https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&feed=atom&action=historyPhotospheric Electric Fields and Energy Fluxes in the Eruptive Active Region NOAA 11158 - Revision history2024-03-29T00:36:50ZRevision history for this page on the wikiMediaWiki 1.16.0https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8423&oldid=prevMariaKazachenko: /* Introduction */2015-09-13T18:17:21Z<p><span class="autocomment">Introduction</span></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>''First,'' if we know both electric and magnetic field vectors in the photosphere, we can estimate both the Poynting flux of magnetic energy and the flux of relative magnetic helicity entering the corona. ''Second,'' knowledge of electric and magnetic fields enables the driving of time-dependent simulations of the coronal magnetic field. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>''First,'' if we know both electric and magnetic field vectors in the photosphere, we can estimate both the Poynting flux of magnetic energy and the flux of relative magnetic helicity entering the corona. ''Second,'' knowledge of electric and magnetic fields enables the driving of time-dependent simulations of the coronal magnetic field. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>This is the goal of the Coronal Global Evolutionary Model ([http://cgem.stanford.edu CGEM]).</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This is the goal of the Coronal Global Evolutionary Model ([http://cgem.stanford.edu CGEM<ins class="diffchange diffchange-inline">], Ref. [4</ins>]).</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A particular active region, [http://www.solarmonitor.org/index.php?date=20110213&region=11158 NOAA 11158], has attracted particular attention.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>A particular active region, [http://www.solarmonitor.org/index.php?date=20110213&region=11158 NOAA 11158], has attracted particular attention.</div></td></tr>
</table>MariaKazachenkohttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8422&oldid=prevMariaKazachenko: /* Poynting Flux: preflare vs postflare */2015-09-13T18:15:17Z<p><span class="autocomment">Poynting Flux: preflare vs postflare</span></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Poynting Flux: preflare vs postflare===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Poynting Flux: preflare vs postflare===</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[[File:Fig10_zoom.png|700px|thumb|center|Figure 4. Horizontal (arrows) and vertical (background) Poynting vector field components at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to Sh in positive and negative areas of the background Sz. The range of the background Sz is [-1, 1] 10<sup>10</sup> erg <del class="diffchange diffchange-inline">cm−2 s−1 </del>in the left panels and [-0.4, 0.4] 10<sup>10</sup> erg <del class="diffchange diffchange-inline">cm−2 s−1 </del> in the right panel.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig10_zoom.png|700px|thumb|center|Figure 4. Horizontal (arrows) and vertical (background) Poynting vector field components at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to Sh in positive and negative areas of the background Sz. The range of the background Sz is [-1, 1] 10<sup>10</sup> <ins class="diffchange diffchange-inline"> </ins>erg <ins class="diffchange diffchange-inline">cm<sup>-2</sup>s<sup>-1</sup> </ins>in the left panels and [-0.4, 0.4] 10<sup>10</sup> erg <ins class="diffchange diffchange-inline">cm<sup>-2</sup>s<sup>-1</sup> </ins> in the right panel.]]</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>We find the photospheric Poynting ranging from [-0.6 to 2.3] 10<sup>10</sup> erg cm<sup>-2</sup>s<sup>-1</sup> with majority of the energy flux moving upward into corona. More than half of the total energy input rate is injected from within the range of Sz = [10<sup>9</sup>, 10<sup>10</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>, while the rest of the energy is injected in the range of [10<sup><del class="diffchange diffchange-inline">9</del></sup>, 10<sup>9</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>. The strongest Poynting flux is concentrated at the PIL.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>We find the photospheric Poynting ranging from [-0.6 to 2.3] 10<sup>10</sup> erg cm<sup>-2</sup>s<sup>-1</sup> with majority of the energy flux moving upward into corona. More than half of the total energy input rate is injected from within the range of Sz = [10<sup>9</sup>, 10<sup>10</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>, while the rest of the energy is injected in the range of [10<sup><ins class="diffchange diffchange-inline">8</ins></sup>, 10<sup>9</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>. The strongest Poynting flux is concentrated at the PIL.</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Six-day Evolution of Vertical Energy Flux===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Six-day Evolution of Vertical Energy Flux===</div></td></tr>
