Energy release from magnetospheres deformed by gravitational waves. (arXiv:1812.06430v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Huiquan Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">Jiancheng Wang</a>
In this work, we consider the possibility of energy release in pulsar
magnetospheres deformed by gravitational waves from nearby sources. The strong
electromagnetic fields in the magnetospheres may release non-negligible energy
despite the weakness of the gravitational wave. When the background spacetime
is perturbed due to the passage of a gravitational wave, the original
force-free state of the inner magnetosphere will be slightly violated. The
plasma-filled magnetosphere tends to evolve into new force-free states as the
spacetime varies with time. During this process, a small portion of the
electromagnetic energy stored in the magnetosphere will be released to
acceleration of charged particles along the magnetic field lines. When the
pulsar is close enough to the gravitational wave source (e.g., $sim10^{-2}$ pc
to the gravitational wave sources observed recently), the resulting energy loss
rate is comparable with the radio luminosity of the pulsar. It is also noticed
that, under very stringent conditions (for magnetars with much shorter distance
to the sources), the released energy can reach the typical energy observed from
fast radio bursts (FRBs).
In this work, we consider the possibility of energy release in pulsar
magnetospheres deformed by gravitational waves from nearby sources. The strong
electromagnetic fields in the magnetospheres may release non-negligible energy
despite the weakness of the gravitational wave. When the background spacetime
is perturbed due to the passage of a gravitational wave, the original
force-free state of the inner magnetosphere will be slightly violated. The
plasma-filled magnetosphere tends to evolve into new force-free states as the
spacetime varies with time. During this process, a small portion of the
electromagnetic energy stored in the magnetosphere will be released to
acceleration of charged particles along the magnetic field lines. When the
pulsar is close enough to the gravitational wave source (e.g., $sim10^{-2}$ pc
to the gravitational wave sources observed recently), the resulting energy loss
rate is comparable with the radio luminosity of the pulsar. It is also noticed
that, under very stringent conditions (for magnetars with much shorter distance
to the sources), the released energy can reach the typical energy observed from
fast radio bursts (FRBs).
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