal flow regime is the meteorological term meaning that the general flow pattern is west to east along the Earth's latitude lines, with weak shortwaves embedded in the flow
assistant
how is the third type of flow?
user
Sorry. I cannot find the answer based on the context.
assistant
what is the density of the last chemical compound found in the planet?
user
Sorry. I cannot find the answer based on the context.
assistant
what is the size of the aforesaid planet?
user
So, for example, the extrasolar planet HD 209458 b has a mass of , while Kappa Andromedae b has a mass of . Theoretical models indicate that if Jupiter had much more mass than it does at present, it would shrink. For small changes in mass, the radius would not change appreciably, and above about (1.6 Jupiter masses) the interior would become so much more compressed under the increased pressure that its volume would "decrease" despite the increasing amount of matter. As a result, Jupiter is thought to have about as large a diameter as a planet of its composition and evolutionary history can achieve.
Jupiter | Mass and size
The planet has mass of 57% of Jupiter and radius of 97% of Jupiter. The radius is relatively large for its mass, probably due to its intense heating from its nearby star that bloats the planet's atmosphere. The large radius for its mass gives a low density of 820 kg/m.
XO-2Nb | Introduction
For small changes in mass, the radius would not change appreciably, but above about (1.6 Jupiter masses) the interior would become so much more compressed under the increased pressure that its volume would "decrease" despite the increasing amount of matter. As a result, Jupiter is thought to have about as large a diameter as a planet of its composition and evolutionary history can achieve. The process of further shrinkage with increasing mass would continue until appreciable stellar ignition was achieved, as in high-mass brown dwarfs having around 50 Jupiter masses. Jupiter would need to be about 75 times as massive to fuse hydrogen and become a star.
Jupiter mass | Context and implications
When it was first formed, Jupiter was much hotter and was about twice its current diameter.
Jupiter | Mass and size
Jupiter is composed primarily of gaseous and liquid matter. It is the largest planet in the Solar System, with a diameter of at its equator. The average density of Jupiter, 1.326 g/cm, is the second highest of the giant planets, but lower than those of the four terrestrial planets.
Jupiter | Physical characteristics
The object is roughly the volume of Jupiter, but is estimated to have 5–40 Jupiter masses (). This would make it less massive than ε Indi Ba. Planets have a mass of less than about 13 Jupiter masses. Infrared spectra shows the object contains water vapor and methane and has a surface temperature of approximately 480–560 kelvins.
UGPS J0722−0540 | Properties
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 mass" ( or ) is often used as a unit to describe masses of other objects, particularly extrasolar planets and brown dwarfs.
Jupiter | Mass and size
The planet's mass has been estimated to be 8.65 times that of Jupiter, while its diameter, at , is 0.951 times Jupiter's. Its small size, despite the bloating of the planet's atmosphere, is caused by the strong gravity of the planet. This indicates its mean density is twice that of Earth and its surface gravity approximately 24 times that on Earth, almost equal to the Sun. The orbit is very eccentric, ranging from 4.90 million to 15.36 million miles from the star. In addition to heat from its primary star, tidal heating is thought to have played a significant role in this planet's evolution.
HAT-P-2b | Orbit and mass
An example of this may be the exoplanet HAT-P-1b with about half the mass of Jupiter but about 1.38 times larger diameter. Corot-3b, with a mass around 22 Jupiter masses, is predicted to have an average density of 26.4 g/cm, greater than osmium (22.6 g/cm), the densest natural element under standard conditions. Extreme compression of matter inside it causes the high density, because it is likely composed mainly of hydrogen. The surface gravity is also high, over 50 times that of Earth.
Super-Jupiter | Introduction
WASP-17b has a radius between 1.5 and 2 times that of Jupiter and about half the mass. Thus its mean density is between 0.08 and 0.19 g/cm, compared with Jupiter's 1.326 g/cm and Earth's 5.515 g/cm (the density of water is 1 g/cm). The unusually low density is thought to be a consequence of a combination of the planet's orbital eccentricity and its proximity to its parent star (less than one seventh of the distance between Mercury and the Sun), leading to tidal flexing and heating of its interior. The same mechanism is behind the intense volcanic activity of Jupiter's moon Io.
WASP-17b | Physical properties
COROT-9b has a mass of 0.84 times that of Jupiter (M) as determined from HARPS spectroscopy, and has a radius of 1.05 times that of Jupiter (R) as determined from photometry of the transit light curve. This implies that this planet has a density of 96% that of water, and surface gravity 1.93 times that of Earth. A search for rings and satellites around this planet with the Spitzer space telescope was negative.