</table>MariaKazachenkohttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8421&oldid=prevMariaKazachenko: /* Poynting Flux: preflare vs postflare */2015-09-13T18:13:32Z<p><span class="autocomment">Poynting Flux: preflare vs postflare</span></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Poynting Flux: preflare vs postflare===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Poynting Flux: preflare vs postflare===</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:Fig10_zoom.png|700px|thumb|center|Figure 4. Horizontal (arrows) and vertical (background) Poynting vector field components at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to Sh in positive and negative areas of the background Sz. The range of the background Sz is [-1, 1] <del class="diffchange diffchange-inline">1010 </del>erg cm−2 s−1 in the left panels and [-0.4, 0.4] <del class="diffchange diffchange-inline">1010 </del>erg cm−2 s−1 in the right panel.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig10_zoom.png|700px|thumb|center|Figure 4. Horizontal (arrows) and vertical (background) Poynting vector field components at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to Sh in positive and negative areas of the background Sz. The range of the background Sz is [-1, 1] <ins class="diffchange diffchange-inline">10<sup>10</sup> </ins>erg cm−2 s−1 in the left panels and [-0.4, 0.4] <ins class="diffchange diffchange-inline">10<sup>10</sup> </ins>erg cm−2 s−1 in the right panel.]]</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>We find the photospheric Poynting ranging from [-0.6 to 2.3] 10<sup>10</sup> erg cm<sup>-2</sup>s<sup>-1</sup> with majority of the energy flux moving upward into corona. More than half of the total energy input rate is injected from within the range of Sz = [10<sup>9</sup>, 10<sup>10</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>, while the rest of the energy is injected in the range of [10<sup>9</sup>, 10<sup>9</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>. The strongest Poynting flux is concentrated at the PIL.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We find the photospheric Poynting ranging from [-0.6 to 2.3] 10<sup>10</sup> erg cm<sup>-2</sup>s<sup>-1</sup> with majority of the energy flux moving upward into corona. More than half of the total energy input rate is injected from within the range of Sz = [10<sup>9</sup>, 10<sup>10</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>, while the rest of the energy is injected in the range of [10<sup>9</sup>, 10<sup>9</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>. The strongest Poynting flux is concentrated at the PIL.</div></td></tr>
</table>MariaKazachenkohttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8420&oldid=prevMariaKazachenko: /* Results */2015-09-13T18:04:21Z<p><span class="autocomment">Results</span></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Results==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Results==</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>To describe the photospheric electric fields E and energy fluxes S in NOAA 11158, we use two approaches: we first show the spatial distribution of the B, E and S fields at two times, before and after the X2.2 flare; we then analyze their temporal spatially integrated evolution over six days of observations. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>To describe the photospheric electric fields E and energy fluxes S in NOAA 11158, we use two approaches: we first show the spatial distribution of the B, E and S fields at two times, before and after the X2.2 flare; we then analyze their temporal spatially integrated evolution over six days of observations<ins class="diffchange diffchange-inline">. For more details of the analysis see Ref. [5]</ins>.</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Magnetic Field: preflare vs postflare===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Magnetic Field: preflare vs postflare===</div></td></tr>
</table>MariaKazachenkohttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8419&oldid=prevMariaKazachenko at 18:01, 13 September 20152015-09-13T18:01:25Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[4] [http://cdsads.u-strasbg.fr/abs/2015SpWea..13..369F "The Coronal Global Evolutionary Model: Using HMI Vector Magnetogram and Doppler Data to Model the Buildup of Free Magnetic Energy in the Solar Corona"]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[4] [http://cdsads.u-strasbg.fr/abs/2015SpWea..13..369F "The Coronal Global Evolutionary Model: Using HMI Vector Magnetogram and Doppler Data to Model the Buildup of Free Magnetic Energy in the Solar Corona"]</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>[5] [http://cdsads.u-strasbg.fr/abs/2015arXiv150505974K "Photospheric Electric Fields and Energy Fluxes in the Eruptive Active Region NOAA 11158"]<del class="diffchange diffchange-inline">)</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[5] [http://cdsads.u-strasbg.fr/abs/2015arXiv150505974K "Photospheric Electric Fields and Energy Fluxes in the Eruptive Active Region NOAA 11158"]</div></td></tr>
