Giant Pulses: Difference between revisions
Emma Platts (talk | contribs) No edit summary |
Emma Platts (talk | contribs) No edit summary |
||
| (2 intermediate revisions by the same user not shown) | |||
| Line 7: | Line 7: | ||
|Progenitor = Giant Pulses | |Progenitor = Giant Pulses | ||
|Type = Repeat | |Type = Repeat | ||
|EnergyMechanism = | |EnergyMechanism = -- | ||
|EmissionMechanism = Synch. <br/> / Curv. | |EmissionMechanism = Synch. <br/> / Curv. | ||
|LFRadioCounterpart = Yes | |LFRadioCounterpart = Yes | ||
| Line 19: | Line 19: | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = http://adsabs.harvard.edu/abs/2012MNRAS.425L..71K, http://adsabs.harvard.edu/abs/2016MNRAS.457..232C, https://arxiv.org/pdf/1505.05535.pdf | |References = http://adsabs.harvard.edu/abs/2012MNRAS.425L..71K, http://adsabs.harvard.edu/abs/2016MNRAS.457..232C, https://arxiv.org/pdf/1505.05535.pdf | ||
|Comments = | |Comments = Rapid flux decay expected to be observed within a few years. | ||
}} | }} | ||
Latest revision as of 05:40, 15 October 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 | |||||||
| SNR (Pulsars) | Giant Pulses | Repeat | -- | Synch. / Curv. |
Yes | -- | -- | -- | -- | -- | -- | -- | -- | http://adsabs.harvard.edu/abs/2012MNRAS.425L..71K, http://adsabs.harvard.edu/abs/2016MNRAS.457..232C, https://arxiv.org/pdf/1505.05535.pdf | Rapid flux decay expected to be observed within a few years. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
Analogous to models for the Crab pulsar, FRBs of extragalactic origins may be giant pulses of a young pulsar. A specific giant pulse mechanism has been proposed for FRBs, in which a nearly charge-neutral clump of particles (produced by a two-streaming instability or a bunching instability) is accelerated through the pulsar magnetosphere by some reconnection event. The resultant coherent curvature radiation will be emitted for the duration that the clump remains intact. Note, however, that the emission mechanism of giant pulses remains an open question, and that this represents one possibility for FRB formation.
Observational Constraints
FRBs are predicted to be repeating and stochastic. A SN explosion a few years prior to the FRB may be observable. The DM, RM and polarization of FRBs in this scenario are owed to the nebula surrounding the pulsar as opposed to the intergalactic medium. This places FRBs at extragalactic (as opposed to cosmological) distances, and thus relaxes the energy requirements. The spin-down luminosity decreases within a timescale of a few years. The giant pulse model therefore depends on the observation of rapid flux decay in FRBs within a few years.