http://starshiptracker.com/sfcwiki/index.php?action=history&feed=atom&title=Planetary_ClassificationsPlanetary Classifications - Revision history2026-10-16T05:14:48ZRevision history for this page on the wikiMediaWiki 1.42.1http://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=44983&oldid=prevDan at 17:52, 17 September 20252025-09-17T17:52:53Z<p></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class M''' (''Minshara'') <br>(''ex: [[Bajor]], [[Cardassia]], [[Earth]]'') || '''Terrestrial'''<br>Class M planets are perfect for most humanoids, they are stable and can often evolve humanoid and other complex animal life. The land masses are mostly rocky but covered in soil and vegetation, twenty to eighty percent of the planet is covered in water. The only other requirement is that it must have a breathable oxygen-nitrogen atmosphere and a temperate climate. Most species in the known universe originated from planets of this class. They are found in the ecosphere of a star that allows their development.<br>'''Noted features:''' average size, developed ecosystems, average atmospheres, geologically active, varied environments, '''inhabitable'''|| Green || Water abundant || Varied: thin, standard or thick (nitrogen, oxygen and trace elements) || [[File:Class M.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class M''' (''Minshara'') <br>(''ex: [[Bajor]], [[Cardassia]], [[Earth]]'') || '''Terrestrial'''<br>Class M planets are perfect for most humanoids, they are stable and can often evolve humanoid and other complex animal life. The land masses are mostly rocky but covered in soil and vegetation, twenty to eighty percent of the planet is covered in water. The only other requirement is that it must have a breathable oxygen-nitrogen atmosphere and a temperate climate. Most species in the known universe originated from planets of this class. They are found in the ecosphere of a star that allows their development.<br>'''Noted features:''' average size, developed ecosystems, average atmospheres, geologically active, varied environments, '''inhabitable'''|| Green || Water abundant || Varied: thin, standard or thick (nitrogen, oxygen and trace elements) || [[File:Class M.png|200px]]</div></td></tr>
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<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class N''' (''Nesheh'') <br>(''ex: [[Essof IV<del style="font-weight: bold; text-decoration: none;">]], [[Venus</del>]]'') || '''Reducing'''<br>'''Class N1''' planets are failures when compared to Class M. While they may appear in a similar location in a star's ecosphere, they are barely hospitable for any race. They are barren with temperatures that reach over 700 Kelvin. Massive amounts of carbon dioxide cover the surface and build up a pressure a hundred times that of an M Class world. This means that from space, it seems like the planet is entirely covered in clouds.<br>'''Noted features:''' average size, thick atmosphere, geologically active, extremely hot surface temperatures, mid orbits, '''uninhabitable''' <br>While Class N1 planets are among the hottest planets known to exist, at the opposite end of the temperature spectrum is the frigid '''Class N2'''. Though similar in appearance to N1 thanks in part to the dense atmosphere and characteristic veil of thick clouds, this secondary class is structurally very different. Temperatures are so cold that liquid methane can pool into lakes, and vast mountain ranges are made of rock-hard ice.<br>'''Noted features:''' average size, thick atmosphere, geologically active, extremely frigid surface temperatures, '''uninhabitable'''|| Inner, Outer || High temperature (N1)<br>Low temperature (N2)|| Extremely dense (carbon dioxide and sulfides) || [[File:Class N.png|200px]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class N''' (''Nesheh'') <br>(''ex: [[Essof IV]]'') || '''Reducing'''<br>'''Class N1''' planets are failures when compared to Class M. While they may appear in a similar location in a star's ecosphere, they are barely hospitable for any race. They are barren with temperatures that reach over 700 Kelvin. Massive amounts of carbon dioxide cover the surface and build up a pressure a hundred times that of an M Class world. This means that from space, it seems like the planet is entirely covered in clouds.