1 | Lattice energy including finite size effects is given by Equation (41![]() |
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2 | “free” means here that the electrons are not bound. However, they are interacting with other electrons and with the atomic lattice. | |
3 | We restrict ourselves to type I X-ray bursts. There are two X-ray bursters that are of type II, with bursts driven not by thermonuclear flashes on the neutron star surface, but originating in the accretion disk itself. | |
4 | In this section, by “energy” we will usually mean energy of a unit volume (i.e. energy density). | |
5 | Such pressures are very small in the context of neutron stars. For iron at room temperature they correspond to a density of about 8.2 g cm–3, in comparison to 7.86 g cm–3 under normal atmospheric pressure [42]. | |
6 | For a body-centered–cubic lattice, the lattice spacing ![]() ![]() ![]() |
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7 | The Fermi surface is the surface in ![]() ![]() |
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8 | In the case of fermionic superfluids, the superfluid particles are fermion pairs. | |
9 | For a proton superconductor, ![]() ![]() ![]() ![]() |
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10 | For instance at ![]() ![]() ![]() |
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11 | Entrainment effects disappear as ![]() ![]() ![]() ![]() |
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12 | This assumption may not remain valid in the “nuclear pasta” layers at the bottom of the crust discussed in Section 3.3. | |
13 | Ion contribution to ![]() ![]() ![]() |
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14 | The gyromagnetic frequency of electrons should not be confused with the electron cyclotron frequency ![]() |
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