</table>MariaKazachenkohttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8418&oldid=prevMariaKazachenko at 18:00, 13 September 20152015-09-13T18:00:07Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We have recently improved the electric field inversion methods introduced in Ref. [1] to create a comprehensive technique for calculating photospheric electric fields from </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We have recently improved the electric field inversion methods introduced in Ref. [1] to create a comprehensive technique for calculating photospheric electric fields from </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[https://en.wikipedia.org/wiki/Vector_magnetograph vector magnetogram] image sequences. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[https://en.wikipedia.org/wiki/Vector_magnetograph vector magnetogram] image sequences. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>The new method, which we dubbed the PDFI (an abbreviation for '''P'''TD-'''D'''oppler-'''F'''LCT-'''I'''deal technique, where PTD and FLCT stand for Poloidal-Toroidal Decomposition </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The new method, which we dubbed the PDFI (an abbreviation for '''P'''TD-'''D'''oppler-'''F'''LCT-'''I'''deal technique, where PTD and FLCT stand for Poloidal-Toroidal Decomposition and Fourier Local Correlation Tracking, respectively), has been systematically tested for accuracy and robustness, using synthetic data from simulations <ins class="diffchange diffchange-inline">(see Ref. [2])</ins>. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>and Fourier Local Correlation Tracking, respectively), has been systematically tested for accuracy and robustness, using synthetic data from simulations. </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>Here we take the next step forward, and apply the PDFI technique directly to observations.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Here we take the next step forward, and apply the PDFI technique directly to observations.</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>MariaKazachenkohttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8414&oldid=prevHhudson: finished light editing2015-09-13T09:59:22Z<p>finished light editing</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 14 September 2015</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 14 September 2015</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|next_nugget = GOES photometry</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|next_nugget = GOES photometry</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/RHESSI and General Relativity]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/<ins class="diffchange diffchange-inline">RHESSI_and_General_Relativity </ins>RHESSI and General Relativity]</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>== Introduction ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Introduction ==</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Flares, CMEs, and other forms of spontaneous energy release - including hard X-ray and gamma-ray bursts - require the gradual build-up of ''free energy'' in the solar corona.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Flares, CMEs, and other forms of spontaneous <ins class="diffchange diffchange-inline">solar </ins>energy release - including <ins class="diffchange diffchange-inline">RHESSI's </ins>hard X-ray and gamma-ray bursts - <ins class="diffchange diffchange-inline">seem to </ins>require the gradual build-up of ''free energy'' in the solar corona.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We are sure that this must come from the gradual transport of energy from the interior to the corona, but in the form of plasma effects rather than electromagnetic radiation (light waves).</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We are sure that this must come from the gradual transport of energy from the interior to the corona, but in the form of plasma effects rather than electromagnetic radiation (light waves).</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This is describable as a form of [https://en.wikipedia.org/wiki/Poynting%27s_theorem Poynting flux], but one that flows at the [http://www.plasma-universe.com/Alfvén_wave Alfv&eacute;n speed]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This is describable as a form of [https://en.wikipedia.org/wiki/Poynting%27s_theorem Poynting flux], but one that flows at the [http://www.plasma-universe.com/Alfvén_wave Alfv&eacute;n speed]</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 21:</td>
<td colspan="2" class="diff-lineno">Line 21:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>''First,'' if we know both electric and magnetic field vectors in the photosphere, we can estimate both the Poynting flux of magnetic energy and the flux of relative magnetic helicity entering the corona. ''Second,'' knowledge of electric and magnetic fields enables the driving of time-dependent simulations of the coronal magnetic field. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>''First,'' if we know both electric and magnetic field vectors in the photosphere, we can estimate both the Poynting flux of magnetic energy and the flux of relative magnetic helicity entering the corona. ''Second,'' knowledge of electric and magnetic fields enables the driving of time-dependent simulations of the coronal magnetic field. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>This is the goal of the Coronal Global Evolutionary Model ([http://cgem.stanford.edu CGEM],</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This is the goal of the Coronal Global Evolutionary Model ([http://cgem.stanford.edu CGEM]<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> </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">A particular active region</ins>, <ins class="diffchange diffchange-inline">[http://www.solarmonitor.org/index.php?date=20110213&region=11158 NOAA 11158], has attracted particular attention.</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">This region produced excellent observations over a wide range of wavelengths, and produced the first X-class flare of Cycle 24: SOL2011-02-15 and a flood of interesting literature.</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>== Method and Data ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Method and Data ==</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 36:</td>
