Difference between revisions of "Young Magnetars"

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|EnergyMechanism        = Maser
 
|EnergyMechanism        = Maser
 
|EmissionMechanism      = Synch.
 
|EmissionMechanism      = Synch.
|LFRadioCounterpart    = Yes <br/>(excl. self absorption)
+
|LFRadioCounterpart    = Yes, persistent
|HFRadioCounterpart    = Yes  
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|HFRadioCounterpart    = Yes, persistent
 
|MicrowaveCounterpart  = Maybe
 
|MicrowaveCounterpart  = Maybe
 
|THzCounterpart        = Maybe
 
|THzCounterpart        = Maybe
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== Observational Constraints ==
 
== Observational Constraints ==
  
FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse will be accompanied by persistent synchrotron radio emissionon timescales of months to years, powered by the nebula of relativistic electrons and magnetic fields inflated by the magnetar flares, or on longer timescales through interaction of the merger ejecta with the interstellar medium;  this timescale is shorter than for the SLSN/LGRB channel.  
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Persistent synchrotron radio emission with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs.  
  
  
The DM, RM and persistent radio emission in the model is consistent with
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==  ==
 +
 
 +
Using FRB 121102 to calibrate the model, the expected DM, RM and persistent radio emission is consistent with the upper limits of FRB 180924. FRBs from NS-NS magnetars distinct host galaxy and spatial offset distributions than the SLSNe/LGRB channel; we anticipate asimilar host population, although possibly different offset distribution for AIC events.

Revision as of 08:47, 6 September 2019





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/Collapse Magnetars Born in NS-NS Mergers and WD Collapse Repeat Maser Synch. Yes, persistent Yes, persistent Maybe Maybe No Afterglow Yes
if jet aligned
Yes Not detectable https://arxiv.org/pdf/1907.00016.pdf Same mechanisms as flares, but magnetars born in mergers or collapse as opposed in to SLSNe or LGRBs.

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


Model Description

This model considers FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse. The FRBs themselves are formed by the same mechanism as that of giant flare FRB theories.

Observational Constraints

Persistent synchrotron radio emission with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs.


Using FRB 121102 to calibrate the model, the expected DM, RM and persistent radio emission is consistent with the upper limits of FRB 180924. FRBs from NS-NS magnetars distinct host galaxy and spatial offset distributions than the SLSNe/LGRB channel; we anticipate asimilar host population, although possibly different offset distribution for AIC events.