Decelerating Blast Waves - Revision history

Emma Platts at 11:48, 6 September 2019

2019-09-06T11:48:03Z

← Older revision		Revision as of 07:48, 6 September 2019
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	\|LFRadioCounterpart = Yes <br/>(excl. self absorption)		\|LFRadioCounterpart = Yes <br/>(excl. self absorption)
	\|HFRadioCounterpart = Yes		\|HFRadioCounterpart = Yes
	\|MicrowaveCounterpart = -		\|MicrowaveCounterpart = --
	\|THzCounterpart = -		\|THzCounterpart = --
	\|OIRCounterpart = Prompt		\|OIRCounterpart = Possible, Prompt
	\|XrayCounterpart = Prompt		\|XrayCounterpart = Prompt
	\|GammarayCounterpart = Prompt		\|GammarayCounterpart = Prompt
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	== Model Description ==		== Model Description ==

	In this model, FRBs are generated from forward shocks of blast waves decelerating into the previously decelerated waves. An example of these blast waves are flare ejecta from young magnetars. The ejected material also produces a persistent radio source and a source of high local dispersion measure and high rotation measure. The flares are expected to produce prompt gamma-ray, X-ray and possibly optical flares.		In this model, FRBs like that of FRB 121102 are generated from forward shocks of blast waves decelerating into the previously decelerated waves. An example of these blast waves are flare ejecta from young magnetars.

	== Observational Constraints ==		== Observational Constraints ==
	~~Observation of~~ a persistent radio source, ~~location in~~ a ~~dwarf galaxy, measurement~~ of high rotation measure ~~for~~ the ~~CHIME/~~FRB ~~repeater would be a good way~~ to ~~test~~ the model.		The ejected magnetar material produces a persistent radio source, and a source of high local dispersion measure and high rotation measure. The flares are expected to produce prompt gamma-ray, X-ray and possibly optical flares.

			== Consistency with Observations ==

			Arecibo telescope and the Robert C. Byrd GreenBank Telescope (GBT) have spent a total of ∼20 hrs observing the remnants of six GRBs (5 long and 1 short) with evidence of having a central magnetar similar to a magnetar that is assumed to powers FRB 121102 (Yunpeng Men et al. 2019). No FRBs were observed from these remnants. The probability of non-detection of FRBs akin to FRB 121102 is 8.9×10−6, which challenges the young magnetar model. The theory is not ruled out though: recent localizations of FRB 180924 (Bannister et al. 2019) and FRB 190523 (Ravi et al. 2019) suggest that the host galaxy of FRB is abnormal for repeating FRBs.

Shriharsh at 17:32, 15 February 2019

2019-02-15T17:32:56Z

← Older revision		Revision as of 13:32, 15 February 2019
Line 11:		Line 11:
	\|LFRadioCounterpart = Yes <br/>(excl. self absorption)		\|LFRadioCounterpart = Yes <br/>(excl. self absorption)
	\|HFRadioCounterpart = Yes		\|HFRadioCounterpart = Yes
	\|MicrowaveCounterpart = ~~Maybe~~		\|MicrowaveCounterpart = -
	\|THzCounterpart = ~~Maybe~~		\|THzCounterpart = -
	\|OIRCounterpart = Prompt		\|OIRCounterpart = Prompt
	\|XrayCounterpart = Prompt		\|XrayCounterpart = Prompt

Shriharsh: Created page with " {{FRBTableTemplate |Category = Shock Inte..."

2019-02-15T17:32:36Z

Created page with "   {{FRBTableTemplate |Category = Shock Inte..."

New page

{{FRBTableTemplate
|Category = Shock Interaction
|Progenitor = Magnetar
|Type = Repeat
|EnergyMechanism = Thin shell
|EmissionMechanism = Synch. Maser
|LFRadioCounterpart = Yes <br/>(excl. self absorption)
|HFRadioCounterpart = Yes
|MicrowaveCounterpart = Maybe
|THzCounterpart = Maybe
|OIRCounterpart = Prompt
|XrayCounterpart = Prompt
|GammarayCounterpart = Prompt
|GWCounterpart = No
|NeutrinoCounterpart = No
|References = http://adsabs.harvard.edu/abs/2019arXiv190201866M
|Comments = None
}}

== Model Description ==

In this model, FRBs are generated from forward shocks of blast waves decelerating into the previously decelerated waves. An example of these blast waves are flare ejecta from young magnetars. The ejected material also produces a persistent radio source and a source of high local dispersion measure and high rotation measure. The flares are expected to produce prompt gamma-ray, X-ray and possibly optical flares.

== Observational Constraints ==
Observation of a persistent radio source, location in a dwarf galaxy, measurement of high rotation measure for the CHIME/FRB repeater would be a good way to test the model.