Some argue that the core of a neutron star, due to its high density, might be an ideal place for this phase transition to happen. So in short, the neutron star could "burn" into a quark star and produce an explosion. The Bodmer-Witten hypothesis is a bit controversial but has very interesting astrophysical imiclations.

May 20, 2022 · The HR diagram is an observational diagram.Whilst neutron stars could be placed in the HR diagram in the same way as white dwarf stars are, it turns out to be impractical to do so because the photospheric luminosity and photospheric temperature of neutron stars is next to impossible to determine.

Dec 4, 2014 · It is difficult to describe what it would inflate out into - the neutron star material can be imagined as an incredibly dense soup of neutrons with some protons and leptons in small numbers. The protons and leptons would make neutron-rich elements like deuterium , but most of the matter would consist of free neutrons.

Oct 26, 2014 · We think that most neutron stars are produced in the cores of massive stars and result from the collapse of a core that is already at a mass of $\sim 1.1-1.2 M_{\odot}$ and so as a result there is a minimum observed mass for neutron stars of about $1.2M_{\odot}$ (see for example Ozel et al. 2012).

May 23, 2014 · The gravitational wave signature of merging neutron stars and merging black holes of the same mass is, in principle different, because the neutron stars are subject to extreme tidal distortion. There may also be an electromagnetic signature, a "kilonova", from a disrupted neutron star that is not expected in the case of merging black holes.

Jul 25, 2015 · The neutron star mass is about 20% less than the mass of the original neutrons. That's significant. Note though that things can get a bit confusing because the zero level for gravitational potential energy is set at infinity. See hyperphysics. So we say that the gravitational potential energy of the neutrons in the neutron star is negative.

There are still plenty of protons and electrons (well ~10%). @WetSavannaAnimal one clue is that the direct URCA process could easily occur if the neutron star was not dominated by degenerate n. If the p/n ratio was high neutron stars would cool extremely fast. $\endgroup$ –

Dec 9, 2020 · $\begingroup$ Neutron stars have a charged components (mostly protons and electrons). For pure neutron matter, it is possible to consider non-minimal coupling of the neutron with the electromagnetic field (minimal coupling is via the monopole: the electric charge) Role of the vacuum energy in the thermodynamics of neutron matter.

Sep 17, 2016 · But as the neutron star cools, such that the neutrino energies fall below an MeV (even after a minute) and the constituent fermions become highly degenerate, then neutrino transparency can be safely assumed. Neutron stars do have an outer crust with non-degenerate nuclei and I would expect these to be a source of neutrino opacity.

Oct 15, 2021 · What supports neutron stars is the repulsion provided by the strong nuclear force between closely-packed neutrons. The central pressure in a neutron star is an order of magnitude higher than ideal neutron degeneracy pressure. no, it's not quark degeneracy pressure, it's actual forces due to gluon exchange.