Stellar Nucleosynthesis Reactions

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Why should we be concerned about where heavy elements—those with a proton number greater than 26—came from?

The supernova explosion model is shaky at best and really doesn’t appear to fit the observable data.

In order to solve this puzzle, secular science turned to stepwise direct nuclear reactions.

If the claimed velocity of the expanding material is based on either of these elements, then the temperature of the expanding supernova debris would be on the order of 2 × 10Fe nuclei but is enough to question the apparent contradiction with the searing gas cited in reference 5.

It’s also interesting that the observation of supernova debris from SN1987A only revealed approximately 1.3% of the Neutron Capture Models So, mainstream science is still faced with the conundrum of where the heavy elements came from.

Since 1957 everybody has spoken about s-process and r-process, but how are these processes realized in fact? more Nearly sixty years after BBFH [1], it is very important to re-investigate neutron capture processes.

Since 1957 everybody has spoken about s-process and r-process, but how are these processes realized in fact?

In neutron stars, the neutrons are typically in a 10 to 1 ratio with protons and electrons—so where do the elemental nuclei, which are just as necessary for the r-process as neutrons, come from?

And the ubiquitous question remains, how much was already there and how much formed from the collision?

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