https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&feed=atom&action=historyElectron acceleration and hard X-ray emission from SOL2013-11-09 - Revision history2024-03-28T19:19:25ZRevision history for this page on the wikiMediaWiki 1.16.0https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=11170&oldid=prevSchriste at 14:52, 21 September 20182018-09-21T14:52:07Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Galina Motorina</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Galina Motorina</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 5 May 2016 </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 5 May 2016 </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">Data-driven radiative hydrodynamics </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: [[Category:Nugget]] [[RHESSI Nugget Index::274]]}}</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/Extreme_events,_stellar_evolution,_and_magnetic_reconnection Extreme events</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::272]</ins>]<ins class="diffchange diffchange-inline">}}</ins></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: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">=</del>== Introduction <del class="diffchange diffchange-inline">=</del>==</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>== Introduction ==</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The acceleration of high-energy particles has long been recognized as </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The acceleration of high-energy particles has long been recognized as </div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This Nugget is devoted to the analysis of the hard X-ray emission</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This Nugget is devoted to the analysis of the hard X-ray emission</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>from different parts of a flare loop based on RHESSI observations</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>from different parts of a flare loop based on RHESSI observations</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>for the well-studied <del class="diffchange diffchange-inline"> </del>solar flare </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>for the well-studied solar flare <ins class="diffchange diffchange-inline">of [[Has event date::2013-Nov-09 06:26:09]], </ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[http://sprg.ssl.berkeley.edu/~tohban/browser/?show=grth1+grth3+qlpcr+qli02+qli04+fergo+rms4a&date=20131109&time=062609&bar=1 SOL2013-11-09 (C1.2)] [1,2].</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[http://sprg.ssl.berkeley.edu/~tohban/browser/?show=grth1+grth3+qlpcr+qli02+qli04+fergo+rms4a&date=20131109&time=062609&bar=1 SOL2013-11-09 (C1.2)] [1,2].</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">=</del>== Relationships between hard X-ray emissions from different parts of a flare loop <del class="diffchange diffchange-inline">=</del>==</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>== Relationships between hard X-ray emissions from different parts of a flare loop ==</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The hard X-ray images (Figure 1) of the solar flare SOL2013-11-09 (C2.6)</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The hard X-ray images (Figure 1) of the solar flare SOL2013-11-09 (C2.6)</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>represented as [3]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>represented as [3]</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[[File:273f2.png|500px|thumb|center</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:273f2.png|500px|thumb|center]]</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; 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>where B(a, b, c) is an incomplete</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>where B(a, b, c) is an incomplete</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>solar flare model requires at least some modifications.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>solar flare model requires at least some modifications.</div></td></tr>
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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">=</del>== Conclusions <del class="diffchange diffchange-inline">=</del>==</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>== Conclusions ==</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The discrepancy between the model estimates and hard X-ray</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The discrepancy between the model estimates and hard X-ray</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>in this case.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>in this case.</div></td></tr>
