Planets

Earth is classified as a temperate mesobaric terra, and it is the archetype for the terran type. Its moon, Luna, is a frigid airless miniselena.

— Example planetary classification

Planets are the comparatively tiny motes of dust and gas that provide a platform for the vibrant verdancy of the living cosmos. There is an incredibly broad range of planetary "phenotypes," but all planets have a few critical similarities that define them as such. According to the International Astronomical Union's 2050 definition, a planetoid is a celestial body that:

(a) has sufficient mass to maintain a gravitational hydrostatic equilibrium in a spheroid shape.

(b) does not undergo natural, self-sustaining nuclear fusion at any point in its existence.

Contents

Terminology
> Terms

• Planets & Planetinos
• Moons
• Unbound Planetoids

Planetary Class System
> Subcategories

• Size
• Temperature
• Atmosphere
1. Type
   • Selenae
   • Desertae
   • Terrae
   • Vulcanae
   • Hestiae
   • Erimae
   • Chionae
   • Aquarae
   • Tethae
   • Oceaniae
   • Nephelae
   • Joviae

Terminology

The IAU definition is quite broad and does not specify orbital qualifications - a planet is defined primarily by its physical attributes, and secondarily by its orbital characteristics. There are more specific terms which derive from "planet" and define more kinds of planetoids. They are also occasionally referred to as "planemos" - short for planetary-mass objects. The Standard English word "planet" is derived from the ancient Greek term "πλανήται" (planḗtai), meaning 'wanderers', which was used to refer to the five stars that appeared to move across the night sky.

Planets & Planetinos

A "planet" (or "major planet") is a planetoid which directly orbits a star (or stars). Natural bodies that orbit a star but are not rounded by gravity, such as asteroids and comets, are called "planetinos" (or "minor planets").

Major & Minor Moons

A "moon" is a planetoid or planetino which orbits another planet or planetino; they are formally called "natural satellites." Planetoid satellites are classified as "major moons," in contrast to planetino "minor moons."

Unbound Planetoids

Planetoids which do not orbit any object, planet or star, are officially classified as "unbound planetoids." However, these objects are more commonly called "rogue planets" or "wandering planets."

Planetary Class System

Beyond the initial definition, planetoids are described by a system of classifications split into four categories: size, temperature, atmosphere, and type, expressed as follows: [temperature] [atmosphere] [size]-[type]. The planetary class designations of planetary bodies are one-word labels representing particular defining aspects of themselves, intended to convey to the reader a very general but fairly accurate assessment of what the planet is like in each category. A planet's biosphere is classified according to a separate system.

Size

All telluric and cryonic planetary bodies can be classified as one of the following size classes based on their mass:
unit: Earth mass

• Micro- (< 0.002 M_Earth)
• Mini- (0.002 M_Earth to 0.02 M_Earth)
• Sub- (0.02 M_Earth to 0.2 M_Earth)
• No prefix (0.2 M_Earth to 2 M_Earth)
• Super- (2 M_Earth to 10 M_Earth)
• Mega- (> 10 M_Earth)

All nephelic planetary bodies can be classified as one of the following size classes based on their mass:
unit: Earth mass

• Mini- (< 5 M_Earth)
• Sub- (5 M_Earth to 10 M_Earth)
• No prefix (10 M_Earth to 25 M_Earth)
• Super- (25 M_Earth to 50 M_Earth)
• Mega- (> 50 M_Earth)

All jovian planetary bodies can be classified as one of the following size classes based on their mass:
unit: Earth mass

• Mini- (< 50 M_Earth)
• Sub- (50 M_Earth to 200 M_Earth)
• No prefix (200 M_Earth to 600 M_Earth)
• Super- (600 M_Earth to 1800 M_Earth)
• Mega- (> 1800 M_Earth)

Temperature

All planetary bodies can be classified as one of the following temperature classes based on their average surface temperature:
unit: Kelvin

• Frigid (< 90 K) - The methane frost line effective temperature threshold is estimated at 90 K
• Cold (90 K to 170 K) - The water frost line effective temperature threshold is estimated at 170 K
• Cool (170 K to 250 K) - The lowest effective temperature for a habitable planet is estimated at 250 K
• Temperate (250 K to 330 K) - The highest effective temperature for a habitable planet is estimated at 330 K
• Warm (330 K to 500 K) - The soot line effective temperature threshold is estimated at 500 K
• Hot (500 K to 1000 K) - The lowest temperature for planetary silicate condensation is estimated around 1000 K
• Torrid (> 1000 K)

