出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：In this paper I will discuss how X-ray observations can be used to constrain the gravitational wave emission mechanisms and interior dynamics of superfluid neutron stars in accreting systems. I will briefly review the multifluid formalism for modelling superfluid neutron stars and then focus in particular on the r-mode instability. I will show that the "minimal" scenario, i.e. a neutron star composed exclusively of neutrons, protons (non superconducting) and electrons is not consistent with the observed temperatures and spins of the Low Mass X-ray Binaries, unless the crust is significantly more rigid than expected. An alternative is that the neutron star core may be contain hyperons or that it may be in a type II superconducting state, giving rise to strong vortex/flux tube interactions. Finally I will discuss how future X-ray missions such as LOFT or IXO and gravitational wave observations could help distinguish between the models.