CoRoT-9b | Mass and size
The process of further shrinkage with increasing mass would continue until appreciable stellar ignition was achieved, as in high-mass brown dwarfs having around 50 Jupiter masses. Although Jupiter would need to be about 75 times as massive to fuse hydrogen and become a star, the smallest red dwarf is only about 30 percent larger in radius than Jupiter. Despite this, Jupiter still radiates more heat than it receives from the Sun; the amount of heat produced inside it is similar to the total solar radiation it receives. This additional heat is generated by the Kelvin–Helmholtz mechanism through contraction. This process causes Jupiter to shrink by about 2 cm each year.
Jupiter | Mass and size
Estimates for the mass, size, and temperature of 2M1207b are still uncertain. Although spectroscopic evidence is consistent with a mass of 8 ± 2 Jupiter masses and a surface temperature of 1600 ± 100 kelvins, theoretical models for such an object predict a luminosity 10 times greater than observed. Because of this, lower estimates for the mass and temperature have been proposed. Alternatively, 2M1207b might be dimmed by a surrounding disk of dust and gas. As an unlikely possibility, Mamajek and Michael Meyer have suggested that the planet is actually much smaller, but is radiating away heat generated by a recent collision.
2M1207b | Properties
The mass is about 0.85 that of Jupiter.
55 Cancri b | Orbit and mass
This planetary object is reported to be about half the mass but slightly larger than the planet Jupiter at 0.467(+0.047, -0.024) M_Jup.
CoRoT-5b | Properties and location
The upper mass limit for planethood is roughly 13 times Jupiter's mass for objects with solar-type isotopic abundance, beyond which it achieves conditions suitable for nuclear fusion. Other than the Sun, no objects of such mass exist in the Solar System; but there are exoplanets of this size. The 13-Jupiter-mass limit is not universally agreed upon and the Extrasolar Planets Encyclopaedia includes objects up to 60 Jupiter masses, and the Exoplanet Data Explorer up to 24 Jupiter masses. The smallest known planet is PSR B1257+12A, one of the first extrasolar planets discovered, which was found in 1992 in orbit around a pulsar.
Planet | Mass
Spectroscopic analysis had shown that the planet had a mass about 0.69 times that of Jupiter. The occurrence of transits allowed astronomers to calculate the planet's radius, which had not been possible for any previously known exoplanet, and it turned out to have a radius some 35% larger than Jupiter's. It had been previously hypothesized that hot Jupiters particularly close to their parent star should exhibit this kind of inflation due to intense heating of their outer atmosphere. Tidal heating due to its orbit's eccentricity, which may have been more eccentric at formation, may also have played a role over the past billion years.
HD 209458 b | Spectroscopic
The planet is a large hot Jupiter, about 1.49 times the radius of Jupiter and approximately 1.03 times as massive, based on ground observations of the star. Its large size is due to its low density combined with the intense heating of its parent star causing the outer layers of the atmosphere to bloat.
CoRoT-1b | Characteristics
If the planet exists, its mass remains unknown, but a lower limit can be estimated based on the orbital displacement of Epsilon Eridani. Only the component of the displacement along the line of sight to Earth is known, which yields a value for the formula "m" sin "i", where "m" is the mass of the planet and "i" is the orbital inclination. Estimates for the value of range from 0.60 Jupiter masses to 1.06 Jupiter masses, which sets the lower limit for the mass of the planet (because the sine function has a maximum value of 1). Taking in the middle of that range at 0.78, and estimating the inclination at 30°, this yields a value of Jupiter masses for the planet's mass.
Epsilon Eridani | Planet b (AEgir)
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 from the Sun's center. Because the mass of Jupiter is so large compared to the other objects in the solar system, the effects of its gravity must be included when calculating satellite trajectories and the precise orbits of other bodies in the solar system, including Earth's moon and even Pluto. Theoretical models indicate that if Jupiter had much more mass than it does at present, its atmosphere would collapse, and the planet would shrink.
Jupiter mass | Context and implications
The majority of Jupiter's mass is hydrogen and helium. These two elements make up more than 87% of the total mass of Jupiter. The total mass of heavy elements other than hydrogen and helium in the planet is between 11 and . The bulk of the hydrogen on Jupiter is solid hydrogen. Evidence suggests that Jupiter contains a central dense core. If so, the mass of the core is predicted to be no larger than about . The exact mass of the core is uncertain due to the relatively poor knowledge of the behavior of solid hydrogen at very high pressures.
Jupiter mass | Mass composition
The planet, designated as HD 17092 b, has a minimum mass of 4.6 Jupiter masses. The mean distance of the planet from the star is more than distance between Earth and the Sun at 1.29 AU, and the eccentricity of the orbit is mild at 0.166.
