https://frbtheorycat.org/index.php?title=NS-WD_Merger&feed=atom&action=history
NS-WD Merger - Revision history
2024-03-28T12:32:43Z
Revision history for this page on the wiki
MediaWiki 1.39.6
https://frbtheorycat.org/index.php?title=NS-WD_Merger&diff=258&oldid=prev
Jake Gordin at 09:53, 11 October 2018
2018-10-11T09:53:10Z
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 05:53, 11 October 2018</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|NeutrinoCounterpart = --</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|NeutrinoCounterpart = --</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|References = <del style="font-weight: bold; text-decoration: none;">https</del>://<del style="font-weight: bold; text-decoration: none;">arxiv</del>.<del style="font-weight: bold; text-decoration: none;">org</del>/<del style="font-weight: bold; text-decoration: none;">abs</del>/1712.03509</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|References = <ins style="font-weight: bold; text-decoration: none;">http</ins>://<ins style="font-weight: bold; text-decoration: none;">adsabs</ins>.<ins style="font-weight: bold; text-decoration: none;">harvard.edu</ins>/<ins style="font-weight: bold; text-decoration: none;">cgi-bin</ins>/<ins style="font-weight: bold; text-decoration: none;">bib_query?arXiv:</ins>1712.03509</div></td></tr>
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Jake Gordin
https://frbtheorycat.org/index.php?title=NS-WD_Merger&diff=232&oldid=prev
Apw at 12:47, 10 October 2018
2018-10-10T12:47:28Z
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 08:47, 10 October 2018</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Model Description ==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Model Description ==</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Upon NS-WD coalescence, magnetic reconnection injects relativistic electrons from the surface of the WD into the magnetosphere of the NS to create an FRB.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Upon NS-WD coalescence, magnetic reconnection injects relativistic electrons from the surface of the WD into the magnetosphere of the NS to create an FRB<ins style="font-weight: bold; text-decoration: none;">. The timescale of the burst is assumed to be from the time of electron injection to the formation of the final merged object. It is predicted that the shorter the intrinsic width of the FRB, the higher the flux density</ins>.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Observational Constraints ==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Observational Constraints ==</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><del style="font-weight: bold; text-decoration: none;">The timescale of the burst is assumed to be from the time of electron injection to the formation of the final merged object. It is predicted that the shorter the intrinsic width of the FRB, the higher the flux density. </del>Of the 28 FRBs analysed (those available at the time), the pulse widths were broader than expected in the NS-WD scenario, but perhaps pulse widths vary more widely between FRBs due to multipath scattering through the IGM.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Of the 28 FRBs analysed (those available at the time), the pulse widths were broader than expected in the NS-WD scenario, but perhaps pulse widths vary more widely between FRBs due to multipath scattering through the IGM.</div></td></tr>
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Apw
https://frbtheorycat.org/index.php?title=NS-WD_Merger&diff=231&oldid=prev
Apw at 12:46, 10 October 2018
2018-10-10T12:46:46Z
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<table style="background-color: #fff; color: #202122;" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 08:46, 10 October 2018</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Model Description ==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Model Description ==</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Upon NS-WD coalescence, magnetic reconnection injects relativistic electrons from the surface of the WD into the magnetosphere of the NS to create an FRB<del style="font-weight: bold; text-decoration: none;">. The timescale of the burst is assumed to be from the time of electron injection to the formation of the final merged object. It is predicted that the shorter the intrinsic width of the FRB, the higher the flux density. Of the 28 FRBs analysed (those available at the time), the pulse widths were broader than expected in the NS-WD scenario, but perhaps pulse widths vary more widely between FRBs due to multipath scattering through the IGM</del>.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Upon NS-WD coalescence, magnetic reconnection injects relativistic electrons from the surface of the WD into the magnetosphere of the NS to create an FRB.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Observational Constraints ==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Observational Constraints ==</div></td></tr>
<tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">The timescale of the burst is assumed to be from the time of electron injection to the formation of the final merged object. It is predicted that the shorter the intrinsic width of the FRB, the higher the flux density. Of the 28 FRBs analysed (those available at the time), the pulse widths were broader than expected in the NS-WD scenario, but perhaps pulse widths vary more widely between FRBs due to multipath scattering through the IGM.</ins></div></td></tr>
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Apw
https://frbtheorycat.org/index.php?title=NS-WD_Merger&diff=90&oldid=prev
Emma Platts: 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..."
2018-09-26T14:08:11Z
<p>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..."</p>
<p><b>New page</b></p><div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = NS-WD<br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = Yes <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/abs/1712.03509<br />
|Comments = <br />
}}<br />
<br />
== Model Description ==<br />
Upon NS-WD coalescence, magnetic reconnection injects relativistic electrons from the surface of the WD into the magnetosphere of the NS to create an FRB. The timescale of the burst is assumed to be from the time of electron injection to the formation of the final merged object. It is predicted that the shorter the intrinsic width of the FRB, the higher the flux density. Of the 28 FRBs analysed (those available at the time), the pulse widths were broader than expected in the NS-WD scenario, but perhaps pulse widths vary more widely between FRBs due to multipath scattering through the IGM.<br />
<br />
== Observational Constraints ==</div>
Emma Platts