2010/07/31 by M. E. Gusakov, E. M. Kantor
Earth and Planetary Sciences · Engineering · Physics and Astronomy · #Astrophysics #Atomic and Subatomic Physics Research #Condensed matter physics #Decoupling (probability) #Engineering #High-pressure geophysics and materials #Neutron #Neutron star #Nuclear physics #Physics #Pulsars and Gravitational Waves Research #Quantum electrodynamics #Stars #Superfluidity #astro-ph.SR #physics.flu-dyn
paper · pdf · doi:10.1103/physrevd.83.081304
published as Phys.Rev.D83:081304(R),2011 · 5 pages, 2 figures; published version + mistake in Eq.(6) and a few typos are corrected; results unchanged
openalex publication_date 2011/04/22 · arxiv created 2012/01/18 · arxiv updated 2012/01/19 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We show that equations governing pulsations of superfluid neutron stars can be split into two sets of weakly coupled equations, one describing the superfluid modes and another one, the normal modes. The coupling parameter s is small, |s|\ensuremath∼0.01--0.05, for realistic equations of state. Already an approximation s=0 is sufficient to calculate the pulsation spectrum within the accuracy of a few percent. Our results indicate, in particular, that emission of gravitational waves from superfluid pulsation modes is suppressed in comparison to that from normal modes. The proposed approach allows to drastically simplify modeling of pulsations of superfluid neutron stars.