SSPSF model
0SSPSF model, by Wikipedia https://en.wikipedia.org/wiki?curid=10062061 / CC BY SA 3.0
#Star_formation
The SSPSF （stochastic self-propagating star formation） model of star formation was proposed by Mueller & Arnett in 1976, generalized afterward by Gerola & Seiden in 1978 and Gerola, Seiden, & Schulman in 1980.
This model proposes that star formation propagates via the action of shock waves produced by stellar winds and supernovae traversing the gas that composes the interstellar medium.
The Henize 206 nebula provides a clear example.
In particular, 24μ infrared （MIPS） emission shows where a new generation of stars heats the remains of the supernova remnant that induced their formation.
In contrast to star formation in density-wave theories, which are limited to disk-shaped galaxies and produce global spiral patterns,
SSPSF applies equally well to spirals, to irregular galaxies and to any local concentrations of gas in elliptical galaxies.
The effect may be envisioned as an "SIR infection model" in a differentially rotating disk, the host galaxy.
The SIR model （perhaps most popularly familiar in the form of Conway's Game of Life） is applied to star formation propagating through the galaxy: Each generation of stars in a neighborhood includes some massive ones whose stellar winds and,
soon, supernovae, produce shock waves in the gas （Susceptible material）.
These lead to collapsing nearby gas clouds, which produce the next generation of stars （Infection propagation）; but in the immediate neighborhood,
all initially available gas is used, so no further stars are born there for some period of time despite the shocks （Recovery from infection）.
SSPSF simulation In a non-flattened galaxy, the infection would produce an outward propagating sphere.
In a non-rotating flattened （disk） environment, the infection would produce an outward propagating ring.
But in a differentially rotating flattened environment, i.
e.
, with mass closer to the galactic center orbiting the center so...
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