https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&feed=atom&action=historyObservational evidence for breakout reconnection - Revision history2024-03-28T21:53:16ZRevision history for this page on the wikiMediaWiki 1.16.0https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=11808&oldid=prevHhudson at 10:58, 26 December 20192019-12-26T10:58:45Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Such a '''breakout reconnection''' scenario, first proposed in 1999 [2], has been studied in many numerical simulations of SEEs, but observational support for it has so far been weak. Nevertheless, this reconnection should be observable, due to associated acceleration of electrons which produce radio emission. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Such a '''breakout reconnection''' scenario, first proposed in 1999 [2], has been studied in many numerical simulations of SEEs, but observational support for it has so far been weak. Nevertheless, this reconnection should be observable, due to associated acceleration of electrons which produce radio emission. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE [3]<del class="diffchange diffchange-inline">. </del>SOL2003-11-03. Figure 1 shows the dynamic radio spectrum (from [http://www.aip.de/de?set_language=de AIP]) and the RHESSI 150-300 keV flux curve. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE [3]<ins class="diffchange diffchange-inline">, </ins>SOL2003-11-03. Figure 1 shows the dynamic radio spectrum (from [http://www.aip.de/de?set_language=de AIP]) and the RHESSI 150-300 keV flux curve. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. </div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=11807&oldid=prevHhudson: IAU target2019-12-26T10:58:23Z<p>IAU target</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Such a '''breakout reconnection''' scenario, first proposed in 1999 [2], has been studied in many numerical simulations of SEEs, but observational support for it has so far been weak. Nevertheless, this reconnection should be observable, due to associated acceleration of electrons which produce radio emission. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Such a '''breakout reconnection''' scenario, first proposed in 1999 [2], has been studied in many numerical simulations of SEEs, but observational support for it has so far been weak. Nevertheless, this reconnection should be observable, due to associated acceleration of electrons which produce radio emission. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE [3]. Figure 1 shows the dynamic radio spectrum (from [http://www.aip.de/de?set_language=de AIP]) and the RHESSI 150-300 keV flux curve. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE [3]<ins class="diffchange diffchange-inline">. SOL2003-11-03</ins>. Figure 1 shows the dynamic radio spectrum (from [http://www.aip.de/de?set_language=de AIP]) and the RHESSI 150-300 keV flux curve. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. </div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=10735&oldid=prevSchriste at 17:27, 22 August 20182018-08-22T17:27:43Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Gordon Holman</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Gordon Holman</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 2013 March 18</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 2013 March 18</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|next_nugget = [<del class="diffchange diffchange-inline">http</del>:<del class="diffchange diffchange-inline">//sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Antipodal_Flares Antipodal Flares</del>]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|next_nugget=<ins class="diffchange diffchange-inline">{{#ask: [</ins>[<ins class="diffchange diffchange-inline">Category</ins>:<ins class="diffchange diffchange-inline">Nugget</ins>]<ins class="diffchange diffchange-inline">] [[RHESSI Nugget Index::197]]}}</ins></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|previous_nugget =[<del class="diffchange diffchange-inline">http</del>:<del class="diffchange diffchange-inline">//sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Burst-on-Tail_(BOT) Burst-on-tail</del>]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|previous_nugget=<ins class="diffchange diffchange-inline">{{#ask: </ins>[<ins class="diffchange diffchange-inline">[Category</ins>:<ins class="diffchange diffchange-inline">Nugget]] [[RHESSI Nugget Index::195]</ins>]<ins class="diffchange diffchange-inline">}}</ins></div></td></tr>
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</table>Schristehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=6294&oldid=prevHhudson: updated infobox2013-08-01T07:22:14Z<p>updated infobox</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Gordon Holman</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Gordon Holman</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 2013 March 18</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 2013 March 18</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|next_nugget = Antipodal Flares</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|next_nugget = <ins class="diffchange diffchange-inline">[http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Antipodal_Flares </ins>Antipodal Flares<ins class="diffchange diffchange-inline">]</ins></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|previous_nugget =<del class="diffchange diffchange-inline">Observational evidence for breakout reconnection</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|previous_nugget =<ins class="diffchange diffchange-inline">[http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Burst-on-Tail_(BOT) Burst-on-tail]</ins></div></td></tr>