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<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins style="color: red; font-weight: bold; text-decoration: none;">== References ==</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">[1] </del>[http://adsabs.harvard.edu/abs/2015A%26A...577A..68S "Direct observation of the energy release site in a solar flare by SDO/AIA, Hinode/EIS, and RHESSI"]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>[http://adsabs.harvard.edu/abs/2015A%26A...577A..68S "Direct observation of the energy release site in a solar flare by SDO/AIA, Hinode/EIS, and RHESSI"]</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div> </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>[http://adsabs.harvard.edu/abs/2015SoPh..290.3573S "Impulsive heating of solar flare ribbons above 10 MK"]</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">[2] </del>[http://adsabs.harvard.edu/abs/2015SoPh..290.3573S "Impulsive heating of solar flare ribbons above 10 MK"]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>[http://adsabs.harvard.edu/abs/2004ApJ...603L.117V "A coronal thick-target interpretation of two hard X-ray loop events"]</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div> </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>[http://adsabs.harvard.edu/abs/2009A%26A...508..993B "Local re-acceleration and a modified thick target model of solar flare electrons"]</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">[3] </del>[http://adsabs.harvard.edu/abs/2004ApJ...603L.117V "A coronal thick-target interpretation of two hard X-ray loop events"]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>[http://adsabs.harvard.edu/abs/2015SoPh..290.3559Z "Particle acceleration and plasma heating in the chromosphere<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> </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># [http://adsabs.harvard.edu/abs/1998ARep...42..275T "The stochastic acceleration of upper chromospheric electrons</ins>"]</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">[4] </del>[http://adsabs.harvard.edu/abs/2009A%26A...508..993B "Local re-acceleration and a modified thick target model of solar flare electrons"]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div> </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">[5] </del>[http://adsabs.harvard.edu/abs/2015SoPh..290.3559Z "Particle acceleration and plasma heating in the chromosphere"]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; 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>[<del class="diffchange diffchange-inline">6</del>] [<del class="diffchange diffchange-inline">http</del>:<del class="diffchange diffchange-inline">//adsabs.harvard.edu/abs/1998ARep...42..275T "The stochastic acceleration of upper chromospheric electrons"</del>]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[<ins class="diffchange diffchange-inline">[Has observation by:: RHESSI| </ins>]<ins class="diffchange diffchange-inline">]</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">[Has observation by</ins>:<ins class="diffchange diffchange-inline">: SDO AIA| ]</ins>]</div></td></tr>
</table>Schristehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=8953&oldid=prevHhudson: /* Relationships between hard X-ray emissions from different */2016-05-08T06:04:50Z<p><span class="autocomment">Relationships between hard X-ray emissions from different</span></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[http://sprg.ssl.berkeley.edu/~tohban/browser/?show=grth1+grth3+qlpcr+qli02+qli04+fergo+rms4a&date=20131109&time=062609&bar=1 SOL2013-11-09 (C1.2)] [1,2].</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[http://sprg.ssl.berkeley.edu/~tohban/browser/?show=grth1+grth3+qlpcr+qli02+qli04+fergo+rms4a&date=20131109&time=062609&bar=1 SOL2013-11-09 (C1.2)] [1,2].</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>=== Relationships between hard X-ray emissions from different ===</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>=== Relationships between hard X-ray emissions from different <ins class="diffchange diffchange-inline">parts of a flare loop </ins>===</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The hard X-ray images (Figure 1) of the solar flare SOL2013-11-09 (C2.6)</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The hard X-ray images (Figure 1) of the solar flare SOL2013-11-09 (C2.6)</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=8949&oldid=prevHhudson at 05:56, 7 May 20162016-05-07T05:56:43Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Galina Motorina</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Galina Motorina</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 5 May 2016 </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 5 May 2016 </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">Non</del>-<del class="diffchange diffchange-inline">thermal recombination radiation </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">Data</ins>-<ins class="diffchange diffchange-inline">driven radiative hydrodynamics </ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Extreme_events,_stellar_evolution,_and_magnetic_reconnection Extreme events]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Extreme_events,_stellar_evolution,_and_magnetic_reconnection Extreme events]</div></td></tr>
