Pulsar-BH Interaction: Difference between revisions
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Revision as of 09:28, 26 September 2018
| 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.