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 pulsar's magnetic dipole direction ($\dotϕ$) and surface magnetic field ($\dot{B}_0$). As it is well known in the context of the classic magnetic dipole radiation, $n<3$ would only be possible for positive $(\dot{B}_0/B_0 + \dotϕ/\tanϕ)$, which, for instance, leads to $\dot{B}_0>0$ ($\dotϕ>0$) when $ϕ$ ($B_0$) is constant. On the other hand, we show that QVF can result in very contrasting predictions with respect to the above ones. Finally, even in the case $\dot{B}_0$ in both aforesaid models for a pulsar has the same sign, for a given $ϕ$, we show that they give rise to different associated timescales, which could be another way to falsify QVF.

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