<br>'''Noted features:''' average size, thick atmosphere, geologically active, extremely hot surface temperatures, mid orbits, '''uninhabitable''' <br>While Class N1 planets are among the hottest planets known to exist, at the opposite end of the temperature spectrum is the frigid '''Class N2'''. Though similar in appearance to N1 thanks in part to the dense atmosphere and characteristic veil of thick clouds, this secondary class is structurally very different. Temperatures are so cold that liquid methane can pool into lakes, and vast mountain ranges are made of rock-hard ice.<br>'''Noted features:''' average size, thick atmosphere, geologically active, extremely frigid surface temperatures, '''uninhabitable'''|| Inner, Outer || High temperature (N1)<br>Low temperature (N2)|| Extremely dense (carbon dioxide and sulfides) || [[File:Class N.png|200px]]</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class O''' (''Ob'taree'')<br>(''ex: [[Azati Prime]], [[Bolarus]], [[Venus]]'') || '''Pelagic'''<br>Class O planets are covered in water; to qualify, a planet needs to be more than 80% surface water. Due to the water they absorb and store, a lot of the heat still reaches the planet, making the atmosphere very charged. They can support vast aquatic ecosystems, as well as tropical islands on peaks above the water. These planets tend to have the most living matter compared to others and teem with vast variations of species. While most do not evolve humanoid life, some do (though they are normally aquatic).<br>'''Noted features:''' average size, developed ecosystems, average atmospheres, geologically active, varied (mostly) aquatic environments, '''inhabitable'''|| Green || 80%+ water || Varied: thin, standard or thick (nitrogen, oxygen and trace elements) || [[File:Class O.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class O''' (''Ob'taree'')<br>(''ex: [[Azati Prime]], [[Bolarus]], [[Venus]]'') || '''Pelagic'''<br>Class O planets are covered in water; to qualify, a planet needs to be more than 80% surface water. Due to the water they absorb and store, a lot of the heat still reaches the planet, making the atmosphere very charged. They can support vast aquatic ecosystems, as well as tropical islands on peaks above the water. These planets tend to have the most living matter compared to others and teem with vast variations of species. While most do not evolve humanoid life, some do (though they are normally aquatic).<br>'''Noted features:''' average size, developed ecosystems, average atmospheres, geologically active, varied (mostly) aquatic environments, '''inhabitable'''|| Green || 80%+ water || Varied: thin, standard or thick (nitrogen, oxygen and trace elements) || [[File:Class O.png|200px]]</div></td></tr>
</table>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43358&oldid=prevDan at 12:33, 24 January 20252025-01-24T12:33:42Z<p></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Y''' (''Yen'deshim'') <br>(''ex: ''[[Ha'Dara]], [[Tholia]], [[Visalayan]]'') || '''Demon'''<br>Class Y planets come in a range of sizes (1,000-10,000 kms), and while they have atmospheres, they are completely hostile to almost all known life. Radioactive, toxic air scours the surface at huge speeds. Temperature moves between huge highs and lows, and almost constantly covered in harsh storms, it would be better to be exposed to space than the surface of a Class Y.<br>'''Noted features:''' small & average sizes, average & thick atmospheres; extreme variances in high & low temperatures, rather geologically active, '''uninhabitable'''|| Inner, Green, Outer, Far || 500°K+ || Dense to extremely dense and turbulent, saturated with toxic chemicals and therionic radiation || [[File:Class Y.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Y''' (''Yen'deshim'') <br>(''ex: ''[[Ha'Dara]], [[Tholia]], [[Visalayan]]'') || '''Demon'''<br>Class Y planets come in a range of sizes (1,000-10,000 kms), and while they have atmospheres, they are completely hostile to almost all known life. Radioactive, toxic air scours the surface at huge speeds. Temperature moves between huge highs and lows, and almost constantly covered in harsh storms, it would be better to be exposed to space than the surface of a Class Y.<br>'''Noted features:''' small & average sizes, average & thick atmospheres; extreme variances in high & low temperatures, rather geologically active, '''uninhabitable'''|| Inner, Green, Outer, Far || 500°K+ || Dense to extremely dense and turbulent, saturated with toxic chemicals and therionic radiation || [[File:Class Y.png|200px]]</div></td></tr>
