Speaker
Cecilia Chirenti
(Federal University of ABC, Santo André, Brazil)
Description
Newly born neutron stars can present differential rotation, even if later it should be suppressed by viscosity or a sufficiently strong magnetic field. And in this early stage of its life, a neutron star is expected to have a strong emission of gravitational waves, which could be influenced by the differential rotation. We present here a new formalism for modelling differentially rotating neutron stars, working on the slow rotation approximation and assuming a small degree of differential rotation. After we establish our equilibrium model, we explore the influence of the differential rotation on the f and r-modes of oscillation of the neutron star in the Cowling approximation, and we also analyze an effect of the differential rotation on the emission of gravitational radiation from the f-modes. Finally, we introduce magnetic fields in our model to aiming to consider their influence in the frequencies of the oscillations.
Primary author
Cecilia Chirenti
(Federal University of ABC, Santo André, Brazil)
Co-authors
Jozef Skakala
(Federal University of ABC, Santo André, Brazil)
Luciano Rezzolla
(Max Planck Institute for Gravitational Physics, AEI Potsdam, Germany)
Shin'ichirou Yoshida
(University of Tokyo, Japan)