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</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=6061&oldid=prevHhudson at 14:35, 30 March 20132013-03-30T14:35:30Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Gordon Holman</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Gordon Holman</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 2013 March 18</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 2013 March 18</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|next_nugget = <del class="diffchange diffchange-inline">TBD</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|next_nugget = <ins class="diffchange diffchange-inline">Antipodal Flares</ins></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|previous_nugget =<del class="diffchange diffchange-inline">[[Burst-on-Tail (BOT)]]</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|previous_nugget =<ins class="diffchange diffchange-inline">Observational evidence for breakout reconnection</ins></div></td></tr>
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</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=5981&oldid=prevHhudson at 22:52, 17 March 20132013-03-17T22:52:37Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A plausible explanation for this arrangement is that the lower radio sources, like the upper X‑ray source, were associated with the upward-directed flare reconnection jet. It is important that the upper radio sources above the flaring active region remained stationary in space in the next minutes of the flare. They indicate the ongoing breakout reconnection process at that height level in the corona. The two 236.6 MHz sources would then naturally be associated with the roughly horizontal jets from the breakout reconnection well above the flaring active region.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A plausible explanation for this arrangement is that the lower radio sources, like the upper X‑ray source, were associated with the upward-directed flare reconnection jet. It is important that the upper radio sources above the flaring active region remained stationary in space in the next minutes of the flare. They indicate the ongoing breakout reconnection process at that height level in the corona. The two 236.6 MHz sources would then naturally be associated with the roughly horizontal jets from the breakout reconnection well above the flaring active region.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[[File:Fig3_neu.png|<del class="diffchange diffchange-inline">550px</del>|thumb|center|'''Figure 3''': Evidence for breakout reconnection in the 2003 November 3 SEE from radio (NRH) and X-ray (RHESSI) data. Contours show radio sources at 432 MHz (red), 327 MHz (cyan), and 236.6 MHz (dark green). The color insert shows the 15 – 20 keV X-ray sources [7].]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig3_neu.png|<ins class="diffchange diffchange-inline">350px</ins>|thumb|center|'''Figure 3''': Evidence for breakout reconnection in the 2003 November 3 SEE from radio (NRH) and X-ray (RHESSI) data. Contours show radio sources at 432 MHz (red), 327 MHz (cyan), and 236.6 MHz (dark green). The color insert shows the 15 – 20 keV X-ray sources [7].]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The configuration given by Figure 3 marks progress in our understanding of X-ray and radio data during the very onset of eruptive energy release in SEEs. The excellent timing between the occurrence of the radially elongated radio source formation and the "above the HXR loop-top source" [6] reveals that both sources belong to the same (upper flare reconnection) hot and turbulent plasma jet. The observations described here for a near-limb event are reminiscent of the results obtained for another SEE seen in projection on the disc, where a radio source at a distance of about 0.3 solar radii from the flaring active region was observed simultaneously with the most energetic X-ray and Gamma-ray emission [5].</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The configuration given by Figure 3 marks progress in our understanding of X-ray and radio data during the very onset of eruptive energy release in SEEs. The excellent timing between the occurrence of the radially elongated radio source formation and the "above the HXR loop-top source" [6] reveals that both sources belong to the same (upper flare reconnection) hot and turbulent plasma jet. The observations described here for a near-limb event are reminiscent of the results obtained for another SEE seen in projection on the disc, where a radio source at a distance of about 0.3 solar radii from the flaring active region was observed simultaneously with the most energetic X-ray and Gamma-ray emission [5].