HD 17092 b | Characteristics
HD 240237 b is a "super-Jupiter", an exoplanet that has a radius and mass larger than that of the 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.
HD 240237 b | Mass, radius and temperature
The planet has a minimum mass of 8.78 Jupiter masses. The true mass, as with the majority of other extrasolar planets discovered by the radial velocity method, is unknown.
Gamma Leonis b | Characteristics
The companion planet HAT-P-6b is a transiting planet discovered on October 15, 2007 by the HATNet Project. The planet's true mass is slightly more than Jupiter at only 5.7%, but the radius is 33% greater, making the planet's density of 0.45 g/cm. Its large size compared to mass comes from the great amount of heat received from the nearby star that expands the planet's atmosphere, categorizing as "hot Jupiter". The orbital period is 3.852985 days and the distance from its star is 0.05235 AU. The inclination of the orbit with respect to the stellar rotation axis is roughly 166º.
HAT-P-6 | Planetary system
The sizes are listed in units of Jupiter radii (, )(71,492 km). All planets listed are larger than two times the size of the largest planet in the Solar System, Jupiter. Some planets that are smaller than have been included for the sake of comparison. A few additional examples with radii lower than 1.7 .
List of largest exoplanets | The List
In 2011, Whitmire and Matese speculated that the hypothesized planet could be up to four times the mass of Jupiter and have a relatively high temperature of approximately , due to residual heat from its formation and Kelvin–Helmholtz heating. It would be insufficiently massive to undergo nuclear fusion reactions in its interior, a process that occurs in objects above roughly 13 Jupiter masses. Although more massive than Jupiter, Tyche would be about Jupiter's size since degenerate pressure causes massive gas giants to increase only in density, not in size, relative to their mass. If Tyche was to be found, it was expected to be found by the end of 2013 and only be 1–2 Jupiter masses.
Tyche (hypothetical planet) | Mass
As of 2016 this limit was increased to 60 Jupiter masses based on a study of mass–density relationships. The Exoplanet Data Explorer includes objects up to 24 Jupiter masses with the advisory: "The 13 Jupiter-mass distinction by the IAU Working Group is physically unmotivated for planets with rocky cores, and observationally problematic due to the sin i ambiguity." The NASA Exoplanet Archive includes objects with a mass (or minimum mass) equal to or less than 30 Jupiter masses. Another criterion for separating planets and brown dwarfs, rather than deuterium fusion, formation process or location, is whether the core pressure is dominated by coulomb pressure or electron degeneracy pressure with the dividing line at around 5 Jupiter masses.
Exoplanet | Alternatives
HD 153950 b is a Jupiter-size exoplanet. The estimated minimum mass is 2.73 times the mass of Jupiter. The planet has been found to orbit its host star every 500 days at a distance of 1.28 AU, which is approximately 28% more of the mean distance between the Sun and the Earth. HD 153950 b has a mildly elliptical orbit, given its orbital eccentricity of 0.34.
HD 153950 b | Mass and orbit
This planetary object is reported to be about 3.3 times the mass of the planet Jupiter and 1.17 times its size with an orbital period of 8.88 days. It is a hot Jupiter with a temperature between 700 and 1000 °C.
CoRoT-6b | Properties and location
PSR J1719−1438 b was, at the time of its August 25, 2011 discovery, the densest planet ever discovered, at nearly 20 times the density of Jupiter (about 23 times the density of water). It is slightly more massive than Jupiter. It is thought to be composed of oxygen and carbon (as opposed to hydrogen and helium, the main components of gas giants like Jupiter and Saturn). The oxygen is most likely on the surface of the planet, with increasingly higher quantities of carbon deeper inside the planet. The intense pressure acting upon the planet suggests that the carbon is crystallized, much like diamond is.
PSR J1719−1438 b | Characteristics
The largest parent bodies must be less than 0.5 km in size. The upper limit on their size was obtained by "New Horizons" spacecraft. The previous upper limit, obtained from HST and "Cassini" observations, was near 4 km. The dust produced in collisions retains approximately the same orbital elements as the parent bodies and slowly spirals in the direction of Jupiter forming the faint (in back-scattered light) innermost part of the main ring and halo ring. The age of the main ring is currently unknown, but it may be the last remnant of a past population of small bodies near Jupiter.
Rings of Jupiter | Origin and age
This was done by observing the Doppler shift in the star's spectrum. Combined with the known inclination of the orbit as determined by the transit observations, this revealed the mass of the planet to be 0.53±0.04 times that of Jupiter.
HAT-P-1b | Orbit and mass
It may also be used to describe the masses of brown dwarfs, as this unit provides a convenient scale for comparison.
