Abstract
The hypothesis explored in this article focuses on the outward-racing accretion shock produced in the course of a Type II supernova explosion. The shock arises in a massive giant star after the core collapse and hydrodynamic bounce. The piling up of material at the shock forms a shell of material which is subjected to an extremely high flux of neutrons. It is therefore rich in elements heavier than Iron - produced by r-process nucleosynthesis. The relatively small amount of material falling back from the volume inside the shell produces a planetary nebula around the central neutron star. The shell itself is ejected, and soon breaks up into gravitationally-bound fragments. Each fragment subsequently proceeds outward, sweeping up additional mass, to form a nebula surrounding a dominant, but relatively small central mass. It is shown that this scenario illustrates how stellar nebulae can be produced directly from Type II supernovae to form all known types of solar systems.
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Brown, W.K. (2002). The Birth of Planetary Systems Directly from Supernovae. In: Manuel, O. (eds) Origin of Elements in the Solar System. Springer, Boston, MA. https://doi.org/10.1007/0-306-46927-8_20
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DOI: https://doi.org/10.1007/0-306-46927-8_20
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