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<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Z''' (''Kohl-kov'')<br>(''ex: [[Sol V]]'')|| '''Asteroid Belt'''<br>Asteroid belts are the region of the a star system that inhabit orbits between planets and occupied by numerous irregularly shaped bodies called asteroids or minor planets and can range down to the size of a dust particle. Asteroid belts form from primordial solar nebulae as a group of planetesimals, the smaller precursors of planets, which in turn formed protoplanets; however, gravitational perturbations from large planets, such as gas giants, imbue the protoplanets with too much orbital energy for them to accrete into a planet. Collisions become too violent, and instead of fusing together, the planetesimals and most of the protoplanets shatter, forming an orbital ring of debris. '''Inhabitable when pressurized'''|| Inner, Green, Outer, Far || Carbonaceous, silicate and metallic materials || None || [[File:Asteroid belt.png]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Z''' (''Kohl-kov'')<br>(''ex: [[Sol V]]'')|| '''Asteroid Belt'''<br>Asteroid belts are the region of the a star system that inhabit orbits between planets and occupied by numerous irregularly shaped bodies called asteroids or minor planets and can range down to the size of a dust particle. Asteroid belts form from primordial solar nebulae as a group of planetesimals, the smaller precursors of planets, which in turn formed protoplanets; however, gravitational perturbations from large planets, such as gas giants, imbue the protoplanets with too much orbital energy for them to accrete into a planet. Collisions become too violent, and instead of fusing together, the planetesimals and most of the protoplanets shatter, forming an orbital ring of debris. '''Inhabitable when pressurized'''|| Inner, Green, Outer, Far || Carbonaceous, silicate and metallic materials || None || [[File:Asteroid belt.png<ins style="font-weight: bold; text-decoration: none;">|200px</ins>]]</div></td></tr>
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</table>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43321&oldid=prevDan at 12:25, 23 January 20252025-01-23T12:25:02Z<p></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable''' || Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable''' || Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td></tr>
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<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class V''' (''Vokaya'') || '''Super Terrestrial'''<br> With a mass greater than terrestrial planets but substantially less than Class I ice giants, Class V planets range from two to ten times the mass of a typical Class M terrestrial with diameters between 1 and 2.5 times the standard. They can have diverse compositions, including rocky, metallic, water-rich, or even gaseous, depending on their density and formation history. '''Class <del style="font-weight: bold; text-decoration: none;">Va</del>''' generally have atmospheres like a gas giant of hydrogen, helium, and trace gases, which account for anywhere from one to five percent of the planet’s mass; '''Class <del style="font-weight: bold; text-decoration: none;">Vb</del>''' have an atmosphere like a terrestrial planet. The entire class tend to orbit closer to their host stars, within the near and inner zones. <br>'''Noted features:''' large, may resemble either a smaller gas giant or an extremely large terrestrial, '''uninhabitable''' || Near, Inner, Green || thin crusts and varies from deep planet-wide oceans to a surface riddled with volcanoes and prone to frequent quakes. || Layers of water, hydrogen, and helium || [[File:Super terrestrial (Class V).png|200px]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class V''' (''Vokaya'') || '''Super Terrestrial'''<br> With a mass greater than terrestrial planets but substantially less than Class I ice giants, Class V planets range from two to ten times the mass of a typical Class M terrestrial with diameters between 1 and 2.5 times the standard. They can have diverse compositions, including rocky, metallic, water-rich, or even gaseous, depending on their density and formation history. '''Class <ins style="font-weight: bold; text-decoration: none;">V1</ins>''' generally have atmospheres like a gas giant of hydrogen, helium, and trace gases, which account for anywhere from one to five percent of the planet’s mass; '''Class <ins style="font-weight: bold; text-decoration: none;">V2</ins>''' have an atmosphere like a terrestrial planet. The entire class tend to orbit closer to their host stars, within the near and inner zones. <br>'''Noted features:''' large, may resemble either a smaller gas giant or an extremely large terrestrial, '''uninhabitable''' || Near, Inner, Green || thin crusts and varies from deep planet-wide oceans to a surface riddled with volcanoes and prone to frequent quakes. || Layers of water, hydrogen, and helium || [[File:Super terrestrial (Class V).png|200px]]</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class W''' (''Wuhlek'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:Brown dwarf.