Difference between revisions of "Pulsar-BH Interaction"

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Revision as of 09:28, 26 September 2018





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
Interaction Pulsar-BH Single -- -- Yes  ? -- -- -- -- -- Yes -- https://arxiv.org/abs/1711.09083

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


Model Description

An enhanced giant pulse generated by a rapidly spun-up neutron star near a spinning black hole could produce a single FRB. A gyroscope is used to model the pulsar's spin-precession, which has been shown to increase rapidly near the event horizon of a Kerr BH. Eventually the spin precession exceeds the pulsar's spin, and the latter can be neglected. As such, the pulsar magnetosphere is essentially rotating around the spin-precession axis. The rapid spin-up causes a giant pulse, whose emission is consistent with an FRB.

Observational Constraints

If two or more bursts are released during the rapid spin-up, the event duration is expected to be >1 ms for an unresolved burst and a double peaked profile is expected if the burst is partially resolved.