</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=5950&oldid=prevHhudson: more links2013-03-17T16:08:12Z<p>more links</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Such a '''breakout reconnection''' scenario, first proposed in 1999 [2], has been studied in many numerical simulations of SEEs, but observational support for it has so far been weak. Nevertheless, this reconnection should be observable, due to associated acceleration of electrons which produce radio emission. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Such a '''breakout reconnection''' scenario, first proposed in 1999 [2], has been studied in many numerical simulations of SEEs, but observational support for it has so far been weak. Nevertheless, this reconnection should be observable, due to associated acceleration of electrons which produce radio emission. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE [3]. Figure 1 shows the dynamic radio spectrum (AIP) and the RHESSI 150-300 keV flux curve. The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2. It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. Several radio sources appear, instead of a previous faint one, above the active region. We show the radio images at three frequencies (from the Nançay Multifrequency Radioheliograph, <del class="diffchange diffchange-inline">NRH, courtesy</del>: <del class="diffchange diffchange-inline">The Radioheliograph Group</del>), as well as the RHESSI hard X-ray image. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE [3]. Figure 1 shows the dynamic radio spectrum (<ins class="diffchange diffchange-inline">from [http://www.aip.de/de?set_language=de </ins>AIP<ins class="diffchange diffchange-inline">]</ins>) and the RHESSI 150-300 keV flux curve. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2.</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Several radio sources appear, instead of a previous faint one, above the active region. We show the radio images at three frequencies (from the Nançay Multifrequency Radioheliograph, <ins class="diffchange diffchange-inline">[http</ins>:<ins class="diffchange diffchange-inline">//secchirh.obspm.fr/nrh.php NRH]</ins>), as well as the RHESSI hard X-ray image. </div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[[Image:Fig1_neu3.png|350px|thumb|center|'''Figure 1''': The dynamic radio spectrum (AIP, top), and the RHESSI 150-300 keV light curve (bottom). The light-brown frame marks the time interval enlarged in Figure 2.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[Image:Fig1_neu3.png|350px|thumb|center|'''Figure 1''': The dynamic radio spectrum </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>(<ins class="diffchange diffchange-inline">[http://www.aip.de/de?set_language=de </ins>AIP<ins class="diffchange diffchange-inline">]</ins>, top), and the RHESSI 150-300 keV light curve (bottom). </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The light-brown frame marks the time interval enlarged in Figure 2.]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| valign="top"|</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| valign="top"|</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[[Image:Fig2.png|350px|thumb|right|'''Figure 2''': This feature (see the black arrow) is the first impulsive spectral signature of coronal radio emission in this flare, shown spatially resolved above the active region at heights of about 0.18 and 0.41 solar radii in Figure 3. The white lines mark two of the <del class="diffchange diffchange-inline">NRH </del>observing frequencies.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[Image:Fig2.png|350px|thumb|right|'''Figure 2''': This feature (see the black arrow) is the first impulsive spectral signature of coronal radio emission in this flare, shown spatially resolved above the active region at heights of about 0.18 and 0.41 solar radii in Figure 3. The white lines mark two of the </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[http://secchirh.obspm.fr/nrh.php Nançay] </ins>observing frequencies.]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|-</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|-</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|}</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|}</div></td></tr>
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<td colspan="2" class="diff-lineno">Line 42:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A plausible explanation for this arrangement is that the lower radio sources, like the upper X‑ray source, were associated with the upward-directed flare reconnection jet. It is important that the upper radio sources above the flaring active region remained stationary in space in the next minutes of the flare. They indicate the ongoing breakout reconnection process at that height level in the corona. The two 236.6 MHz sources would then naturally be associated with the roughly horizontal jets from the breakout reconnection well above the flaring active region.