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class W''' (''Wuhlek'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:Brown dwarf.png|200px]]</div></td></tr>
</table>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43320&oldid=prevDan at 12:22, 23 January 20252025-01-23T12:22:20Z<p></p>
<a href="http://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43320&oldid=43317">Show changes</a>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43317&oldid=prevDan at 11:37, 23 January 20252025-01-23T11:37:41Z<p></p>
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 04:37, 23 January 2025</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class T''' (''Taurik'') <br>(''ex: [[Kappa Andromedae b]]'') || '''Ultragiant'''<br>If a Class S planet gains matter by consuming other planets or dust in a star system, it can keep growing to a Class T. These planets are the size of small stars (between 4,161,000 and 5,200,000 kms radius and largest of the "gas giants") and are right on the edge of critical mass. Once they reach it, the planet collapses in on itself, becoming a young star. Due to the extremely strong gravimetric sheer that develop between the Class T and its parent star(s), satellites don't tend to get captured by it, but get flung away or pulled right in.<br>'''Noted features:''' largest giant, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates considerable heat || Variable pressure and composition; may contain water vapor || [[File:Class T.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class T''' (''Taurik'') <br>(''ex: [[Kappa Andromedae b]]'') || '''Ultragiant'''<br>If a Class S planet gains matter by consuming other planets or dust in a star system, it can keep growing to a Class T. These planets are the size of small stars (between 4,161,000 and 5,200,000 kms radius and largest of the "gas giants") and are right on the edge of critical mass. Once they reach it, the planet collapses in on itself, becoming a young star. Due to the extremely strong gravimetric sheer that develop between the Class T and its parent star(s), satellites don't tend to get captured by it, but get flung away or pulled right in.<br>'''Noted features:''' largest giant, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates considerable heat || Variable pressure and composition; may contain water vapor || [[File:Class T.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable''' || Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class V''' (''Vokaya'') || '''Super <del style="font-weight: bold; text-decoration: none;">Tellurian</del>'''<br><del style="font-weight: bold; text-decoration: none;">Cool and low-</del>mass <del style="font-weight: bold; text-decoration: none;">(in relation to other gas </del>giants<del style="font-weight: bold; text-decoration: none;">)</del>, Class <del style="font-weight: bold; text-decoration: none;">U </del>planets <del style="font-weight: bold; text-decoration: none;">have cores made up </del>of <del style="font-weight: bold; text-decoration: none;">rock and ice, </del>with <del style="font-weight: bold; text-decoration: none;">atmospheric layers of mostly hydrogen </del>and <del style="font-weight: bold; text-decoration: none;">helium</del>. They <del style="font-weight: bold; text-decoration: none;">are large planets (between 25</del>,<del style="font-weight: bold; text-decoration: none;">000 </del>and <del style="font-weight: bold; text-decoration: none;">75</del>,<del style="font-weight: bold; text-decoration: none;">000 kms radius</del>, <del style="font-weight: bold; text-decoration: none;">4th largest "gas giants")</del>, <del style="font-weight: bold; text-decoration: none;">generally larger than </del>Class <del style="font-weight: bold; text-decoration: none;">I ice giants</del>, and <del style="font-weight: bold; text-decoration: none;">are more often found in the interior orbits of younger solar systems</del>.