NS-NS Merger (Mag. Flux Change): Difference between revisions
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Emma Platts (talk | contribs) (Created page with " <!-- Brings in the summary table --> <!-- This is an example. Change the right hand side of all these assignments --> {{FRBTableTemplate |Category = Merger |Pr...") |
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|Type = Both | |Type = Both | ||
|EnergyMechanism = Mag. flux change | |EnergyMechanism = Mag. flux change | ||
|EmissionMechanism = | |EmissionMechanism = -- | ||
|LFRadioCounterpart = Yes | |LFRadioCounterpart = Yes | ||
|HFRadioCounterpart = Yes | |HFRadioCounterpart = Yes | ||
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== Model Description == | == Model Description == | ||
A close encounter between two NSs results in the formation of highly elongated orbits, continuously shrinking due to dissipation through gravitational waves. As the orbital separation decreases, the changing magnetic flux bunches particles, which then radiate coherently. The NSs will approach each other several times, during which their respective magnetospheres will interact, leading to several FRBs before the final merger. | |||
== Observational Constraints == | == Observational Constraints == | ||
The expectation is that FRBs would be localized to centers of galaxies, or at least would be clustered with stellar density. | The expectation is that FRBs would be localized to centers of galaxies, or at least would be clustered with stellar density. | ||
Latest revision as of 04:55, 9 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 | |||||||
| Merger | NS-NS | Both | Mag. flux change | -- | Yes | Yes | -- | -- | Kilonova | Afterglow | sGRB if jet aligned |
Yes | -- | http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1701.02492 | In dense stellar clusters |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
A close encounter between two NSs results in the formation of highly elongated orbits, continuously shrinking due to dissipation through gravitational waves. As the orbital separation decreases, the changing magnetic flux bunches particles, which then radiate coherently. The NSs will approach each other several times, during which their respective magnetospheres will interact, leading to several FRBs before the final merger.
Observational Constraints
The expectation is that FRBs would be localized to centers of galaxies, or at least would be clustered with stellar density.