Effects of proton decay on the cosmological future
Abstract
Upon calculating matter and radiation densities for the case of an open universe where the proton lifetime is 10 to the 30th years, and considering the contribution to these densities from the decay of matter in both clumps and interstellar gas, it is found that for times shorter than the proton lifetime, proton decay keeps dead stars at a few K and neutron stars at about 100 K. For times much greater than the proton lifetime, and a Robertson-Walker metric geometric constant value smaller than zero, the energy density of the universe is eventually dominated by the contribution of a tenuous e(+)e(-) plasma that is too thin for direct e(+)e(-) annihilation, and perhaps too thin for gravitational collapse. The cycle expansion factor alpha for the case of a closed universe is computed, taking into account entropy production by both stellar nucleosynthesis and proton decay.
- Publication:
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The Astrophysical Journal
- Pub Date:
- January 1982
- DOI:
- Bibcode:
- 1982ApJ...252....1D
- Keywords:
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- Cosmology;
- Interstellar Gas;
- Nuclear Fusion;
- Protons;
- Radioactive Decay;
- Stellar Evolution;
- Baryons;
- Electron-Positron Plasmas;
- Gravitational Collapse;
- Neutron Stars;
- Photons;
- Stellar Temperature;
- Universe;
- White Dwarf Stars;
- Astrophysics