Stellar Coronae - Revision history

Emma Platts at 08:42, 12 October 2018

2018-10-12T08:42:40Z

← Older revision		Revision as of 04:42, 12 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	One of the last surviving theories for FRBs of Galactic origins was flare stars. The theory was seemed fitting because dwarf stars have been observed to produce bursts of coherent radiation on short timescales <5 ms) and have been observed within FRB fields. A cyclotron maser in the lower part of the stellar corona could produce a flare consistent with FRB observations; the large DM and pulse smearing could be attributed to the corona plasma. Free-free absorption that occurs in the corona, however, presents a problem: a radio signal from the lower corona with the required DM may be unobservable unless the corona is infeasibly extended or hot. Further, the plasma density required for the DM is arguably too high to produce the frequency dependence on the pulse arrival times observed for FRBs. In defense of the theory, observations by are given that show high flare temperatures capable of mitigating significant free-free absorption. Further, if frequency drifts occur in flares (as observed in), the measured dispersion relationship for FRBs may be possible. Doubt is then cast on the theory again when it is shown that the brightness temperature of FRBs could not escape plasma as dense as the DM demands.		One of the last surviving theories for FRBs of Galactic origins was flare stars. The theory was seemed fitting because dwarf stars have been observed to produce bursts of coherent radiation on short timescales (<5 ms) and have been observed within FRB fields. A cyclotron maser in the lower part of the stellar corona could produce a flare consistent with FRB observations; the large DM and pulse smearing could be attributed to the corona plasma. Free-free absorption that occurs in the corona, however, presents a problem: a radio signal from the lower corona with the required DM may be unobservable unless the corona is infeasibly extended or hot. Further, the plasma density required for the DM is arguably too high to produce the frequency dependence on the pulse arrival times observed for FRBs. In defense of the theory, observations by are given that show high flare temperatures capable of mitigating significant free-free absorption. Further, if frequency drifts occur in flares (as observed in), the measured dispersion relationship for FRBs may be possible. Doubt is then cast on the theory again when it is shown that the brightness temperature of FRBs could not escape plasma as dense as the DM demands.

	== Observational Constraints ==		== Observational Constraints ==

	--		--

Emma Platts at 08:42, 12 October 2018

2018-10-12T08:42:20Z

← Older revision		Revision as of 04:42, 12 October 2018
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	<!-- This is an example. Change the right hand side of all these assignments -->		<!-- This is an example. Change the right hand side of all these assignments -->
	{{FRBTableTemplate		{{FRBTableTemplate
	\|Category = ~~Void~~		\|Category = Inviable
	\|Progenitor = Stellar Corona		\|Progenitor = Stellar Corona
	\|Type = Both		\|Type = Both
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	One of the last surviving theories for FRBs of Galactic origins was flare stars. The theory was seemed fitting because dwarf stars have been observed to produce bursts of coherent radiation on short timescales ($< 5$ ms) and have been observed within FRB fields. A cyclotron maser in the lower part of the stellar corona could produce a flare consistent with FRB observations; the large DM and pulse smearing could be attributed to the corona plasma. Free-free absorption that occurs in the corona, however, presents a problem: a radio signal from the lower corona with the required DM may be unobservable unless the corona is infeasibly extended or hot. Further, the plasma density required for the DM is arguably too high to produce the frequency dependence on the pulse arrival times observed for FRBs. In ~~defence~~ of the theory, observations by are given that show high flare temperatures capable of mitigating significant free-free absorption. Further, if frequency drifts occur in flares (as observed in), the measured dispersion relationship for FRBs may be possible. Doubt is then cast on the theory again when it is shown that the brightness temperature of FRBs could not escape plasma as dense as the DM demands.		One of the last surviving theories for FRBs of Galactic origins was flare stars. The theory was seemed fitting because dwarf stars have been observed to produce bursts of coherent radiation on short timescales <5 ms) and have been observed within FRB fields. A cyclotron maser in the lower part of the stellar corona could produce a flare consistent with FRB observations; the large DM and pulse smearing could be attributed to the corona plasma. Free-free absorption that occurs in the corona, however, presents a problem: a radio signal from the lower corona with the required DM may be unobservable unless the corona is infeasibly extended or hot. Further, the plasma density required for the DM is arguably too high to produce the frequency dependence on the pulse arrival times observed for FRBs. In defense of the theory, observations by are given that show high flare temperatures capable of mitigating significant free-free absorption. Further, if frequency drifts occur in flares (as observed in), the measured dispersion relationship for FRBs may be possible. Doubt is then cast on the theory again when it is shown that the brightness temperature of FRBs could not escape plasma as dense as the DM demands.