<br>'''Noted features:''' large, gas <del style="font-weight: bold; text-decoration: none;">planet</del>, '''uninhabitable'''|| <del style="font-weight: bold; text-decoration: none;">Green</del>, <del style="font-weight: bold; text-decoration: none;">Outer </del>|| <del style="font-weight: bold; text-decoration: none;">Comprised of gaseous hydrogen </del>and <del style="font-weight: bold; text-decoration: none;">hydrogen compounds; radiates some heat </del>|| <del style="font-weight: bold; text-decoration: none;">Variable pressure </del>and <del style="font-weight: bold; text-decoration: none;">composition </del>|| [[File:Class <del style="font-weight: bold; text-decoration: none;">U</del>.png|200px]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class V''' (''Vokaya'') || '''Super <ins style="font-weight: bold; text-decoration: none;">Terrestrial</ins>'''<br> <ins style="font-weight: bold; text-decoration: none;">With a </ins>mass <ins style="font-weight: bold; text-decoration: none;">greater than terrestrial planets but substantially less than Class I ice </ins>giants, Class <ins style="font-weight: bold; text-decoration: none;">V </ins>planets <ins style="font-weight: bold; text-decoration: none;">range from two to ten times the mass </ins>of <ins style="font-weight: bold; text-decoration: none;">a typical Class M terrestrial </ins>with <ins style="font-weight: bold; text-decoration: none;">diameters between 1 </ins>and <ins style="font-weight: bold; text-decoration: none;">2.5 times the standard</ins>. They <ins style="font-weight: bold; text-decoration: none;">can have diverse compositions, including rocky, metallic, water-rich, or even gaseous</ins>, <ins style="font-weight: bold; text-decoration: none;">depending on their density </ins>and <ins style="font-weight: bold; text-decoration: none;">formation history. '''Class Va''' generally have atmospheres like a gas giant of hydrogen</ins>, <ins style="font-weight: bold; text-decoration: none;">helium</ins>, <ins style="font-weight: bold; text-decoration: none;">and trace gases</ins>, <ins style="font-weight: bold; text-decoration: none;">which account for anywhere from one to five percent of the planet’s mass; '''</ins>Class <ins style="font-weight: bold; text-decoration: none;">Vb''' have an atmosphere like a terrestrial planet. The entire class tend to orbit closer to their host stars</ins>, <ins style="font-weight: bold; text-decoration: none;">within the near </ins>and <ins style="font-weight: bold; text-decoration: none;">inner zones</ins>. <br>'''Noted features:''' large, <ins style="font-weight: bold; text-decoration: none;">may resemble either a smaller </ins>gas <ins style="font-weight: bold; text-decoration: none;">giant or an extremely large terrestrial</ins>, '''uninhabitable''' || <ins style="font-weight: bold; text-decoration: none;">Near</ins>, <ins style="font-weight: bold; text-decoration: none;">Inner </ins>|| <ins style="font-weight: bold; text-decoration: none;">thin crusts and varies from deep planet-wide oceans to a surface riddled with volcanoes </ins>and <ins style="font-weight: bold; text-decoration: none;">prone to frequent quakes. </ins>|| <ins style="font-weight: bold; text-decoration: none;">Layers of water, hydrogen, </ins>and <ins style="font-weight: bold; text-decoration: none;">helium </ins>|| [[File:<ins style="font-weight: bold; text-decoration: none;">Super terrestrial (</ins>Class <ins style="font-weight: bold; text-decoration: none;">V)</ins>.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class W''' (''Wuhlek'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:Brown dwarf.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class W''' (''Wuhlek'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:Brown dwarf.png|200px]]</div></td></tr>
</table>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43315&oldid=prevDan at 10:54, 23 January 20252025-01-23T10:54:03Z<p></p>
