Fast radio bursts from axion stars moving through pulsar magnetospheres. (arXiv:2004.06486v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Buckley_J/0/1/0/all/0/1">James H. Buckley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dev_P/0/1/0/all/0/1">P. S. Bhupal Dev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrer_F/0/1/0/all/0/1">Francesc Ferrer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_F/0/1/0/all/0/1">Fa Peng Huang</a>
We study the radio signals generated when an axion star enters into the
magnetosphere of a neutron star. As the axion star moves through the resonant
region where the plasma-induced photon mass becomes equal to the axion mass,
the axions can efficiently convert into photons, giving rise to an intense,
transient radio signal. The energy released is determined by the axion star
mass and conversion probability. Similarly, the peak frequency of the emitted
radio signal is fixed by the axion mass, while cosmological redshift and
Doppler shift could give rise to a wide range of frequencies. In particular, we
show that a dense axion star with a mass $sim 10^{-13}M_{odot}$ composed of
$sim 10: mu$eV axions can account for most of the mysterious fast radio
bursts in a wide frequency range.
We study the radio signals generated when an axion star enters into the
magnetosphere of a neutron star. As the axion star moves through the resonant
region where the plasma-induced photon mass becomes equal to the axion mass,
the axions can efficiently convert into photons, giving rise to an intense,
transient radio signal. The energy released is determined by the axion star
mass and conversion probability. Similarly, the peak frequency of the emitted
radio signal is fixed by the axion mass, while cosmological redshift and
Doppler shift could give rise to a wide range of frequencies. In particular, we
show that a dense axion star with a mass $sim 10^{-13}M_{odot}$ composed of
$sim 10: mu$eV axions can account for most of the mysterious fast radio
bursts in a wide frequency range.
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