Atmosphere

All planetary bodies can be classified as one of the following atmosphere classes based on their surface pressure:
unit: bar

• Airless (< 1e^-6 bar)
• Infrabaric (1e^-6 bar to 1e^-2 bar)
• Hypobaric (1e^-2 bar to 1e^-1 bar)
• Mesobaric (1e^-1 bar to 1e¹ bar)
• Hyperbaric (1e¹ bar to 1e² bar)
• Ultrabaric (> 1e² bar)

Type

All planetary bodies can be classified as one of the following twelve types based on their overall geophysical structure, composition, solvent presence, and atmosphere. Solid planets are generally divided into two phyla depending on their bulk composition: tellurae are worlds that are >50% silicate mineral or metallic; cryonae are worlds that are >50% carbonaceous or volatiles. These two solid planet phyla are further classified by the atmosphere and liquisphere properties they exhibit.

Tellurae are typically stratified into three or more layers: a solid inner core, a molten mantle, and a solid crust. They are composed mostly of stable transition metals and silicates, though this is concentrated in the inner layers (especially the core). The crust of telluric planets, by contrast, consist largely of lighter metalloids and nonmetals (such as silicon, carbon, and aluminum). Telluric planets often have tectonic activity caused by interior magma cycles or, in some cases, extreme heating and cooling of the surface.

Cryonic planets, by contrast, are enveloped in glacial shells rather than rocky crusts, which may span all the way to the planets' smaller, lighter cores, often of porous rock; some cryonae even have undifferentiated interiors of jumbled rock in ice. Occasionally, however, these icy crusts hide global liquid oceans, akin to the molten mantles of tellurae, that produce tectonic activity in the glacial crust. These subsurface oceans are warmed by either a core dynamo effect between the core and whatever thin mantle may exist, or tidal heating in certain cases.

The other two major classes of planet are nephelae and joviae. Nephelae are planets composed mostly of supercritical volatiles, while joviae are characterized by hydrogen-helium-dominant compositions. These types of planets, unlike solid worlds, are characterized by a density gradient toward their cores. Typically the stratification of supercritical and gaseous planets includes a solid metallic core at the center, surrounded by a hot, supercritical mantle which is in turn enveloped by an atmosphere of gaseous hydrogen, helium, and trace volatiles.

Selenae

by Gregory Rivera

Luna, a selenic planetoid moon.

Selenic planets (designated by s) are telluric worlds with extremely thin to nonexistent atmospheres. Because of this, their rough surfaces remain unweathered, though they are subject to extreme temperature fluctuations between sunlight and shadow. A selenic planet with endemic life is unheard of, though technically not impossible. Chemosynthetic or photovoltaic autotrophs could form colonies on the airless surfaces of selenae, though this is as yet unproven.

Desertae

by ESA (Rosetta)

Mars, a desert planet (prior to terraformation).

Desert planets (designated by d) are worlds with an overall arid climate and scarce precipitation or surface solvent. This is not to say desertae are entirely devoid of solvent; it often exists under the surface, inside permanent polar ice caps, or even on the surface in liquid state. However, desertae are defined as having less than one third of their surface covered by liquid solvent, often much less. Life is not common on desert worlds, but exists in relative abundance; typically organic but occasionally exotic in nature.

Terrae

by UNAC (SEO-44) / Doug Marshall

Earth, a terran planet.

Terran planets (designated by tr) are telluric worlds with a significant amount of liquid solvent present on the surface; specifically, more than one third of the surface. Life is common on terrae, typically organic but with the occasional exotic biosphere. The presence of life maintains the oceans and atmosphere, just as the oceans and atmosphere allow for the presence of life in the first place. In light of this elaborate circular dance of geology and biology, the most complex planetary bodies are usually terrae.

Hestiae

by UNAC (Sojourn 2) / Doug Marshall

Vulcan, a hestian planet.

Hestian planets (designated by h) are telluric worlds which have permanent regions of liquid silicate or metallic compounds on their surfaces. Their atmospheres are often composed of CO₂, sulfur, and silica vapor. These molten planets are quite rare but magnificent to behold and almost impossible to visit, as the conditions on their surfaces are hostile to most environmental protection technologies employed by spacefaring sophonts. No known hestiae bear life.