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A plausible explanation for this arrangement is that the lower radio sources, like the upper X‑ray source, were associated with the upward-directed flare reconnection jet. It is important that the upper radio sources above the flaring active region remained stationary in space in the next minutes of the flare. They indicate the ongoing breakout reconnection process at that height level in the corona. The two 236.6 MHz sources would then naturally be associated with the roughly horizontal jets from the breakout reconnection well above the flaring active region.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[[File:Fig3_neu.png|550px|thumb|center|'''Figure 3''': Evidence for breakout reconnection in the 2003 November 3 SEE from radio (NRH) and X-ray (RHESSI) data. Contours show radio sources at 432 MHz (red), 327 MHz (cyan), and 236.6 MHz (dark green). The color insert shows the 15 – 20 keV X-ray sources <del class="diffchange diffchange-inline">(from Veronig et al. 2006)</del>.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig3_neu.png|550px|thumb|center|'''Figure 3''': Evidence for breakout reconnection in the 2003 November 3 SEE <ins class="diffchange diffchange-inline"> </ins>from radio (NRH) and X-ray (RHESSI) data. Contours show radio sources at 432 MHz (red), 327 MHz (cyan), and 236.6 MHz (dark green). The color insert shows the 15 – 20 keV X-ray sources <ins class="diffchange diffchange-inline">[7]</ins>.]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>The configuration given by Figure 3 marks progress in our understanding of X-ray and radio data during the very onset of eruptive energy release in SEEs. The excellent timing between the occurrence of the radially elongated radio source formation and the "above the HXR loop-top source" <del class="diffchange diffchange-inline">(Sui et al. 2004) </del>reveals that both sources belong to the same (upper flare reconnection) hot and turbulent plasma jet. The observations described here for a near-limb event are reminiscent of the results obtained for another SEE seen in projection on the disc, where a radio source at a distance of about 0.3 solar radii from the flaring active region was observed simultaneously with the most energetic X-ray and Gamma-ray emission <del class="diffchange diffchange-inline">(see Aurass et al. 2011, 2006)</del>.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The configuration given by Figure 3 marks progress in our understanding of X-ray and radio data during the very onset of eruptive energy release in SEEs. The excellent timing between the occurrence of the radially elongated radio source formation and the "above the HXR loop-top source" <ins class="diffchange diffchange-inline"> [6] </ins>reveals that both sources belong to the same (upper flare reconnection) hot and turbulent plasma jet. The observations described here for a near-limb event are reminiscent of the results obtained for another SEE seen in projection on the disc, where a radio source at a distance of about 0.3 solar radii from the flaring active region was observed simultaneously with the most energetic X-ray and Gamma-ray emission <ins class="diffchange diffchange-inline">[5]</ins>.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== References ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== References ==</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=5947&oldid=prevHhudson: regularised the references and added some links2013-03-17T13:29:54Z<p>regularised the references and added some links</p>
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<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 13:29, 17 March 2013</td>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Authors: </del>Henry Aurass <del class="diffchange diffchange-inline">and </del>Gordon Holman</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">{{Infobox Nugget</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">|name = Nugget</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">|title = Observational Evidence for Breakout Reconnection</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">|number = 196</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">|first_author = </ins>Henry Aurass</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">|second_author = </ins>Gordon Holman</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">|publish_date = 2013 March 18</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">|next_nugget = TBD</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">|previous_nugget =[[Burst-on-Tail (BOT)]]</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">}}</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>In solar eruptive events (<del class="diffchange diffchange-inline">SEE's, Holman 2012</del>) the transition from slow to fast (eruptive) energy release leads to the interaction of a flux rope with the overlying magnetic field. If the flux rope has a field component opposite to that of the overlying field, magnetic reconnection between the flux<del class="diffchange diffchange-inline">-</del>rope and overlying <del class="diffchange diffchange-inline">fields </del>can occur. Such a '''breakout reconnection''' scenario, <del class="diffchange diffchange-inline">since Antiochos, DeVore & Klimchuk </del>proposed <del class="diffchange diffchange-inline">it </del>in 1999, has been <del class="diffchange diffchange-inline">included </del>in many numerical simulations of SEEs, but observational support for it has so far been weak. Nevertheless, this reconnection should be observable, due to associated acceleration of electrons which produce radio emission. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>In solar eruptive events (<ins class="diffchange diffchange-inline">SEEs; see Ref. [1]</ins>) the transition from slow to fast (eruptive) energy release leads to the interaction of a</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[http://www.nasa.gov/mission_pages/sdo/news/flux-ropes.html </ins>flux rope<ins class="diffchange diffchange-inline">] </ins>with the overlying magnetic field <ins class="diffchange diffchange-inline">of the large-scale corona.</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">Such a SEE combines the properties of a [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm solar flare] and a </ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[http://solarscience.msfc.nasa.gov/CMEs.shtml coronal mass ejection]</ins>. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>If the flux rope has a <ins class="diffchange diffchange-inline">magnetic-</ins>field component opposite to that of the overlying field, </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[http://en.wikipedia.org/wiki/Magnetic_reconnection </ins>magnetic reconnection<ins class="diffchange diffchange-inline">] </ins>between the flux rope and <ins class="diffchange diffchange-inline">this </ins>overlying <ins class="diffchange diffchange-inline">field </ins>can occur. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Such a '''breakout reconnection''' scenario, <ins class="diffchange diffchange-inline">first </ins>proposed in 1999 <ins class="diffchange diffchange-inline">[2]</ins>, has been <ins class="diffchange diffchange-inline">studied </ins>in many numerical simulations of SEEs, but observational support for it has so far been weak. Nevertheless, this reconnection should be observable, due to associated acceleration of electrons which produce radio emission. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE <del class="diffchange diffchange-inline">(Aurass, Holman et al. 2013)</del>. Figure 1 shows the dynamic radio spectrum (AIP) and the RHESSI 150-300 keV flux curve. The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2. It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. Several radio sources appear, instead of a previous faint one, above the active region. We show the radio images at three frequencies (from the Nançay Multifrequency Radioheliograph, NRH, courtesy: The Radioheliograph Group), as well as the RHESSI hard X-ray image. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Strong evidence for breakout reconnection has recently been identified in the combined meter-wave radio and RHESSI X-ray observations of a well-observed SEE <ins class="diffchange diffchange-inline">[3]</ins>. Figure 1 shows the dynamic radio spectrum (AIP) and the RHESSI 150-300 keV flux curve. The onset of strong particle acceleration is indicated by a light-brown box in Figure 1, and the radio spectrum is enlarged and contrast-enhanced in Figure 2. It depicts the dynamic spectrum of a seemingly minute feature (the black arrow points to it) shown spatially resolved in Figure 3. Several radio sources appear, instead of a previous faint one, above the active region. We show the radio images at three frequencies (from the Nançay Multifrequency Radioheliograph, NRH, courtesy: The Radioheliograph Group), as well as the RHESSI hard X-ray image. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>{| border="0" align="center"</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>{| border="0" align="center"</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|-</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|-</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| valign="top"|</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| valign="top"|</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[[Image:Fig1_neu3.png|<del class="diffchange diffchange-inline">500px</del>|thumb|center|'''Figure 1''': The dynamic radio spectrum (AIP, top), and the RHESSI 150-300 keV light curve (bottom). The light-brown frame marks the time interval enlarged in Figure 2.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[Image:Fig1_neu3.png|<ins class="diffchange diffchange-inline">350px</ins>|thumb|center|'''Figure 1''': The dynamic radio spectrum (AIP, top), and the RHESSI 150-300 keV light curve (bottom). The light-brown frame marks the time interval enlarged in Figure 2.]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| valign="top"|</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| valign="top"|</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[[Image:Fig2.png|<del class="diffchange diffchange-inline">500px</del>|thumb|right|'''Figure 2''': This feature (see the black arrow) is the first impulsive spectral signature of coronal radio emission in this flare, shown spatially resolved above the active region at heights of about 0.18 and 0.41 solar radii in Figure 3. The white lines mark two of the NRH observing frequencies.