Jupiter mass | Introduction
Based on a generic magnitude-to-diameter conversion, measures approximately 14 kilometers in diameter, for an assumed albedo of 0.12 as the median for small Jupiter trojans, and an absolute magnitude of 12.2. , no rotational light curve of has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.
P/2019 LD2 (ATLAS) | Physical characteristics
The largest planet, Jupiter, is 0.09% the mass of the Sun, while the Earth is about three millionths (0.0003%) of the mass of the Sun. Various different conventions are used in the literature to overcome this problem: for example, inverting the ratio so that one quotes the planetary mass in the 'number of planets' it would take to make up one Sun. Here, we have chosen to list all planetary masses in 'microSuns' – that is the mass of the Earth is just over three 'microSuns', or three millionths of the mass of the Sun – unless they are specifically quoted in kilograms.
Planetary mass | Choice of units
The planet's density is extreme for its amount of mass. It implies the existence of an amount of heavy elements with a mass between about 140 and 300M.
CoRoT-13b | Introduction
Both estimates put the planet's density at about 5.5 grams per cubic centimetre, which is 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 | Size, mass and composition
Jupiter mass ( or "M"), is the unit of mass equal to the total mass of the planet Jupiter, . Jupiter mass is used to describe masses of the gas giants, such as the outer planets and extrasolar planets. It is also used in describing brown dwarfs and Neptune-mass planets.
Astronomical system of units | Jupiter mass
The planet is considered a Hot Jupiter, and although it is slightly less massive than Jupiter, it is bloated to nearly twice Jupiter's size. At the time of its discovery, HAT-P-32b had one of the largest radii known amongst extrasolar planets. This phenomenon, which has also been observed in planets like WASP-17b and HAT-P-33b, has shown that something more than temperature is influencing why these planets become so large.
HAT-P-32b | Introduction
Additionally, a small planet in one of the gas giant's Trojan points could survive in a habitable orbit for long periods. The high mass of HD 28185 b, of over six Jupiter masses, actually makes either of these scenarios more likely than if the planet was about Jupiter's mass or less.
HD 28185 b | Characteristics
The Anglo-Australian Planet Search team announced the discovery of HD 30177 b, which has a minimum mass 8 times that of Jupiter, on June 13, 2002. The scientific paper describing the discovery was published in The Astrophysical Journal in 2003. A second massive gas giant planet was later discovered in an approximately 32 year orbit.
HD 30177 | Planetary system
Given the planet's high mass, the planet is a gas giant with no solid surface. Since the planet has only been detected indirectly, parameters such as its radius, composition, and temperature are unknown. Assuming a composition similar to that of Jupiter and that the planet's atmosphere is close to chemical equilibrium, it is predicted that 55 Cancri d is covered in a layer of water clouds: the planet's internal heat probably keeps it too warm to form the ammonia-based clouds that are typical of Jupiter. Its surface gravity is likely to be about 4 to 5 times stronger than Jupiter, or about 10 to 15 times that of Earth which is because the radius of the planet is unlikely to be much more than Jupiter's and is probably slightly smaller than Jupiter due to the high metal content in the parent star.
55 Cancri d | Characteristics
is located from Earth. At , it is listed as among most massive planets in the NASA Exoplanet Archive.
DENIS-P J082303.1−491201 b | Properties
Jupiter mass, also called Jovian mass, is the unit of mass equal to the total mass of the planet Jupiter. This value may refer to the mass of the planet alone, or the mass of the entire Jovian system to include the moons of Jupiter. Jupiter is by far the most massive planet in the Solar System. It is approximately 2.5 times as massive as all of the other planets in the Solar System combined. Jupiter mass is a common unit of mass in astronomy that is used to indicate the masses of other similarly-sized objects, including the outer planets and extrasolar planets.
Jupiter mass | Introduction
Prior to recent results from the "Kepler" space observatory, most confirmed planets were gas giants comparable in size to Jupiter or larger because they are most easily detected. However, the planets detected by "Kepler" are mostly between the size of Neptune and the size of Earth. If a planet is detectable by both the radial-velocity and the transit methods, then both its true mass and its radius can be determined, as well as its density. Planets with low density are inferred to be composed mainly of hydrogen and helium, whereas planets of intermediate density are inferred to have water as a major constituent.
Exoplanetology | Radius, density, and bulk composition
38 Virginis b is a super-Jupiter, an exoplanet that has a mass larger than that of the planet Jupiter. It has a minimum mass of 4.51 .
38 Virginis b | Mass
The planet is 0.919 times as massive as Jupiter but 1.799 times the diameter, the largest planet ever found at the time (next to WASP-17b, found on 1 May 2009), giving it an average density of only about 0.333 grams per cubic centimetre, approximately the same as Saturn's moon Methone. This made TrES-4 both the largest known planet and the planet with the lowest known density at the time of its discovery. TrES-4's orbital radius is 0.05091 AU, giving it a predicted surface temperature of about 1782 K. This by itself is not enough to explain the planet's low density, however.
