The Daemon Kernel of the Sun
| dc.creator | Drobyshevski, E. M. | |
| dc.date | 2002-05-21 | |
| dc.date.accessioned | 2026-07-07T11:28:54Z | |
| dc.date.available | 2026-07-07T11:28:54Z | |
| dc.description | The daemon-stimulated proton decay is capable of providing an appreciable part of the Sun luminosity as well as nonelectron flavor component in the solar neutrino flux. This follows (1) from our experiments on detection of negative daemons in Earth-crossing orbits, which give ~1 microsec for the decay time of a daemon-containing proton, and (2) from an estimate of the total number of daemons which could be captured by the Sun from the Galactic disk (up to \~2.4E30). Because of their huge mass (~3E-5 g), the captured daemons form in the Sun's center a kernel a few cm in size. The protons diffuse into the kernel to decay there with a release of energy. Physically sound estimates of the parameters of the kernel can be obtained if it consists mainly of negative daemons. Proton decay maintains a high temperature of the daemon gas (up to \~1E11-1E12 K), which makes it physically collisionless and prevents kernel collapse into a black hole. | |
| dc.description | 11 pages | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0205353 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0205353 | |
| dc.identifier | Astron.Astrophys.Trans.23:173-183,2004 | |
| dc.identifier | doi:10.1080/10556790310001612535 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/196550 | |
| dc.subject | Astrophysics | |
| dc.title | The Daemon Kernel of the Sun | |
| dc.type | text |