Erimae

by NASA (Voyager 2)

Callisto, an erimic planetoid moon.

Erimic planets (designated by e) are airless worlds, similar to selenae, which are primarily composed of solidified volatiles. Erimae are exposed to the same intense temperature fluctuations as their telluric counterparts, though this does not melt the ices at the surface due to the lack of atmosphere. Erimae sometimes have native life, most often in whatever liquid ocean exists beneath the icy crust but occasionally playing host to surface-dwelling microbes.

Chionae

by NASA (JPL - Cassini) / Val Klavans

Titan, a chionic planetoid moon.

Chionic planets (designated by c) are the cryonic counterpart to desertae: they possess atmospheres ranging from infrabaric to hyperbaric, and less than one third of their surfaces are covered by liquid solvent. Like other cryonic worlds, chionae frequently possess interior oceans as well, and occasionally these subglacial seas breach the surface. Life is not common on erimic worlds, but does exist; typically exotic in nature due to the bizarre chemical and energy environments typical of cryonae.

Aquarae

by UNAC (Sojourn 2) / Doug Marshall

Juventas, an aquaric planetoid moon.

Aquaric planets (designated by q) are the cryonic counterpart to terrae: they possess atmospheres ranging from infrabaric to hyperbaric, and more than one third of their surfaces are covered by liquid solvent. Like other cryonic worlds, aquarae frequently possess interior oceans as well, and these subglacial seas often breach the surface. Life is relatively common on aquaric worlds, but is typically exotic in nature due to the bizarre chemical environments and low energy systems typical of cryonic planets.

Oceaniae

by UNAC / Doug Marshall

Oceanus, an oceanic planet.

Oceanic planets (designated by o) are worlds whose surfaces are completely covered by solvent, and often a substantial portion of their mass is said solvent. The global seas lay atop a dense nickel-iron and/or silicate core, which is typically surrounded by a mantle of high-pressure ice. The solvent mass of oceaniae is almost always water, though an ammonia oceanic world exists: Gongong in the FL Virginis system. Life on oceanic worlds is uncommon, but virtually always organic.

Venusiae

by UNAC (Morning Star 17) / Doug Marshall

Venus, a venusian planet.

Venusian planets (designated by v) are telluric worlds with ultrabaric atmospheres dominated by carbon dioxide and trace amounts of other compounds. The intense pressure and heat-trapping effects of their heavy atmospheres cause them to exhibit supercritical behavior at low altitudes, but they retain a solid surface. Venusian worlds rarely have endemic life, but some bear unicellular extremophiles that thrive in the heat and high pressures.

Tethae

by UNAC (DSASF) / Doug Marshall

Echidna, a tethian planet.

Tethian planets (designated by th) are telluric worlds with ultrabaric atmospheres dominated by gaseous volatiles (usually water vapor) and traces of other compounds. Much like venusiae the intense pressure and heat-trapping effects of tethian atmospheres cause them to exhibit supercritical behavior at low altitudes, but unlike venusiae they do not retain a solid surface. No known tethian worlds harbor endemic life, but it may be possible for a tethia to bear extremophilic unicellular organisms in its upper atmosphere.

Nephelae

by NASA (JPL - Voyager 2)

Neptune, a nephelic planet.

Nephelic planets (designated by n), also called ice giants, are vaporous worlds composed primarily of volatiles in a gaseous or often supercritical state. In essence, ice giants occupy the planetary spectrum between oceaniae and joviae. Life on nephelae is quite rare, and tends to be exotic more often than organic: based on nitrogen, phosphorus, and other alternative biochemistries. Most nephelic biospheres are aerial in nature, though in denser strata the inhabitants function more like marine life.

Joviae

by NASA/ESA (Hubble Space Telescope)

Jupiter, a jovian planet.

Jovian planets (designated by j), also called gas giants, are worlds composed primarily of gaseous hydrogen and helium. In jovian planets, the mantle is composed of supercritical hydrogen and helium, gradually fading to a vast hydrogen-helium atmosphere. The outermost layers of joviae are the most complex and beautiful: trace compounds form an ever-shifting, multicolored labyrinth of cloud strata and cyclones. Life on joviae is very rare and almost always exotic in nature.

Hazards

Omnipedia uses a symbolic shorthand to advise users of potentially hazardous conditions on any given celestial body. The full list is shown here for reference. Hover over each symbol with your cursor (or tap and hold on a touchscreen) to view the description of each hazard.

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