Types of planet

planetary-mass object in hydrostatic equilibrium which is not a satellite of another one, but which has still not significantly cleared its neighborhood to dominate it gravitationally and maintain its cohesion

alt=Timelapse of exoplanets orbit motion|thumb|upright=1.5|Four exoplanets of the HR 8799 system imaged by the [[W. M. Keck Observatory over the course of seven years. Motion is interpolated from annual observations.]] thumb|295x295px|Comparison of the size of exoplanets orbiting Kepler-37 to Mercury, Mars and Earth An exoplanet or extrasolar planet is a planet outside of the Solar System. The first confirmed detection of an exoplanet was in 1992 around a pulsar, and the first detection around a main-sequence star was in 1995. A different planet, first detected in 1988, was confirmed in 2003.

planet that is composed primarily of silicate rocks or metals. Within the Solar System, the terrestrial planets are the inner planets closest to the Sun, i.e. Mercury, Venus, Earth, and Mars

giant planet which mainly consist of light elements such as hydrogen and helium

type of substellar object larger than a gas giant

giant planet primarily composed of elements heavier than hydrogen and helium

planetary-mass object that orbits the galaxy directly

class of gas giant exoplanets that are inferred to be physically similar to Jupiter but that have very short orbital periods (P < 10 days)

thumb|upright=1.75|right|Illustration of the inferred size of the super-Earth CoRoT-7b (center) in comparison with [[Earth and Neptune]] A super-Earth is a type of exoplanet with a mass higher than Earth's, but substantially below those of the Solar System's ice giants, Uranus and Neptune, which are 14.5 and 17.1 times Earth's mass 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, although "m

thumb|4 Vesta|Vesta is one of the best known examples of a protoplanet. A protoplanet or planetary embryo is an astronomical body originated within a protoplanetary disk that has undergone internal melting to produce a differentiated interior.

hypothetical type of planet whose surface is completely covered with an ocean of water with potential signs of life; in fiction see Q98807723

planet much larger than the Earth

binary satellite system where two planetary-mass objects share an orbital axis external to both

planet type

astronomical object of planetary mass that formed in the manner of stars

hot, water-covered planet with a hydrogen-rich atmosphere that may harbor lifeforms

another planet with environmental conditions similar to those found on the planet Earth

planet that is outside the Milky Way Galaxy

exoplanet orbiting a pulsar

extrasolar terrestrial planet

Mesoplanets are planetary-mass objects with sizes smaller than Mercury but larger than Ceres. The term was coined by Isaac Asimov. Assuming size is defined in relation to equatorial radius, mesoplanets should be approximately 500 km to 2,500 km in radius.

planetary type

upright=1.5|thumb|Size comparison of Earth and Neptune with the mega-Earth TOI-1853 b (center), a very dense Neptune-sized [[exoplanet believed to be nearly entirely made of solid rock, metal, and water.]]

type of planet with a surface primarily covered in molten lava

Jovian planet that orbits its star in an eccentric orbit

planet that orbits two stars instead of one

thumb|Artist's impression of 2M1207b A super-Jupiter is a gas giant exoplanet that is more massive than the planet Jupiter. For example, companions at the planet–brown dwarf borderline have been called super-Jupiters, such as around the star Kappa Andromedae.

thumb|300px|Comparing the size of Earth, [[Mars, and exoplanets of Kepler-20 and Kepler-42]]

thumb|Artistic representation of a super-puff planet A super-puff is a type of exoplanet with a mass only a few times larger than Earth's but with a radius larger than that of Neptune, giving it a very low mean density. They are cooler and less massive than the inflated low-density hot-Jupiters.

Wikimedia list article

planet with an orbital period less than one Earth day

thumb|Artistic impression A synestia is a hypothesized structure for the debris field generated by the collision of planets: a rapidly spinning doughnut-shaped mass of vaporized rock. The term was coined in 2017 by Sarah T. Stewart-Mukhopadhyay, taken from Hestia, goddess of the hearth, combined with syn- meaning together. In computer simulations of giant impacts of rotating objects, a synestia can form if the total angular momentum is greater than the co-rotational limit. Beyond the co-rotational limit, the velocity at the equator of a body would exceed the orbital velocity.

thumb|Artist's interpretation of a super-Neptune Super-Neptunes, also known as a sub-Saturns, are a rare population of exoplanets that have properties between that of Neptune and Saturn (, , 0.687-1.64 g/cm3). According to the core-accretion model of planet formation, most planets that reach a threshold are expected to rapidly expand to gas giant sizes (≥) in a mechanism known as runaway gas accretion. Despite this, Super-Neptunes sit between this bimodal distribution of sub-Neptunes and gas giants, failing to either begin or fully complete runaway accretion.

thumb|Artistic rendering of a sub-neptune