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What allows neutron stars to overcome the degeneracy pressure? Does the electron get so close to the proton that it gets absorbed and then the pressure disappea
by changoplatanero 4y ago
What allows neutron stars to overcome the degeneracy pressure? Does the electron get so close to the proton that it gets absorbed and then the pressure disappears?
- deleted 4y ago[deleted]
- rayiner 4y agoYes, essentially. Degeneracy pressure arises as compression forces electrons into higher energy states to avoid being forced into the same quantum state (Pauli Exclusion principle). But at a certain point the gravitation pressure becomes so strong that protons capture electrons, producing a neutron and an electron neutrino, and relieving the electron degeneracy pressure. See: http://csep10.phys.utk.edu/OJTA2dev/ojta/c2c/neutron/neutronstars/degeneracy_tl.html http://csep10.phys.utk.edu/OJTA2dev/ojta/c2c/neutron/neutron...
- chaps 4y agoWhat happens to the neutrino at that point? Does it stay with the neutron star?
- rayiner 4y agoInitially they’re trapped but they play a major role in the supernova explosion that accompanies stellar collapse: https://indico.cern.ch/event/657167/contributions/2677895/attachments/1547824/2430987/CCSN_nu_production_16by9.pdf https://indico.cern.ch/event/657167/contributions/2677895/at...
- monus21 4y agoYes but after exceeding ~2 solar masses (Tolman–Oppenheimer–Volkoff limit) the neutron star will undergo further collapse to form a black hole.