	== Observational Constraints ==		== Observational Constraints ==

	--		--

Jake Gordin: /* Observational Constraints */

2018-10-11T11:30:18Z

Observational Constraints

← Older revision		Revision as of 07:30, 11 October 2018
Line 28:		Line 28:
	== Observational Constraints ==		== Observational Constraints ==

	~~N/A~~		--

Sulona: /* Model Description */

2018-10-11T10:36:43Z

Model Description

← Older revision		Revision as of 06:36, 11 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	**To fill in with ~~updated draft~~		One of the last surviving theories for FRBs of Galactic origins was flare stars. The theory was seemed fitting because dwarf stars have been observed to produce bursts of coherent radiation on short timescales ($< 5$ ms) and have been observed within FRB fields. A cyclotron maser in the lower part of the stellar corona could produce a flare consistent with FRB observations; the large DM and pulse smearing could be attributed to the corona plasma. Free-free absorption that occurs in the corona, however, presents a problem: a radio signal from the lower corona with the required DM may be unobservable unless the corona is infeasibly extended or hot. Further, the plasma density required for the DM is arguably too high to produce the frequency dependence on the pulse arrival times observed for FRBs. In defence of the theory, observations by are given that show high flare temperatures capable of mitigating significant free-free absorption. Further, if frequency drifts occur in flares (as observed in), the measured dispersion relationship for FRBs may be possible. Doubt is then cast on the theory again when it is shown that the brightness temperature of FRBs could not escape plasma as dense as the DM demands.

	== Observational Constraints ==		== Observational Constraints ==

	N/A		N/A

Jake Gordin at 09:58, 11 October 2018

2018-10-11T09:58:30Z

← Older revision		Revision as of 05:58, 11 October 2018
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	\|GWCounterpart = N/A		\|GWCounterpart = N/A
	\|NeutrinoCounterpart = N/A		\|NeutrinoCounterpart = N/A
	\|References = ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1310.2419~~.pdf~~, http://adsabs.harvard.edu/abs/2015MNRAS.454.2183M		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1310.2419, http://adsabs.harvard.edu/abs/2015MNRAS.454.2183M
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts at 13:18, 2 October 2018

2018-10-02T13:18:03Z

← Older revision		Revision as of 09:18, 2 October 2018
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	\|Category = Void		\|Category = Void
	\|Progenitor = Stellar Corona		\|Progenitor = Stellar Corona
	\|Type = ~~N/A~~		\|Type = Both
	\|EnergyMechanism = N/A		\|EnergyMechanism = N/A
	\|EmissionMechanism = N/A		\|EmissionMechanism = N/A

Emma Platts at 12:09, 2 October 2018

2018-10-02T12:09:21Z

← Older revision		Revision as of 08:09, 2 October 2018
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	\|GWCounterpart = N/A		\|GWCounterpart = N/A
	\|NeutrinoCounterpart = N/A		\|NeutrinoCounterpart = N/A
	\|References = https://arxiv.org/pdf/~~1009~~.~~5392~~.pdf, http://adsabs.harvard.edu/abs/~~2014ApJ~~..~~.797...70K~~		\|References = https://arxiv.org/pdf/1310.2419.pdf, http://adsabs.harvard.edu/abs/2015MNRAS.454.2183M
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts: Created page with " {{FRBTableTemplate |Category = Void |Prog..."

2018-10-02T12:04:52Z

Created page with "   {{FRBTableTemplate |Category = Void |Prog..."

New page

{{FRBTableTemplate
|Category = Void
|Progenitor = Stellar Corona
|Type = N/A
|EnergyMechanism = N/A
|EmissionMechanism = N/A
|LFRadioCounterpart = N/A
|HFRadioCounterpart = N/A
|MicrowaveCounterpart = N/A
|THzCounterpart = N/A
|OIRCounterpart = N/A
|XrayCounterpart = N/A
|GammarayCounterpart = N/A
|GWCounterpart = N/A
|NeutrinoCounterpart = N/A
|References = https://arxiv.org/pdf/1009.5392.pdf, http://adsabs.harvard.edu/abs/2014ApJ...797...70K
|Comments = None
}}

== Model Description ==

**To fill in with updated draft

== Observational Constraints ==

N/A