NS-NS Merger (Mag. Flux Change)

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Summary Table
Category Progenitor Type Energy Mechanism Emission Mechanism Counterparts References Brief Comments
LF Radio HF Radio Microwave Terahertz Optical/IR X-rays Gamma-rays Gravitational Waves Neutrinos
Merger NS-NS Both Mag. flux change -- Yes Yes -- -- Kilonova Afterglow sGRB
if jet aligned
Yes -- http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1701.02492 In dense stellar clusters

Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)

Model Description

A close encounter between two NSs results in the formation of highly elongated orbits, continuously shrinking due to dissipation through gravitational waves. As the orbital separation decreases, the changing magnetic flux bunches particles, which then radiate coherently. The NSs will approach each other several times, during which their respective magnetospheres will interact, leading to several FRBs before the final merger.

Observational Constraints

The expectation is that FRBs would be localized to centers of galaxies, or at least would be clustered with stellar density.