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[Image:Fig2.png|<ins class="diffchange diffchange-inline">350px</ins>|thumb|right|'''Figure 2''': This feature (see the black arrow) is the first impulsive spectral signature of coronal radio emission in this flare, shown spatially resolved above the active region at heights of about 0.18 and 0.41 solar radii in Figure 3. The white lines mark two of the NRH observing frequencies.]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|-</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|-</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|}</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|}</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The configuration given by Figure 3 marks progress in our understanding of X-ray and radio data during the very onset of eruptive energy release in SEEs. The excellent timing between the occurrence of the radially elongated radio source formation and the "above the HXR loop-top source" (Sui et al. 2004) reveals that both sources belong to the same (upper flare reconnection) hot and turbulent plasma jet. The observations described here for a near-limb event are reminiscent of the results obtained for another SEE seen in projection on the disc, where a radio source at a distance of about 0.3 solar radii from the flaring active region was observed simultaneously with the most energetic X-ray and Gamma-ray emission (see Aurass et al. 2011, 2006).</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The configuration given by Figure 3 marks progress in our understanding of X-ray and radio data during the very onset of eruptive energy release in SEEs. The excellent timing between the occurrence of the radially elongated radio source formation and the "above the HXR loop-top source" (Sui et al. 2004) reveals that both sources belong to the same (upper flare reconnection) hot and turbulent plasma jet. The observations described here for a near-limb event are reminiscent of the results obtained for another SEE seen in projection on the disc, where a radio source at a distance of about 0.3 solar radii from the flaring active region was observed simultaneously with the most energetic X-ray and Gamma-ray emission (see Aurass et al. 2011, 2006).</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>References<del class="diffchange diffchange-inline">: </del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">== </ins>References <ins class="diffchange diffchange-inline">==</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Antiochos, S</del>. <del class="diffchange diffchange-inline">K</del>.<del class="diffchange diffchange-inline">, DeVore, C</del>. <del class="diffchange diffchange-inline">R</del>.<del class="diffchange diffchange-inline">, Klimchuk, J</del>. <del class="diffchange diffchange-inline">A</del>.<del class="diffchange diffchange-inline">: 1999, ApJ 510, 485</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[1] [http://adsabs</ins>.<ins class="diffchange diffchange-inline">harvard</ins>.<ins class="diffchange diffchange-inline">edu/abs/2012PhT</ins>....<ins class="diffchange diffchange-inline">65d..56H Solar eruptive events]</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Aurass, H</del>.<del class="diffchange diffchange-inline">, G</del>. <del class="diffchange diffchange-inline">Holman, S</del>. <del class="diffchange diffchange-inline">Braune, G</del>. <del class="diffchange diffchange-inline">Mann, P</del>. <del class="diffchange diffchange-inline">Zlobec: 2013, A&</del>A <del class="diffchange diffchange-inline">submitted</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[2] [http://adsabs</ins>.<ins class="diffchange diffchange-inline">harvard</ins>.<ins class="diffchange diffchange-inline">edu/abs/1999ApJ</ins>...<ins class="diffchange diffchange-inline">510..485A </ins>A <ins class="diffchange diffchange-inline">model for solar Coronal Mass Ejections]</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Aurass, H., G. Mann, P. Zlobec, M. Karlicky: 2011, ApJ 730, 57A</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[3] [Radio evidence for breakout reconnection in a solar eruptive event]</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Aurass, H</del>.<del class="diffchange diffchange-inline">, G</del>. <del class="diffchange diffchange-inline">Mann, G</del>. <del class="diffchange diffchange-inline">Rausche, A</del>. <del class="diffchange diffchange-inline">Warmuth: 2006, A&A 457, 681</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[5] [http://adsabs</ins>.<ins class="diffchange diffchange-inline">harvard</ins>.<ins class="diffchange diffchange-inline">edu/abs/2011ApJ</ins>..<ins class="diffchange diffchange-inline">.730...57A Radio evidence of breakout reconnection?]</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Holman, G</del>.<del class="diffchange diffchange-inline">D</del>.<del class="diffchange diffchange-inline">: 2012, Physics Today 04</del>, <del class="diffchange diffchange-inline">56</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[4] [http://adsabs</ins>.<ins class="diffchange diffchange-inline">harvard</ins>.<ins class="diffchange diffchange-inline">edu/abs/2006A%26A...457..681A The GLE on Oct. 28</ins>, <ins class="diffchange diffchange-inline">2003 - radio diagnostics of relativistic electron and proton injection]</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Sui, L</del>.