TrES-4b | Physical characteristics
HD 196885 Ab (also referred to as HD 196885 b) is a jovian planet with at least 2.96 times the mass of Jupiter. This planet was discovered on October 23, 2007.
HD 196885 Ab | Introduction
Jupiter was expected to either consist of a dense core, a surrounding layer of liquid metallic hydrogen (with some helium) extending outward to about 78% of the radius of the planet, and an outer atmosphere consisting predominantly of molecular hydrogen, or perhaps to have no core at all, consisting instead of denser and denser fluid (predominantly molecular and metallic hydrogen) all the way to the center, depending on whether the planet accreted first as a solid body or collapsed directly from the gaseous protoplanetary disk. However, the "Juno" mission, which arrived in July 2016, found that Jupiter has a very diffuse core, mixed into the mantle.
Jupiter | Internal structure
When reporting on the masses of extrasolar planets, astronomers often discuss them in terms of multiples of Jupiter's mass ( = 1.9 kg). For example, "Astronomers recently discovered a planet outside our Solar System with a mass of approximately 3 Jupiters." Furthermore, the mass of Jupiter is nearly equal to one thousandth of the mass of the Sun.
List of unusual units of measurement | Jupiter
Kepler-1625b is a Jovian-sized gas giant, a type of planet several times greater in radius than Earth and mostly composed of hydrogen and helium. It is 11.4 times Earth's radius, approximately equal to that of the planet Jupiter. However, it is up to 11.6 times more massive (about 3,700 Earth masses), based on radial velocity observations. 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. However, this mass value only corresponds to an 3-sigma upper limit and the mass of the planet remains undetected at this time.
Kepler-1625b | Mass and radius
The planet has a mass at least slightly less than that of Jupiter. It orbits its parent star at the distance of 4.18 AU. Its orbital period is about 9.095 Earth years and its orbit is circular. There are no interior planets of minimum mass ("m" sin"i") greater than 0.3 Jupiter. Jupiter-like planets with these orbital and system characteristics are unlikely to be perturbed from the star's inclination. Since the star's inclination is known as around 50°, this would make the planet's most likely mass greater than Jupiter's mass but less than twice that mass. As such HD 154345 b is presumed to be a gas giant "Jupiter twin".
HD 154345 b | Characteristics
As of 2011 the Extrasolar Planets Encyclopaedia included objects up to 25 Jupiter masses, saying, "The fact that there is no special feature around in the observed mass spectrum reinforces the choice to forget this mass limit". As of 2016 this limit was increased to 60 Jupiter masses based on a study of mass–density relationships. The Exoplanet Data Explorer includes objects up to 24 Jupiter masses with the advisory: "The 13 Jupiter-mass distinction by the IAU Working Group is physically unmotivated for planets with rocky cores, and observationally problematic due to the sin i ambiguity." The NASA Exoplanet Archive includes objects with a mass (or minimum mass) equal to or less than 30 Jupiter masses.
Brown dwarf | Current IAU standard
The claimed planet had a minimum mass equal to the mass of Jupiter and was thought to be located in an elliptical orbit with a period of 264 days. However independent measurements of the star failed to confirm the existence of the planet, and the planet does not appear in the current web version of the Catalog of Nearby Exoplanets. But another planet was discovered in system in 2012; this Jupiter-twin completes one orbit in roughly 16 years. Its eccentricity and orbit is very poorly constrained.
HD 150706 | Introduction
The planets in the system have a size between Neptune and Saturn. Only planet b has a size similar to Jupiter. Models predict that the planets have a minimum core mass of 5 and are surrounded by a thick envelope that make up 20% of their mass. The total mass of planet c and d was predicted to be 2 - 28 and the total mass of planet d and b was predicted to be 9 - 120 . In a follow-up paper the mass of V1298 Tauri b was constrained to <2.2 .
V1298 Tauri | Planetary System
The Earth's Moon has a density of 3.4 g·cm and Jupiter's satellites, Io, 3.528 and Europa, 3.013 g·cm; other satellites typically have densities less than 2 g·cm.
Terrestrial planet | Solar System's terrestrial planets
In results published in 2018, a planet in the disk, named PDS 70b, was imaged by the Very Large Telescope (VLT). With a mass estimated to be a few times greater than Jupiter, the planet was thought to have a temperature of around and an atmosphere with clouds; its orbit has an approximate radius of , taking around 120 years for a revolution. Modelling predicts that the planet has acquired its own accretion disk. The accretion disk was observationally confirmed in 2019, and accretion rate was measured to be at least 5*10 Jupiter masses per year, which is equivalent to about 1/80 the mass of the Moon.
