Pulsar rotation with superfluid entrainment

Abstract

Large pulsar glitches (like the ones detected in the Vela) are though to be a consequence of the superfluid component present in the interior of mature neutron stars. However strong entrainment challenges this picture. We study the impact of entrainment on the angular momentum that can be exchanged between the normal component and the superfluid during a glitch by means of a consistent global model. This allows to estimate the maximum angular momentum reservoir stored into the superfluid component of the star: the essential ingredient are newly calculated mesoscopic pinning forces that block the superfluid vorticity in the crust of the neutron star. This method can also provide a quantitative test for global models of rotating neutron stars, as well as for microphysical inputs present in literature (like entrainment parameters and pinning forces).

To be published in Journal of Physics: Conference Series (IOP). Conference: "Compact Stars in the QCD phase diagram V" and "Working Group 2 Meeting of COST Action MP1304", 23-27 May 2016 (GSSI and LNGS, L'Aquila)

References in corpus (8)

• Models of Pulsar Glitches
• Neutron conduction in the inner crust of a neutron star in the framework of the band theory of solids
• Crustal Entrainment and Pulsar Glitches
• Avalanche dynamics of radio pulsar glitches
• Transitions between turbulent and laminar superfluid vorticity states in the outer core of a neutron star
• Unpinning triggers for superfluid vortex avalanches
• Vortex Creep Against Toroidal Flux Lines, Crustal Entrainment, and Pulsar Glitches
• Entrainment parameters in cold superfluid neutron star core