<del class="diffchange diffchange-inline">, Holman, G</del>.<del class="diffchange diffchange-inline">D</del>.<del class="diffchange diffchange-inline">, Dennis, B</del>.<del class="diffchange diffchange-inline">R</del>.<del class="diffchange diffchange-inline">: 2004, ApJ </del>612<del class="diffchange diffchange-inline">, 546</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[6] [http://adsabs</ins>.<ins class="diffchange diffchange-inline">harvard</ins>.<ins class="diffchange diffchange-inline">edu/abs/2004ApJ</ins>...612<ins class="diffchange diffchange-inline">..546S Evidence for magnetic reconnection in three homologous solar flares observed by RHESSI]</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Veronig, A</del>. <del class="diffchange diffchange-inline">M</del>.<del class="diffchange diffchange-inline">, Karlický, M</del>.<del class="diffchange diffchange-inline">, Vršnak, B</del>.<del class="diffchange diffchange-inline">, Temmer, M</del>.<del class="diffchange diffchange-inline">, Magdalenić, J</del>.<del class="diffchange diffchange-inline">, Dennis, B</del>. <del class="diffchange diffchange-inline">R</del>.<del class="diffchange diffchange-inline">, Otruba, W., Pötzi, W.: 2006, A&A 446, 675</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[7] [http://adsabs</ins>.<ins class="diffchange diffchange-inline">harvard</ins>.<ins class="diffchange diffchange-inline">edu/abs/2006A%26A</ins>...<ins class="diffchange diffchange-inline">446</ins>..<ins class="diffchange diffchange-inline">675V X-ray sources and magnetic reconnection in the X3</ins>.<ins class="diffchange diffchange-inline">9 flare of 2003 November 3]</ins></div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=5946&oldid=prevHaurass at 15:24, 14 March 20132013-03-14T15:24:24Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The two observed coronal X-ray sources serve to locate the two jets above and below the indicated flare reconnection site. In projection on the plane of sky, two radio sources are located radially above the active region (432 MHz, red in Figure 3, coinciding with NRH 410 MHz, not shown) and the X-ray sources. The lower one is a counterpart of the upper X-ray source. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The two observed coronal X-ray sources serve to locate the two jets above and below the indicated flare reconnection site. In projection on the plane of sky, two radio sources are located radially above the active region (432 MHz, red in Figure 3, coinciding with NRH 410 MHz, not shown) and the X-ray sources. The lower one is a counterpart of the upper X-ray source. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>The upper of these two sources indicates the '''breakout reconnection'''. Two other sources, shown at the lower frequency of 236.6 MHz (green in Figure 3), flank the upper radio sources. The upper radio source at the intermediate frequency of 327 MHz (cyan in Figure 3) is inclined toward North. <del class="diffchange diffchange-inline">Note </del>that 20 s later (with the main pulse of HXR emission; see Figure 1, bottom) the upper red (432 MHz) and the cyan (327 MHz) <del class="diffchange diffchange-inline">source sites </del>coincide <del class="diffchange diffchange-inline">in </del>the <del class="diffchange diffchange-inline">midth of its actual position </del>shown in Figure 3. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The upper of these two sources indicates the '''breakout reconnection'''. Two other sources, shown at the lower frequency of 236.6 MHz (green in Figure 3), flank the upper radio sources. The upper radio source at the intermediate frequency of 327 MHz (cyan in Figure 3) is inclined toward North. <ins class="diffchange diffchange-inline">The observations show </ins>that 20 s later (<ins class="diffchange diffchange-inline">in association </ins>with the main pulse of HXR emission; see Figure 1, bottom) the upper red (432 MHz) and the cyan (327 MHz) <ins class="diffchange diffchange-inline">sources </ins>coincide <ins class="diffchange diffchange-inline">at a location between </ins>the <ins class="diffchange diffchange-inline">positions </ins>shown in Figure 3. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A plausible explanation for this arrangement is that the lower radio sources, like the upper X‑ray source, were associated with the upward-directed flare reconnection jet. It is important that the upper radio sources above the flaring active region remained stationary in space in the next minutes of the flare. They indicate the ongoing breakout reconnection process at that height level in the corona. The two 236.6 MHz sources would then naturally be associated with the roughly horizontal jets from the breakout reconnection well above the flaring active region.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A plausible explanation for this arrangement is that the lower radio sources, like the upper X‑ray source, were associated with the upward-directed flare reconnection jet. It is important that the upper radio sources above the flaring active region remained stationary in space in the next minutes of the flare. They indicate the ongoing breakout reconnection process at that height level in the corona. The two 236.6 MHz sources would then naturally be associated with the roughly horizontal jets from the breakout reconnection well above the flaring active region.