PDS 70 | Planetary system
The ambiguity inherent in the IAU's definition was highlighted in December 2005, when the Spitzer Space Telescope observed Cha 110913-773444 (above), only eight times Jupiter's mass with what appears to be the beginnings of its own planetary system. Were this object found in orbit around another star, it would have been termed a planet. In September 2006, the Hubble Space Telescope imaged CHXR 73 b (left), an object orbiting a young companion star at a distance of roughly 200 AU. At 12 Jovian masses, CHXR 73 b is just under the threshold for deuterium fusion, and thus technically a planet; however, its vast distance from its parent star suggests it could not have formed inside the small star's protoplanetary disc, and therefore must have formed, as stars do, from gravitational collapse.
Definition of planet | Planetary-mass stellar objects
If the atmosphere of a hot Jupiter is stripped away via hydrodynamic escape, its core may become a chthonian planet. The amount of gas removed from the outermost layers depends on the planet's size, the gases forming the envelope, the orbital distance from the star, and the star's luminosity. In a typical system, a gas giant orbiting at 0.02 AU around its parent star loses 5–7% of its mass during its lifetime, but orbiting closer than 0.015 AU can mean evaporation of a substantially larger fraction of the planet's mass. No such objects have been found yet and they are still hypothetical.
Hot Jupiter | Atmospheric loss
Massive solid planets can also exist. 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. 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 exoplanet equals approximately 4000 Earth masses.
Giant planet | Massive solid planets
This red supergiant or red hypergiant of the largest stars found, with a size of around 1,200 solar radii. If it replaced the sun as the central body of our solar system, its photosphere would engulf the orbit of Jupiter.
SP77 31-18 | Introduction
The perihelia of these object would cycle over periods of over 100 Myr, returning many to the influence of the Neptune. The estimated mass remaining at the current time is 0.3 – 0.4 Earth masses.
Jumping-Jupiter scenario | Planet Nine cloud
With the upward revision in the age of the Upper Scorpius group from 5 million to 11 million years, the estimated mass of 1RXS J1609b is approximately 14 Jupiter masses, i.e. above the deuterium-burning limit. An older age for the J1609 system implies that the luminosity of J1609b is consistent with a much more massive object, making more likely that J1609b may be simply a brown dwarf which formed in a manner similar to that of other low-mass and substellar companions.
1RXS J160929.1−210524 | Planetary system
The current best known value for the mass of Jupiter can be expressed as : which is about as massive as the sun (is about ): Jupiter is 318 times as massive as Earth:
Jupiter mass | Current best estimates
The Jupiter trojans' densities (as measured by studying binaries or rotational lightcurves) vary from 0.8 to 2.5 g·cm. Jupiter trojans are thought to have been captured into their orbits during the early stages of the Solar System's formation or slightly later, during the migration of giant planets.
Jupiter trojan | Introduction
In 2007, a Neptune-mass planet was found orbiting the star by Melo. According to the author, assuming an Earth-like rocky composition, the planet could yield a radius 2.2 times that of Earth. This could be furtherly proved if transit were observed, though, as authors state, it is a difficult task. At this point, it was suggested that a best fit orbital solution hints the presence of an additional planetary companion (so far unconfirmed) with 70% of Jupiter's mass, likely orbital separation of 0.68 Astronomical units and eccentric orbit (e=0.3). However, in 2016, further analysis or radial velocity data confirmed the presence of an outer planet larger and more eccentric than was originally believed.
HD 219828 | Planetary system
The planet is a large hot Jupiter, about 1.43 times the radius of Jupiter and approximately 3.3 times as massive. Its huge size is due to the intense heating from its parent star, which causes the outer layers of its atmosphere to bloat. The extremely large radius of the planet indicates that CoRoT-2b is very hot, estimated to be around 1500 K, even hotter than would be expected given its location close to its parent star. This fact may be a sign of tidal heating due to interactions with another planet. At Jupiter-like distances its radius would roughly be the same as Jupiter.
CoRoT-2b | Characteristics
has a diameter estimated at around , roughly a fifth the size of Pluto.
2014 FC72 | Physical characteristics
Additional measurements taken over six years show a long-term linear trend in the radial velocity data consistent with a companion of 15 Jupiter masses or greater. Adaptive optics images were taken at the Keck telescope and when combined with the radial velocity data show the maximum mass of the companion is that of an M dwarf star. The planet was discovered by the HATNet Project and the researchers there believed the planet to be 10-20% larger than Jupiter. This discovery is important as it provides further support for the existing theory of planetary structure.