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</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=8948&oldid=prevHhudson at 21:48, 6 May 20162016-05-06T21:48:44Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>SDO/AIA 171 &#8491; image (in inverted colors)</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>SDO/AIA 171 &#8491; image (in inverted colors)</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>overlaid with RHESSI images at 4.1-4.9~keV (white) near the peak</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>overlaid with RHESSI images at 4.1-4.9~keV (white) near the peak</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>of the impulsive phase, with contours at 50, 70 and 90% of the</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>of the impulsive phase, with contours at 50<ins class="diffchange diffchange-inline">, 60</ins>, 70 and 90% of the</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>maximum of each image, and at 23.0-27.5 keV (blue, levels 50,</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>maximum of each image, and at 23.0-27.5 keV (blue, levels 50,</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>60, 70, <del class="diffchange diffchange-inline">80, </del>90 of the image maximum) integrated for ~300 s, </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>60, 70, <ins class="diffchange diffchange-inline">and </ins>90<ins class="diffchange diffchange-inline">% </ins>of the image maximum) integrated for ~300 s, </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>covering the entire main impulsive phase (time intervals</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>covering the entire main impulsive phase (time intervals</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>indicated in the figure legend).</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>indicated in the figure legend).</div></td></tr>
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<td colspan="2" class="diff-lineno">Line 61:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>propagating from the looptop to the footpoints. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>propagating from the looptop to the footpoints. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>In particular, supposing the</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>In particular, supposing the</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>coronal loop column density </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>coronal loop column density <ins class="diffchange diffchange-inline">N = nL/2 = </ins>1-2 x 10<sup>20</sup> cm<sup>-2</sup>, and that</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>1-2 x 10<sup>20</sup> cm<sup>-2</sup>, and that</div></td><td class='diff-marker'>+</td><td style="background: #cfc; 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>the cosine between the direction of the</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the cosine between the direction of the</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>magnetic field and the electron velocity &mu; = 0.5, we find that</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>magnetic field and the electron velocity &mu; = 0.5, we find that</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=8926&oldid=prevHhudson at 12:24, 4 May 20162016-05-04T12:24:31Z<p></p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
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<col class='diff-marker' />
<col class='diff-content' />
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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 12:24, 4 May 2016</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 67:</td>
<td colspan="2" class="diff-lineno">Line 67:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>accelerated electrons will be collisionaly stopped in the coronal</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>accelerated electrons will be collisionaly stopped in the coronal</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>part of a flare loop if their energy E < E<sub>loop</sub> ~ 10 (N<sub>19</sub>/&mu;)<sup>1/2</sup> = 45-63 keV,</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>part of a flare loop if their energy E < E<sub>loop</sub> ~ 10 (N<sub>19</sub>/&mu;)<sup>1/2</sup> = 45-63 keV,</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>where N<sub>19</sub> = 10<sup>19</sup><del class="diffchange diffchange-inline">N</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>where N<sub>19</sub> = <ins class="diffchange diffchange-inline">N/</ins>10<sup>19</sup></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>The relationship between the spectral fluxes of hard X-ray</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The relationship between the spectral fluxes of hard X-ray</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>emission at the coronal part I<sub>lp</sub> and the footpoints I<sub>fp</sub></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>emission at the coronal part I<sub>lp</sub> and the footpoints I<sub>fp</sub><ins class="diffchange diffchange-inline">,</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>as predicted by the</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>as predicted by the</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[http://solarphysics.livingreviews.org/open?pubNo=lrsp-2008-1&amp;page=articlesu7.html collisional thick target] model can be</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[http://solarphysics.livingreviews.org/open?pubNo=lrsp-2008-1&amp;page=articlesu7.html collisional thick target] model<ins class="diffchange diffchange-inline">, </ins>can be</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>represented as [3]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>represented as [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 colspan="2" class="diff-lineno">Line 81:</td>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[https://en.wikipedia.org/wiki/Beta_function beta function] and &delta; is the </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[https://en.wikipedia.org/wiki/Beta_function beta function] and &delta; is the </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>spectral index of the electron flux. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>spectral index of the electron flux. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Then, adopting delta = 5.6 and E<sub>loop</sub> = 0.5, we</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Then, adopting delta = 5.6 and <ins class="diffchange diffchange-inline">&epsilon;/</ins>E<sub>loop</sub> = 0.5, we</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>find I<sub>lp</sub>/ I<sub>fp</sub> ~ 11.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>find I<sub>lp</sub>/ I<sub>fp</sub> ~ 11.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The estimate thus obtained contradicts the</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The estimate thus obtained contradicts the</div></td></tr>
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<td colspan="2" class="diff-lineno">Line 93:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>observations suggests that electron acceleration can occur not</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>observations suggests that electron acceleration can occur not</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>only in the coronal part of a loop but also in the footpoints.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>only in the coronal part of a loop but also in the footpoints.</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>This inference <del class="diffchange diffchange-inline">well </del>agrees well with the idea of re-acceleration [4]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This inference agrees well with the idea of re-acceleration [4]</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">as well as </del>the solar flare model proposed by Zaitsev and</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">and in addition with </ins>the solar flare model proposed by Zaitsev and</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Stepanov [5]; see also [6]. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Stepanov [5]; see also [6]. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Note that an extended acceleration region in the corona does not</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Note that an extended acceleration region in the corona does not</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=8924&oldid=prevHhudson at 10:04, 4 May 20162016-05-04T10:04:38Z<p></p>
<table style="background-color: white; color:black;">
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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>where B(a, b, c) is an incomplete beta function and delta is the </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>where B(a, b, c) is an incomplete</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>spectral index of the <del class="diffchange diffchange-inline">electrons</del>. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[https://en.wikipedia.org/wiki/Beta_function </ins>beta function<ins class="diffchange diffchange-inline">] </ins>and <ins class="diffchange diffchange-inline">&</ins>delta<ins class="diffchange diffchange-inline">; </ins>is the </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>spectral index of the <ins class="diffchange diffchange-inline">electron flux</ins>. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Then, adopting delta = 5.6 and E<sub>loop</sub> = 0.5, we</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Then, adopting delta = 5.6 and E<sub>loop</sub> = 0.5, we</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>find I<sub>lp</sub>/ I<sub>fp</sub> ~ 11.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>find I<sub>lp</sub>/ I<sub>fp</sub> ~ 11.</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=8923&oldid=prevHhudson: tiny fixes and a large link2016-05-04T10:02:57Z<p>tiny fixes and a large link</p>
<table style="background-color: white; color:black;">
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<td colspan='2' style="background-color: white; color:black;">Revision as of 10:02, 4 May 2016</td>
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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>The relationship between the spectral fluxes of hard X-ray</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The relationship between the spectral fluxes of hard X-ray</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>emission at the coronal part <del class="diffchange diffchange-inline">$I_{</del>lp<del class="diffchange diffchange-inline">}$ </del> and the footpoints <del class="diffchange diffchange-inline">$I_{</del>fp<del class="diffchange diffchange-inline">}$</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>emission at the coronal part <ins class="diffchange diffchange-inline">I<sub></ins>lp<ins class="diffchange diffchange-inline"></sub> </ins> and the footpoints <ins class="diffchange diffchange-inline">I<sub></ins>fp<ins class="diffchange diffchange-inline"></sub></ins></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>as <del class="diffchange diffchange-inline">it follows from </del>the collisional thick target model can be</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>as <ins class="diffchange diffchange-inline">predicted by </ins>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://solarphysics.livingreviews.org/open?pubNo=lrsp-2008-1&amp;page=articlesu7.html </ins>collisional thick target<ins class="diffchange diffchange-inline">] </ins>model can be</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>represented as [3]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>represented as [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>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=8921&oldid=prevHhudson: added links2016-05-03T19:30:36Z<p>added links</p>
