Quark Nova Model for Fast Radio Bursts
Abstract
FRBs are puzzling, millisecond, energetic radio transients with no discernible source; observations show no counterparts in other frequency bands. The birth of a quark star from a parent neutron star experiencing a quark nova - previously thought undetectable when born in isolation - provides a natural explanation for the emission characteristics of FRBs. The generation of unstable r-process elements in the quark nova ejecta provides millisecond exponential injection of electrons into the surrounding strong magnetic field at the parent neutron star's light cylinder via -decay. This radio synchrotron emission has a total duration of hundreds of milliseconds and matches the observed spectrum while reducing the inferred dispersion measure by approximately 200 cm pc. The model allows indirect measurement of neutron star magnetic fields and periods in addition to providing astronomical measurements of -decay chains of unstable neutron rich nuclei. Using this model, we can calculate expected FRB average energies ( 10 ergs), spectra shapes and provide a theoretical framework for determining distances.
Cite
@article{arxiv.1505.08147,
title = {Quark Nova Model for Fast Radio Bursts},
author = {Zachary Shand and Amir Ouyed and Nico Koning and Rachid Ouyed},
journal= {arXiv preprint arXiv:1505.08147},
year = {2016}
}
Comments
Updated Version: 18 pages, 9 figures, 2 tables; Style package (LaTeX macro) changed to RAA; Results unchanged; Discussion points added: other quark star observables, detailed light curve discussion (and figure), addition of rate estimate and clarifying additional clarifying comments. Original: 8 pages, 8 figures, 1 table