Model
Digital Document
Publisher
Florida Atlantic University
Description
The propagation of shock and detonation waves through non-uniform dense
stellar material was numerically followed by characteristics. A number
of computations were performed for various initial shock strengths for
cases in which burning of materials was and was not present . For cases
in which burning was included, an analytic expression for the burning of
carbon was used. From such computations it was concluded that: (1)
due to the divergent nature of spherical systems and the subsequent decay
of shocks (for a region sufficiently close to the center of the star)
it may not be possible for the shock to support a steady detonation and
(2) after reaching a minimum strength, the shock may again accelerate,
thus forming a new detonation wave.
stellar material was numerically followed by characteristics. A number
of computations were performed for various initial shock strengths for
cases in which burning of materials was and was not present . For cases
in which burning was included, an analytic expression for the burning of
carbon was used. From such computations it was concluded that: (1)
due to the divergent nature of spherical systems and the subsequent decay
of shocks (for a region sufficiently close to the center of the star)
it may not be possible for the shock to support a steady detonation and
(2) after reaching a minimum strength, the shock may again accelerate,
thus forming a new detonation wave.
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