<table style="background-color: #fff; color: #202122;" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 03:54, 23 January 2025</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class T''' (''Taurik'') <br>(''ex: [[Kappa Andromedae b]]'') || '''Ultragiant'''<br>If a Class S planet gains matter by consuming other planets or dust in a star system, it can keep growing to a Class T. These planets are the size of small stars (between 4,161,000 and 5,200,000 kms radius and largest of the "gas giants") and are right on the edge of critical mass. Once they reach it, the planet collapses in on itself, becoming a young star. Due to the extremely strong gravimetric sheer that develop between the Class T and its parent star(s), satellites don't tend to get captured by it, but get flung away or pulled right in.<br>'''Noted features:''' largest giant, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates considerable heat || Variable pressure and composition; may contain water vapor || [[File:Class T.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class T''' (''Taurik'') <br>(''ex: [[Kappa Andromedae b]]'') || '''Ultragiant'''<br>If a Class S planet gains matter by consuming other planets or dust in a star system, it can keep growing to a Class T. These planets are the size of small stars (between 4,161,000 and 5,200,000 kms radius and largest of the "gas giants") and are right on the edge of critical mass. Once they reach it, the planet collapses in on itself, becoming a young star. Due to the extremely strong gravimetric sheer that develop between the Class T and its parent star(s), satellites don't tend to get captured by it, but get flung away or pulled right in.<br>'''Noted features:''' largest giant, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates considerable heat || Variable pressure and composition; may contain water vapor || [[File:Class T.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek<del style="font-weight: bold; text-decoration: none;">-ek'tra</del>'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class W''' (''Wuhlek<del style="font-weight: bold; text-decoration: none;">-yel</del>'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:Brown dwarf.png|200px]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">|'''Class V''' (''Vokaya'') || '''Super Tellurian'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</ins></div></td></tr>
<tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">|-</ins></div></td></tr>
<tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class W''' (''Wuhlek'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:Brown dwarf.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Y''' (''Yen'deshim'') <br>(''ex: ''[[Ha'Dara]], [[Tholia]], [[Visalayan]]'') || '''Demon'''<br>Class Y planets come in a range of sizes (1,000-10,000 kms), and while they have atmospheres, they are completely hostile to almost all known life. Radioactive, toxic air scours the surface at huge speeds. Temperature moves between huge highs and lows, and almost constantly covered in harsh storms, it would be better to be exposed to space than the surface of a Class Y.<br>'''Noted features:''' small & average sizes, average & thick atmospheres; extreme variances in high & low temperatures, rather geologically active, '''uninhabitable'''|| Inner, Green, Outer, Far || 500°K+ || Dense to extremely dense and turbulent, saturated with toxic chemicals and therionic radiation || [[File:Class Y.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Y''' (''Yen'deshim'') <br>(''ex: ''[[Ha'Dara]], [[Tholia]], [[Visalayan]]'') || '''Demon'''<br>Class Y planets come in a range of sizes (1,000-10,000 kms), and while they have atmospheres, they are completely hostile to almost all known life. Radioactive, toxic air scours the surface at huge speeds. Temperature moves between huge highs and lows, and almost constantly covered in harsh storms, it would be better to be exposed to space than the surface of a Class Y.<br>'''Noted features:''' small & average sizes, average & thick atmospheres; extreme variances in high & low temperatures, rather geologically active, '''uninhabitable'''|| Inner, Green, Outer, Far || 500°K+ || Dense to extremely dense and turbulent, saturated with toxic chemicals and therionic radiation || [[File:Class Y.