Random Planet Generator

Planet

This planet orbits a main sequence star of spectral class ??V — meaning that it appears ? times as bright as the Sun, ? times as as large, and ? as massive.

On average, a star of that kind exists for about billion years.
Your star's own age is % of that, or about million years.

An Earth-like planet could exist between A.U. and A.U. from the star (assuming no other stellar companions), with an ideal distance of A.U.
A condition similiar to that of Venus would lie at A.U. from the star, while a condition similar to that of Mars would lie at A.U. away.

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Inner Planets: - planets that lie within the "frost line" where planetary formation starts to be dominated by ice.
Rocky: - while terrestrial planets are typically composed of rock and metal, in this case "Rocky" inner planetoids are distinguished as planets without an atmosphere,
(e.g.) Mercury or Ceres.
Terrestrial: - a rocky planet with an atmosphere. These tend to lie within the so-called "habitable" or "water" zone and have a substantial mass to retain gasses.
Terrestrial planets, defined here, include Venusian, Martian, Earth-like, or other planetary variations.
note: Picking this option might produce a habitable planet, but it is not guaranteed.; -- special case: Habitable Earth-like worlds: these are designed to be more friendly to Earthlike conditions, but can still be somewhat extreme.; -- special case: Gaia worlds: these are designed to be very friendly to Earthlike conditions as we know it.
Water: - planets whose surface is dominated by 90% or more liquid (typically but not exclusively H₂0). These tend to be high in mass and orbit closer to the parent star than the "frost line".
Gas Giant (typical medium jovial): - planets made up of mostly hydrogen and helium, with a mantle containing metallic hydrogen.
(e.g. Jupiter, Saturn)
Gas Sub-Giant (small jovial): - sometimes called "ice giants" instead, planets whose atmosphere made up of hydrogen and helium, but substantially other ices, like methane, ammonia, and various hydrocarbons.
(e.g. Uranus and Neptune)
Gas Super-Giant (huge jovial): - sometimes called "super-Jupiters", these are gas giants with masses several times that of Jupiter. They are so massive that they almost became stars, but couldn't initiate stellar fusion. On the upper scale, they are brown dwarfs that still radiate heat.
Asteroid: - represents the non-planetoid, irregular shaped objects not orbiting as the satellites of other planetoids. (e.g. 243 Ida)
Ice: - more often formally called "Plutoids", "Trans-Neptunian objects", "cubewano" or other various names, these are planetoids beyond the "frost line" whose surface is composed of various ices. For this reason, they are distinct from other dwarf planets (like Ceres) and may have transient atmospheres. While most examples here are of dwarf planets, the definition here includes any planet dominated by ice on the surface and atmosphere.
(e.g. most Kupier Belt objects, like Pluto, Eris, Sedna, Makemake, Haumea, Charon).
Moons: Gigantic moons hypothetical satellites found only around huge super-giant jovial planets, they can be as large as Mars (6780 km dia), have an atmosphere, and may even possess tiny sub-moons of their own.
Huge moons (e.g. Ganymede, Titan) are so large (4000+ km dia), they are even larger than some planets, like Mercury.
Large moons (e.g. Earth's Moon, Triton) (2000-4000 km dia), are rare, but even moreso for terrestrial planets, like Earth.
Medium moons (e.g. Rhea, Charon) (1000-2000 km dia) are more typical of the smaller jovians, but also observed as moons of Kuiper objects (Charon).
Small moons (e.g. Enceladus, Amalthea, Mimas, Prometheus)(100-1000 km dia) make up more quantity of satellites, but often are barely a fraction of a planetary system's total mass. Most are irregular in shape.
Tiny moons (e.g. Phobos & Deimos, Leda)(1-100 km dia) are most likely captured asteroids, left over planetary debris, or fragments of larger moon collisions.
Several may even be pulled out of their current observed orbits.
Astronomical Unit (A.U.): - The average distance of the Earth to the Sun. 1 A.U. = 149,600,000 km = 92,957,130 miles. To put it another way, it takes light from the sun a bit over 8 minutes to reach Earth.
E's: - Earths (i.e. any property, like size, atmosphere, mass, gravity, etc. relative to that of Earth – it makes comparisons more relatable to what we know rather than spouting out millions of unit measures.)
Earth Masses (EM's): - A relatable way to compare a planet's mass to Earth's. A planet with 1.50 EM is 50% heavier than our Earth. It also makes doing the math easier, too.
Earth Radii (ER's) or Earth Diameters (ED's): - A relatable way to compare a planet's size to Earth's. A planet with 2.00 ER is twice the size of Earth.
(Note: Diameter is the distance from one edge to the other. Radius is the distance from the center to the edge. Doubling the radius also doubles the diameter—trust me, it's a geometry thing.)
g's (Gee's) or Earth Gravities: - A relatable way to compare a planet's gravitation to Earth's. A planet with 1.10 g pulls on a mass 10% more than Earth. This means that a 100 lbf (pounds-force = 444.8 N) weight on Earth will weigh 110 lbf (489.3 N) on your planet. A mass of 100 kg on Earth will still be 100 kg on your planet, but its weight (force = mass × gravity) will feel like about W ≈ 100 kg × 9.81 m/sec² × 1.10 = 1079.1 N

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