ONE/4 Planetary Orbits
STEP ONE: Determine the number of potential orbits by rolling on table 1.4.1.
STEP TWO: Determine the mean distance of the orbits by consulting the formulae under 1.4.2.
STEP THREE: Remove all impossible orbits. This includes any orbit which would put a planet within a star's radius or so close as to vaporize it, and any orbit which is unstable in a binary system (between the binary's closest separation / 3 and the furthest separation x 3 distance). Worlds may orbit both stars in a binary, if the more massive companion has any orbits generated beyond the furthest separation distance x 3. Only consider such orbits for the more massive companion. For white dwarves, remove all orbits within the limit provided by table 1.4.3.
STEP FOUR: Remove all orbits where a planet would be vaporized, according to the formulae in 1.4.4. Also, determine the limit of the original inner system. Note this limit, it will be used in the next section.
INNER SYSTEM ZONE:
The area of the stellar system where the early system is too hot to allow icy planetoids. Inner system objects thus have higher density and mostly consist of silicates and metals, while the area outside is more dominated by frozen water and gasses.
STARS WITHOUT PLANETARY ORBITS:
There may be some other objects around these stars, typically either a few icy chunks in distant random orbits (1d10 x 1d10 AU) or more rarely a captured planetoid. Captured planetoids have eccentric orbits (1D10 AU) and may be of any general planet type. Some planetless stars have very sparse "rings" of chunks of debris:
If any orbits where removed by the binary effects, the system is likely to have a fair deal of stray asteroids and debris.