<table style="background-color: white; color:black;">
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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 19:30, 3 May 2016</td>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Until now it has not been clear exactly where the electron acceleration region</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Until now it has not been clear exactly where the electron acceleration region</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>is located during the flare energy release. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>is located during the flare energy release. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>It is usually considered that electrons are accelerated in the corona. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>It is usually considered that electrons are accelerated in the </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>In particular, they can be accelerated in the region of the <del class="diffchange diffchange-inline">looptop</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[https://en.wikipedia.org/wiki/Corona solar </ins>corona<ins class="diffchange diffchange-inline">]</ins>. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>In particular, they can be accelerated in the region of the <ins class="diffchange diffchange-inline">top</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">of a [https://en.wikipedia.org/wiki/Coronal_loop magnetic loop] structure</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>(models with a compact acceleration region) or in the whole loop</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>(models with a compact acceleration region) or in the whole loop</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>(models with an extended acceleration region). </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>(models with an extended acceleration region). </div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 27:</td>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This Nugget is devoted to the analysis of the hard X-ray emission</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This Nugget is devoted to the analysis of the hard X-ray emission</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>from different parts of a flare loop based on RHESSI observations</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>from different parts of a flare loop based on RHESSI observations</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>for the well-studied solar flare <del class="diffchange diffchange-inline">onSOL2013</del>-11-09 (C1.2) [1,2].</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>for the well-studied solar flare </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://sprg.ssl.berkeley.edu/~tohban/browser/?show=grth1+grth3+qlpcr+qli02+qli04+fergo+rms4a&date=20131109&time=062609&bar=1 SOL2013</ins>-11-09 (C1.2)<ins class="diffchange diffchange-inline">] </ins>[1,2].</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>=== Relationships between hard X-ray emissions from different ===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>=== Relationships between hard X-ray emissions from different ===</div></td></tr>
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<td colspan="2" class="diff-lineno">Line 51:</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 RHESSI imaging appears to resolve this looptop source as a</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The RHESSI imaging appears to resolve this looptop source as a</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>dense [1], [2] <del class="diffchange diffchange-inline">(</del>n<sub>e</sub> ~ 3 x 10<sup>11</sup> cm<sup>-3</sup></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>dense <ins class="diffchange diffchange-inline">structure </ins>[1], [2]<ins class="diffchange diffchange-inline">, with estimates of </ins>n<sub>e</sub> ~ 3 x 10<sup>11</sup> cm<sup>-3</sup></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>and a characteristic size L ~ 9-18 arcsec.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>and a characteristic size L ~ 9-18 arcsec.</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>These <del class="diffchange diffchange-inline">estiates </del>apply at the maximum of the hard X-ray emission (06:25:41~UT) </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>These <ins class="diffchange diffchange-inline">estimates </ins>apply at the <ins class="diffchange diffchange-inline">time of </ins>maximum of the hard X-ray emission (06:25:41~UT) </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>in terms of the simultaneous </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>in terms of the simultaneous </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[http://global.jaxa.jp/projects/sat/solar_b/ Hinode]/[http://solarb.mssl.ucl.ac.uk/SolarB/Solar-B.jsp EIS]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[http://global.jaxa.jp/projects/sat/solar_b/ Hinode]/[http://solarb.mssl.ucl.ac.uk/SolarB/Solar-B.jsp EIS]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>observations [1].