José C. N. de Araujo

THE INFLUENCE OF QUANTUM VACUUM FRICTION ON PULSARS

We firstly revisit the energy loss mechanism known as quantum vacuum friction (QVF), clarifying some of its subtleties. Then we investigate the observables that could easily differentiate QVF from the classical magnetic dipole radiation for pulsars with braking indices (n) measured accurately. We show this is specially the case for the time evolution of a pulsars magnetic dipole direction (

Detectability of f-mode unstable neutron stars by the Schenberg spherical antenna

\dot{\phi}

Gravitational wave emission by the high braking index pulsar PSR J1640-4631

) and surface magnetic field (

Gravitational waves from pulsars with measured braking index

\dot{B}_0

GRAVITATIONAL WAVES FROM PULSARS AND THEIR BRAKING INDICES: THE ROLE OF A TIME DEPENDENT MAGNETIC ELLIPTICITY

). As it is well known in the context of the classic magnetic dipole radiation,

Collapse of primordial clouds — II. The role of dark matter

n 0

A Possible Dynamical Effect of a Primordial Magnetic Field

(

A perturbative solution for gravitational waves in quadratic gravity

\dot{\phi}>0

Possible Strong Gravitational Wave Sources for the LISA Antenna

) when

Determining the neutron star equation of state using the narrow-band gravitational wave detector Schenberg

\phi