Reciprocal System Research Society

A supernova occurs in RS2 from a single cause: age-limit destruction of heavy elements at the stellar core. The age limit is the point at which the atom has accumulated sufficient isotope as to destabilize its rotational structure, destroying the rotating system and emitting it as particles and EM radiation, in massive quantities. This can occur under two, different conditions:

1. Class O (blue supergiant) stars that have reached their maximum mass, and as a result, the magnetic ionization level of the star becomes sufficient to cause age-limit detonation at the Nickel-Iron-Cobalt layer within the star, causing a supernova. These are the Type II supernovae of conventional astronomy.
2. A later-generation star. These supernova reconstructed stars start with a high concentration of heavy elements, already near their age limit and may become a supernova in any stellar class. These are the Type I supernovae.

(Larson labels stars with generations; the first generation is an aggregate that has not yet gone through the supernova and stellar reconstruction. The 2nd generation are normally the binary star pairs, the reconstruction of supernova debris back into stars. 3rd and later generations form multiple star groups. Larson also labels the spatial explosion the "A component" and the temporal explosion the "B component.")

The primary factor in the evolutionary speed of a star is the amount of matter available for it to consume. The more matter, the faster it will grow. As a result, stars present in nebula and dust clouds quickly move to the blue giant range and become supernovae. The most common example of this is when a globular cluster becomes trapped in the dust-filled galactic disk, becoming an open cluster. Red, globular clusters predominate outside the galactic disk and blue, open clusters predominate inside because of the availability of dust. Supernovae in red, globular clusters will be rare. Supernovae in the galactic disk will be common, and in the galactic core where there is a considerable quantity of heavy elements, very common (though not easily observed).