</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>observations [1].</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The high plasma density suggests that accelerated</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The high plasma density suggests that accelerated</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>electrons <del class="diffchange diffchange-inline">should </del>lose the kinetic energy quite <del class="diffchange diffchange-inline">fast </del>while</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>electrons <ins class="diffchange diffchange-inline">must </ins>lose the kinetic energy quite <ins class="diffchange diffchange-inline">rapidly </ins>while</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>propagating from the looptop to the footpoints. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>propagating from the looptop to the footpoints. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>In particular, supposing the</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>In particular, supposing the</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 63:</td>
<td colspan="2" class="diff-lineno">Line 66:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>magnetic field and the electron velocity &mu; = 0.5, we find that</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>magnetic field and the electron velocity &mu; = 0.5, we find that</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>accelerated electrons will be collisionaly stopped in the coronal</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>accelerated electrons will be collisionaly stopped in the coronal</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>part of a flare loop if their energy </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>part of a flare loop if their energy <ins class="diffchange diffchange-inline">E < </ins>E<sub>loop</sub> ~ 10 <ins class="diffchange diffchange-inline">(N</ins><<ins class="diffchange diffchange-inline">sub</ins>><ins class="diffchange diffchange-inline">19</ins></<ins class="diffchange diffchange-inline">sub</ins>><ins class="diffchange diffchange-inline">/&mu;)</ins><sup><ins class="diffchange diffchange-inline">1/</ins>2</sup> = 45-63 keV,</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>E<sub>loop</sub> ~ 10<<del class="diffchange diffchange-inline">sup</del>><del class="diffchange diffchange-inline">xxx</del></<del class="diffchange diffchange-inline">sup</del>> <del class="diffchange diffchange-inline">cm</del><sup><del class="diffchange diffchange-inline">-</del>2</sup></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>where N<ins class="diffchange diffchange-inline"><sub>19<</ins>/<ins class="diffchange diffchange-inline">sub> = </ins>10<ins class="diffchange diffchange-inline"><sup></ins>19<ins class="diffchange diffchange-inline"></sup>N</ins></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">10 \sqrt{N_{19}/\mu}</del>=45-63<del class="diffchange diffchange-inline">$~</del>keV, where <del class="diffchange diffchange-inline">$N_{19} =</del>N/10<del class="diffchange diffchange-inline">^{</del>19<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></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div> </div></td><td class='diff-marker'>+</td><td style="background: #cfc; 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>The relationship between the spectral fluxes of hard X-ray</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The relationship between the spectral fluxes of hard X-ray</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>emission at the coronal part $I_{lp}$ and the footpoints $I_{fp}$</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>emission at the coronal part $I_{lp}$ and the footpoints $I_{fp}$</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 108:</td>
<td colspan="2" class="diff-lineno">Line 110:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[5] [http://adsabs.harvard.edu/abs/2015SoPh..290.3559Z "Particle acceleration and plasma heating in the chromosphere"]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[5] [http://adsabs.harvard.edu/abs/2015SoPh..290.3559Z "Particle acceleration and plasma heating in the chromosphere"]</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>[6] [1998ARep...42..275T "The stochastic acceleration of upper chromospheric electrons"]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[6] [<ins class="diffchange diffchange-inline">http://adsabs.harvard.edu/abs/</ins>1998ARep...42..275T "The stochastic acceleration of upper chromospheric electrons"]</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Electron_acceleration_and_hard_X-ray_emission_from_SOL2013-11-09&diff=8920&oldid=prevHhudson: initial entry for Nugget 2732016-05-03T18:22:14Z<p>initial entry for Nugget 273</p>
<p><b>New page</b></p><div>{{Infobox Nugget<br />
|name = Nugget<br />
|title = Electron Acceleration and Hard X-ray Emission from SOL2013-11-09<br />
|number = 273 <br />
|first_author = Yuri Tsap<br />
|second_author = Galina Motorina<br />
|publish_date = 5 May 2016 <br />