</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Antiochos, S. K., DeVore, C. R., Klimchuk, J. A.: 1999, ApJ 510, 485</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Antiochos, S. K., DeVore, C. R., Klimchuk, J. A.: 1999, ApJ 510, 485</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>H. <del class="diffchange diffchange-inline">Aurass</del>, G. Holman, S. Braune, G. Mann, P. Zlobec: 2013, A&A submitted</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">Aurass, </ins>H., G. Holman, S. Braune, G. Mann, P. Zlobec: 2013, A&A submitted</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>H. <del class="diffchange diffchange-inline">Aurass</del>, G. Mann, P. Zlobec, M. Karlicky: 2011, ApJ 730, 57A</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">Aurass, </ins>H., G. Mann, P. Zlobec, M. Karlicky: 2011, ApJ 730, 57A</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>H. <del class="diffchange diffchange-inline">Aurass</del>, G. Mann, G. Rausche, A. Warmuth: 2006, A&A 457, 681</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">Aurass, </ins>H., G. Mann, G. Rausche, A. Warmuth: 2006, A&A 457, 681</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Holman, G.D.: 2012, Physics Today 04, 56</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Holman, G.D.: 2012, Physics Today 04, 56</div></td></tr>
</table>Haurasshttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Observational_evidence_for_breakout_reconnection&diff=5945&oldid=prevHaurass at 09:44, 13 March 20132013-03-13T09:44:35Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|}</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|}</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>The two observed coronal X-ray sources serve to locate the two jets above and below the indicated flare reconnection site. <del class="diffchange diffchange-inline">Two </del>radio sources are located radially above the active region (432 MHz, red in Figure 3, <del class="diffchange diffchange-inline">and </del>coinciding with NRH 410 MHz, not shown <del class="diffchange diffchange-inline">here</del>) and the X-ray sources <del class="diffchange diffchange-inline">(in projection on the plane of sky)</del>. The lower one is a counterpart of the upper X-ray source. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The two observed coronal X-ray sources serve to locate the two jets above and below the indicated flare reconnection site. <ins class="diffchange diffchange-inline">In projection on the plane of sky, two </ins>radio sources are located radially above the active region (432 MHz, red in Figure 3, coinciding with NRH 410 MHz, not shown) and the X-ray sources. The lower one is a counterpart of the upper X-ray source. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>The upper of these two sources indicates the '''breakout reconnection'''. Two other sources, shown at the lower frequency of 236.6 MHz (green in Figure 3), flank the upper radio sources. The upper radio source at the intermediate frequency of 327 MHz (cyan in Figure 3) is inclined toward North. Note that 20 s later (with the main pulse of HXR emission) the upper red (432 MHz) and the cyan (327 MHz) source sites coincide in the midth of its actual position shown in Figure 3. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The upper of these two sources indicates the '''breakout reconnection'''. Two other sources, shown at the lower frequency of 236.6 MHz (green in Figure 3), flank the upper radio sources. The upper radio source at the intermediate frequency of 327 MHz (cyan in Figure 3) is inclined toward North. Note that 20 s later (with the main pulse of HXR emission<ins class="diffchange diffchange-inline">; see Figure 1, bottom</ins>) the upper red (432 MHz) and the cyan (327 MHz) source sites coincide in the midth of its actual position shown in Figure 3. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A plausible explanation for this arrangement is that the lower radio sources, like the upper X‑ray source, were associated with the upward-directed flare reconnection jet. It is important that the upper radio sources above the flaring active region remained stationary in space in the next minutes of the flare. They indicate the ongoing breakout reconnection process at that height level in the corona. The two 236.6 MHz sources would then naturally be associated with the roughly horizontal jets from the breakout reconnection well above the flaring active region.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A plausible explanation for this arrangement is that the lower radio sources, like the upper X‑ray source, were associated with the upward-directed flare reconnection jet. It is important that the upper radio sources above the flaring active region remained stationary in space in the next minutes of the flare. They indicate the ongoing breakout reconnection process at that height level in the corona. The two 236.6 MHz sources would then naturally be associated with the roughly horizontal jets from the breakout reconnection well above the flaring active region.</div></td></tr>
</table>Haurass