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Z''' <br>(''ex: [[Sol V]]'')|| '''Asteroid Belt'''<br>Asteroid belts are the region of the a star system that inhabit orbits between planets and occupied by numerous irregularly shaped bodies called asteroids or minor planets and can range down to the size of a dust particle. Asteroid belts form from primordial solar nebulae as a group of planetesimals, the smaller precursors of planets, which in turn formed protoplanets; however, gravitational perturbations from large planets, such as gas giants, imbue the protoplanets with too much orbital energy for them to accrete into a planet. Collisions become too violent, and instead of fusing together, the planetesimals and most of the protoplanets shatter, forming an orbital ring of debris. '''Inhabitable when pressurized'''|| Inner, Green, Outer, Far || Carbonaceous, silicate and metallic materials || None || [[File:Asteroid belt.png]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Z''' <ins style="font-weight: bold; text-decoration: none;">(''Kohl-kov'')</ins><br>(''ex: [[Sol V]]'')|| '''Asteroid Belt'''<br>Asteroid belts are the region of the a star system that inhabit orbits between planets and occupied by numerous irregularly shaped bodies called asteroids or minor planets and can range down to the size of a dust particle. Asteroid belts form from primordial solar nebulae as a group of planetesimals, the smaller precursors of planets, which in turn formed protoplanets; however, gravitational perturbations from large planets, such as gas giants, imbue the protoplanets with too much orbital energy for them to accrete into a planet. Collisions become too violent, and instead of fusing together, the planetesimals and most of the protoplanets shatter, forming an orbital ring of debris. '''Inhabitable when pressurized'''|| Inner, Green, Outer, Far || Carbonaceous, silicate and metallic materials || None || [[File:Asteroid belt.png]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|}</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|}</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Background|{{PAGENAME}}]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Background|{{PAGENAME}}]]</div></td></tr>
</table>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43230&oldid=prevDan at 00:09, 22 January 20252025-01-22T00:09:45Z<p></p>
<table style="background-color: #fff; color: #202122;" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 17:09, 21 January 2025</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l49">Line 49:</td>
<td colspan="2" class="diff-lineno">Line 49:</td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek-ek'tra'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek-ek'tra'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|'''Class W''' (''Wuhlek-yel'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:<del style="font-weight: bold; text-decoration: none;">Class U</del>.png|200px]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|'''Class W''' (''Wuhlek-yel'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:<ins style="font-weight: bold; text-decoration: none;">Brown dwarf</ins>.png|200px]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Y''' (''Yen'deshim'') <br>(''ex: ''[[Ha'Dara]], [[Tholia]], [[Visalayan]]'') || '''Demon'''<br>Class Y planets come in a range of sizes (1,000-10,000 kms), and while they have atmospheres, they are completely hostile to almost all known life. Radioactive, toxic air scours the surface at huge speeds. Temperature moves between huge highs and lows, and almost constantly covered in harsh storms, it would be better to be exposed to space than the surface of a Class Y.<br>'''Noted features:''' small & average sizes, average & thick atmospheres; extreme variances in high & low temperatures, rather geologically active, '''uninhabitable'''|| Inner, Green, Outer, Far || 500°K+ || Dense to extremely dense and turbulent, saturated with toxic chemicals and therionic radiation || [[File:Class Y.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Y''' (''Yen'deshim'') <br>(''ex: ''[[Ha'Dara]], [[Tholia]], [[Visalayan]]'') || '''Demon'''<br>Class Y planets come in a range of sizes (1,000-10,000 kms), and while they have atmospheres, they are completely hostile to almost all known life. Radioactive, toxic air scours the surface at huge speeds. Temperature moves between huge highs and lows, and almost constantly covered in harsh storms, it would be better to be exposed to space than the surface of a Class Y.<br>'''Noted features:''' small & average sizes, average & thick atmospheres; extreme variances in high & low temperatures, rather geologically active, '''uninhabitable'''|| Inner, Green, Outer, Far || 500°K+ || Dense to extremely dense and turbulent, saturated with toxic chemicals and therionic radiation || [[File:Class Y.png|200px]]</div></td></tr>
</table>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43228&oldid=prevDan at 23:50, 21 January 20252025-01-21T23:50:02Z<p></p>
<table style="background-color: #fff; color: #202122;" data-mw="interface">
<col class="diff-marker" />