|next_nugget = Non-thermal recombination radiation <br />
|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Extreme_events,_stellar_evolution,_and_magnetic_reconnection Extreme events]<br />
}}<br />
<br />
=== Introduction ===<br />
<br />
The acceleration of high-energy particles has long been recognized as <br />
one of the fundamental characteristics of a solar flare.<br />
<br />
Until now it has not been clear exactly where the electron acceleration region<br />
is located during the flare energy release. <br />
It is usually considered that electrons are accelerated in the corona. <br />
In particular, they can be accelerated in the region of the looptop<br />
(models with a compact acceleration region) or in the whole loop<br />
(models with an extended acceleration region). <br />
In our view, we can shed light on this issue based on the relationship <br />
between hard X-ray emissions from the coronal part (looptop) of a flare loop<br />
and its footpoints.<br />
<br />
This Nugget is devoted to the analysis of the hard X-ray emission<br />
from different parts of a flare loop based on RHESSI observations<br />
for the well-studied solar flare onSOL2013-11-09 (C1.2) [1,2].<br />
<br />
=== Relationships between hard X-ray emissions from different ===<br />
<br />
The hard X-ray images (Figure 1) of the solar flare SOL2013-11-09 (C2.6)<br />
show three sources [1]. <br />
One of them was located between two others and characterized by the <br />
strong hard X-ray emission dominated in some time intervals. <br />
This appears to correspond to the looptop.<br />
<br />
[[File:273f1.png|700px|thumb|center|Figure 1: <br />
SDO/AIA 171 &#8491; image (in inverted colors)<br />
overlaid with RHESSI images at 4.1-4.9~keV (white) near the peak<br />
of the impulsive phase, with contours at 50, 70 and 90% of the<br />
maximum of each image, and at 23.0-27.5 keV (blue, levels 50,<br />
60, 70, 80, 90 of the image maximum) integrated for ~300 s, <br />
covering the entire main impulsive phase (time intervals<br />
indicated in the figure legend).<br />
]]<br />
<br />
The RHESSI imaging appears to resolve this looptop source as a<br />
dense [1], [2] (n<sub>e</sub> ~ 3 x 10<sup>11</sup> cm<sup>-3</sup><br />
and a characteristic size L ~ 9-18 arcsec.<br />
These estiates apply at the maximum of the hard X-ray emission (06:25:41~UT) <br />
in terms of the simultaneous <br />
[http://global.jaxa.jp/projects/sat/solar_b/ Hinode]/[http://solarb.mssl.ucl.ac.uk/SolarB/Solar-B.jsp EIS]<br />
observations [1].<br />
The high plasma density suggests that accelerated<br />
electrons should lose the kinetic energy quite fast while<br />
propagating from the looptop to the footpoints. <br />
In particular, supposing the<br />
coronal loop column density <br />
1-2 x 10<sup>20</sup> cm<sup>-2</sup>, and that<br />
the cosine between the direction of the<br />
magnetic field and the electron velocity &mu; = 0.5, we find that<br />
accelerated electrons will be collisionaly stopped in the coronal<br />
part of a flare loop if their energy <br />
E<sub>loop</sub> ~ 10<sup>xxx</sup> cm<sup>-2</sup><br />
10 \sqrt{N_{19}/\mu}=45-63$~keV, where $N_{19} =N/10^{19}$.<br />
<br />
The relationship between the spectral fluxes of hard X-ray<br />
emission at the coronal part $I_{lp}$ and the footpoints $I_{fp}$<br />
as it follows from the collisional thick target model can be<br />
represented as [3]<br />
<br />
[[File:273f2.png|500px|thumb|center<br />
]]<br />
<br />
where B(a, b, c) is an incomplete beta function and delta is the <br />
spectral index of the electrons. <br />
Then, adopting delta = 5.6 and E<sub>loop</sub> = 0.5, we<br />
find I<sub>lp</sub>/ I<sub>fp</sub> ~ 11.<br />
The estimate thus obtained contradicts the<br />
observed intensities of the hard X-ray sources in the energy range<br />
23.0-27.5 keV (see Fig.1) and demonstrates that the standard<br />
solar flare model requires at least some modifications.<br />
<br />
=== Conclusions ===<br />
<br />
The discrepancy between the model estimates and hard X-ray<br />
observations suggests that electron acceleration can occur not<br />
only in the coronal part of a loop but also in the footpoints.<br />
This inference well agrees well with the idea of re-acceleration [4]<br />
as well as the solar flare model proposed by Zaitsev and<br />
Stepanov [5]; see also [6]. <br />
Note that an extended acceleration region in the corona does not<br />
significantly improve the relationship (1) since the generation of<br />
the hard X-ray emission in the coronal part will be more effective<br />
in this case.<br />
<br />
<br />
[1] [http://adsabs.harvard.edu/abs/2015A%26A...577A..68S "Direct observation of the energy release site in a solar flare by SDO/AIA, Hinode/EIS, and RHESSI"]<br />
<br />
[2] [http://adsabs.harvard.edu/abs/2015SoPh..290.3573S "Impulsive heating of solar flare ribbons above 10 MK"]<br />
<br />
[3] [http://adsabs.harvard.edu/abs/2004ApJ...603L.117V "A coronal thick-target interpretation of two hard X-ray loop events"]<br />
<br />
[4] [http://adsabs.harvard.edu/abs/2009A%26A...508..993B "Local re-acceleration and a modified thick target model of solar flare electrons"]<br />
<br />
[5] [http://adsabs.harvard.edu/abs/2015SoPh..290.3559Z "Particle acceleration and plasma heating in the chromosphere"]<br />
<br />
[6] [1998ARep...42..275T "The stochastic acceleration of upper chromospheric electrons"]</div>Hhudson