  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 $\beta$-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$^{-3}$ pc. The model allows indirect measurement of
neutron star magnetic fields and periods in addition to providing astronomical
measurements of $\beta$-decay chains of unstable neutron rich nuclei. Using
this model, we can calculate expected FRB average energies ($\sim$ 10$^{41}$
ergs), spectra shapes and provide a theoretical framework for determining
distances.

High Energy Astrophysical Phenomena;Nuclear Theory