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<tr class="diff-title" lang="en">
<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 16:50, 21 January 2025</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l48">Line 48:</td>
<td colspan="2" class="diff-lineno">Line 48:</td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek-ek'tra'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class U''' (''Um-sfek-ek'tra'') || '''Low Density Giant'''<br>Cool and low-mass (in relation to other gas giants), Class U planets have cores made up of rock and ice, with atmospheric layers of mostly hydrogen and helium. They are large planets (between 25,000 and 75,000 kms radius, 4th largest "gas giants"), generally larger than Class I ice giants, and are more often found in the interior orbits of younger solar systems.<br>'''Noted features:''' large, gas planet, '''uninhabitable'''|| Green, Outer || Comprised of gaseous hydrogen and hydrogen compounds; radiates some heat || Variable pressure and composition || [[File:Class U.png|200px]]</div></td></tr>
<tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">|-</ins></div></td></tr>
<tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">|'''Class W''' (''Wuhlek-yel'') || '''Brown Dwarf'''<br>Substellar objects that occupy the mass range between the Class T ultragiants and the smallest stars, though their radii fall strictly within the range of 62,000 and 76,000 kms. They form like stars through the collapse of gas clouds, but lack sufficient mass to sustain hydrogen fusion in their cores. Brown dwarfs are characterized by their ability to fuse deuterium and, in more massive cases, lithium. They emit minimal visible light, primarily radiating in the infrared spectrum, and gradually cool over time. Unlike planets, brown dwarfs can generate their own heat and light through internal processes, albeit at much lower levels than true stars<br>'''Noted features:''' large (for planet), failed star, '''uninhabitable'''|| Near, Inner, Green, Outer || Comprised of gaseous hydrogen and hydrogen; radiates heat through some fusion but primarily gravitic pressure|| Variable pressure and composition || [[File:Class U.png|200px]]</ins></div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|-</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Y''' (''Yen'deshim'') <br>(''ex: ''[[Ha'Dara]], [[Tholia]], [[Visalayan]]'') || '''Demon'''<br>Class Y planets come in a range of sizes (1,000-10,000 kms), and while they have atmospheres, they are completely hostile to almost all known life. Radioactive, toxic air scours the surface at huge speeds. Temperature moves between huge highs and lows, and almost constantly covered in harsh storms, it would be better to be exposed to space than the surface of a Class Y.<br>'''Noted features:''' small & average sizes, average & thick atmospheres; extreme variances in high & low temperatures, rather geologically active, '''uninhabitable'''|| Inner, Green, Outer, Far || 500°K+ || Dense to extremely dense and turbulent, saturated with toxic chemicals and therionic radiation || [[File:Class Y.png|200px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|'''Class Y''' (''Yen'deshim'') <br>(''ex: ''[[Ha'Dara]], [[Tholia]], [[Visalayan]]'') || '''Demon'''<br>Class Y planets come in a range of sizes (1,000-10,000 kms), and while they have atmospheres, they are completely hostile to almost all known life. Radioactive, toxic air scours the surface at huge speeds. Temperature moves between huge highs and lows, and almost constantly covered in harsh storms, it would be better to be exposed to space than the surface of a Class Y.<br>'''Noted features:''' small & average sizes, average & thick atmospheres; extreme variances in high & low temperatures, rather geologically active, '''uninhabitable'''|| Inner, Green, Outer, Far || 500°K+ || Dense to extremely dense and turbulent, saturated with toxic chemicals and therionic radiation || [[File:Class Y.png|200px]]</div></td></tr>
</table>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43212&oldid=prevDan at 22:18, 21 January 20252025-01-21T22:18:34Z<p></p>
<a href="http://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43212&oldid=43211">Show changes</a>Danhttp://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43211&oldid=prevDan at 21:50, 21 January 20252025-01-21T21:50:58Z<p></p>
<a href="http://starshiptracker.com/sfcwiki/index.php?title=Planetary_Classifications&diff=43211&oldid=43210">Show changes</a>Dan