HD 147506 | Planetary system
As of June 2016, all but one of the confirmed Kepler circumbinary planets are smaller than Jupiter. This cannot be a selection effect because larger planets are easier to detect. Simulations had predicted this would be the case.
Circumbinary planet | Planet size limit
Iota Draconis b is a "super-Jupiter" a planet that has mass larger than that of the gas giants Jupiter and Saturn. It has a blackbody temperature of . It has an estimated mass of around 8.82 and a potential radius of around 12 based on its mass, since it is more massive than Jupiter.
Iota Draconis b | Mass, radius and temperature
HIP 11915 b is a jovian planet, an exoplanet with a mass and radius close to that of the planet Jupiter. It has a mass of 0.99 (315 ) and a likely radius of around 1 . Based on models, it is expected to have a temperature of around . This is nearly the same as the planet Jupiter.
HIP 11915 b | Mass, radius and temperature
At the time of discovery of the planet HD 49674 b in 2002, it was the least massive planet known, very close to the boundary between sub-Jupiter mass and Neptune-mass at 0.1 M. This planet orbits very close to the star.
HD 49674 | Planetary system
HD 142415 b is an exoplanet with the semi-amplitude of 51.3 ± 2.3 m/s. This indicates the minimum mass of 1.69 Jupiter mass, an orbital period of 386.3 days, and the semi-major axis of 1.07 astronomical units based from its stellar mass. The wild, oval pathed wobble of the star used by Doppler spectrometer indicates that the orbit of the planet is highly eccentric at around 50%. The planet was discovered in La Silla Observatory on 30 June 2003 by Mayor, who used the CORALIE spectrograph.
HD 142415 b | Introduction
There cannot be any habitable planets in this system. Also, observation has ruled out planets heavier than 0.7 Jupiter mass with a period of one year or less.
HD 80606 and HD 80607 | Planetary system
HD 40307 b does not transit and has not been imaged. More specific characteristics, such as its radius, composition, and possible surface temperature cannot be determined. With a lower mass bound of 4.2 times the mass of the Earth, HD 40307 b is presumably too small to be a jovian planet. This concept was challenged in a 2009 study, which stated that if HD 40307 b is terrestrial, the planet would be highly unstable and would be affected by tidal heating in a manner greater than Io, a volcanic satellite of planet Jupiter; restrictions that seem to bind terrestrial planets, however, do not restrict ice giant planets like Neptune or Uranus.
HD 40307 b | Characteristics
In November 2003, a planet was announced orbiting the giant star. A doppler spectrometer was used to look for effects on the star caused by the gravitational tug of the orbiting planet. Using the amplitude from the radial velocity method, he calculated the planetary mass as 5.25 Jupiter masses and with period 303 days. However that mass is only a minimum because the inclination of the orbit is not known. Using the stellar mass and period, he calculated the semimajor axis as 0.911 astronomical units. He found that the shape of the stellar wobble is circular, implying that the planet has zero eccentricity.
HD 59686 | Planetary system
HD 168443 b is a planet with a minimum mass seven times as that of Jupiter. Given the high mass, this planet is likely to be a gas giant, or possibly a small brown dwarf depending on the orbital inclination. It orbits closer to its star than Mercury does to the Sun, and its surface temperature is likely to be very high. It was discovered in 1999 using radial velocity measurements taken at the W. M. Keck Observatory in Hawaii.
HD 168443 b | Introduction
Further study of the system using Hubble Space Telescope astrometry revised the mass of HD 38529 c downwards to 17.7 Jupiter masses and suggested the presence of an additional planet, orbiting in the gap between HD 38529 b and c. The possible third planet was refuted after additional radial velocity measurements were collected.
HD 38529 | Planetary system
Depending on composition the two planets may be around the same size, or HD 154345 b may be larger. This planet may also harbor a system of moons and rings.
HD 154345 b | Characteristics
Still glowing red hot, it will shrink to a size slightly smaller than Jupiter as it cools over the next few billion years. An initial photometric estimate for the distance to 2M1207 was 70 parsecs. In December 2005, American astronomer reported a more accurate distance (53 ± 6 parsecs) to 2M1207 using the moving cluster method. The new distance gives a fainter luminosity for 2M1207. Recent trigonometric parallax results have confirmed this moving cluster distance, leading to a distance estimate of 53 ± 1 parsec or 172 ± 3 light years.
2M1207 | Introduction
At the time of discovery, with 5.5 Earth masses, the planet was less massive than the previous candidate for lowest-mass exoplanet around a main-sequence star, the 7.5 Earth mass Gliese 876 d. Since 2013, many Earth-sized or smaller planets around main-sequence stars have been detected by the "Kepler" spacecraft and others.
OGLE-2005-BLG-390Lb | Mass, radius and temperature
Through infrared and ultraviolet measurements, trace amounts of benzene and other hydrocarbons have also been found. The interior contains denser materials—by mass it is roughly 71% hydrogen, 24% helium, and 5% other elements. The atmospheric proportions of hydrogen and helium are close to the theoretical composition of the primordial solar nebula. Neon in the upper atmosphere only consists of 20 parts per million by mass, which is about a tenth as abundant as in the Sun. Helium is also depleted to about 80% of the Sun's helium composition. This depletion is a result of precipitation of these elements into the interior of the planet.
Jupiter | Composition
WASP-104b's size is comparable to that of Jupiter; its mass and radius are 1.272 times and 1.137 times greater than Jupiter's, respectively. It has 12.5 times the mass of Earth and a low density, and may be composed of gas.
WASP-104b | Size, radius, and temperature
This appears to be a result of the rapid rotation and underlying symmetry of the planet. There are no oceans or landmasses to cause local heating and the rotation speed is much higher than that of Earth. There are smaller structures as well: spots of different sizes and colors. On Jupiter, the most noticeable of these features is the Great Red Spot, which has been present for at least 300 years. These structures are huge storms. Some such spots are thunderheads as well.
Giant planet | Atmospheres
It is possible that a planet in this system may have been scattered and ended up being accreted by the star, which may account for the large surface metallicity.
HD 12661 | Properties
In 2009, a gas giant was found in orbit around the star using the radial velocity method. It has an orbital period of and has at least 68% of the mass of Jupiter.
HD 8535 | Planetary system
The planet has a mass about half that of Jupiter and orbits at a distance of 0.921 AU from the star with a period of 310.55 days. The planet may be located at a distance close enough to the star to receive a comparable amount of ultraviolet radiation as the Earth does from the Sun. However, it is too close to the star to be able to support liquid water at its surface. Furthermore, given its mass, the planet is likely to be a gas giant with no solid surface.
Mu Arae d | Characteristics
However the particle size distribution of the dust is somewhat shallower than in the Amalthea ring. It follows a power law with q < 2. In the Thebe extension the parameter q may be even smaller.
Rings of Jupiter | Thebe gossamer ring
The sizes are listed in units of Earth radii (). All planets listed are smaller than Earth and being up to 0.7 Earth radii.
List of smallest exoplanets | List
Countering this argument, the density of Hektor as determined from its rotational lightcurve (2.480 g/cm) is significantly higher than that of 617 Patroclus. Such a difference in densities suggests that density may not be a good indicator of asteroid origin.
Jupiter trojan | Composition
However these measurements were later proved useful only for upper limits of inclination. If the planet orbits in the same plane as the claimed circumstellar disk, which seems a plausible assumption, it would have an inclination of 40° and an absolute mass of 2.2 times Jupiter, however later observations failed to confirm the disk's existence.
HD 210277 b | Introduction
However, since it is probably an ocean planet or Mini-Neptune, it is likely larger.
HD 219134 g | Introduction
HD 50554 b is a Jupiter-sized extrasolar planet with minimum mass 4.4 times that of Jupiter. The planet was announced in 2001 by the European Southern Observatory and confirmed in 2002 using observations from the Lick and Keck telescopes.
HD 50554 b | Introduction
A gas giant planet with a minimum mass almost double that of Jupiter was discovered as part of a radial velocity survey of subgiant stars at Keck Observatory.. The International Astronomical Union (IAU) has named it Ixbalanqué, the twin brother of Hunahpú.
HD 98219 | Planetary system
The object's mass has been calculated as approximately 12.8 times Jupiter's mass, the host star's mass as 2.4 to 2.5 solar masses. The temperature of the object is estimated to be around 1700 kelvins, and, if seen up close, would appear reddish in color. The object's distance from its parent star is about 1.8 times Neptune's distance from the Sun.
Kappa Andromedae b | Discovery
The best fit to the preliminary data suggests two periodicities: one almost exactly a year long like the Earth's periodicity, and a second of around two years. Both objects are predicted to have masses greater than that of the planet Jupiter: their minimum masses are 1.8 and 1.9 Jupiter masses, respectively. Until the inclination of their orbits is known, their actual masses cannot be pinned down more accurately.
HD 47366 | Introduction
HD 178911 Bb is a planet discovered in 2001 by Zucker who used the radial velocity method. The minimum mass of this giant planet is 7.35 times that of Jupiter that orbits close to the star. The period of the planet is 71.5 days and the semi-amplitude is 346.9 m/s.
HD 178911 Bb | Introduction
It has at least 2.3 times Jupiter's mass.
Rho Indi | Planetary system