<td colspan="2" class="diff-lineno">Line 39:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We used this sequence of 770 vector magnetic field and velocity measurements to derive the temporal evolution of electric fields E and Poynting fluxes S during these six days.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We used this sequence of 770 vector magnetic field and velocity measurements to derive the temporal evolution of electric fields E and Poynting fluxes S during these six days.</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:Fig06.png|700px|thumb|center|Figure 1: (A)–(D): HMI vertical magnetic field (Bz) maps at four different times of NOAA 11158 <del class="diffchange diffchange-inline">evolution</del>. Panel (E): positive/negative vertical magnetic fluxes during the 6-day interval. Diamonds indicate the times of images on the left. An X2.2 flare is marked with the dashed line. ]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig06.png|700px|thumb|center|Figure 1: (A)–(D): HMI vertical magnetic field (Bz) maps at four different times <ins class="diffchange diffchange-inline">in the evolution </ins>of NOAA 11158. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Panel (E): positive/negative vertical magnetic fluxes during the 6-day interval. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Diamonds indicate the times of images on the left. An X2.2 flare is marked with the dashed line. ]]</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>==Results==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Results==</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>To describe the photospheric electric fields E and energy fluxes S in NOAA 11158, we use two approaches: we first show the spatial distribution of B, E and S at two times, before and after the X2.2 flare; we then analyze their temporal spatially integrated evolution over six days of observations. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>To describe the photospheric electric fields E and energy fluxes S in NOAA 11158, we use two approaches: we first show the spatial distribution of <ins class="diffchange diffchange-inline">the </ins>B, E and S <ins class="diffchange diffchange-inline">fields </ins>at two times, before and after the X2.2 flare; we then analyze their temporal spatially integrated evolution over six days of observations. </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>===Magnetic Field: preflare vs postflare===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Magnetic Field: preflare vs postflare===</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:Fig07 bz zoom.png|700px|thumb|center|Figure 2. Horizontal (arrows) and vertical (grayscale) components of the magnetic field in NOAA 11158 at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to horizontal fields in areas of positive and negative <del class="diffchange diffchange-inline">Bz</del>.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig07 bz zoom.png|700px|thumb|center|Figure 2. Horizontal (arrows) and vertical (grayscale) components of the magnetic field in NOAA 11158 at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to horizontal fields in areas of positive and negative <ins class="diffchange diffchange-inline">B<sub>z</sub></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>Pre- and post-flare snapshots of the vertical magnetic field (Figure 2) show that the horizontal magnetic field close to PIL increased by over 300 G during the X2.2 flare (see arrows), while the vertical magnetic field remained nearly constant, consistent with the field implosion scenario. On the difference image (right panel) we also notice two circular patterns, directed counter-clockwise in negative and clockwise in positive polarities, implying that the field connecting those polarities becomes less twisted during the flare.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Pre- and post-flare snapshots of the vertical magnetic field (Figure 2) show that the horizontal magnetic field close to <ins class="diffchange diffchange-inline">the</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">''photospheric inversion line'' (</ins>PIL<ins class="diffchange diffchange-inline">) </ins>increased by over 300 G during the X2.2 flare (see arrows), while the vertical magnetic field remained nearly constant, consistent with the field implosion scenario. </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">The PIL separates the regions of opposite B<sub>z</sub> orientation, i.e. up and down.</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>On the difference image (right panel) we also notice two circular patterns, directed counter-clockwise in negative and clockwise in positive polarities, implying that the field connecting those polarities becomes less twisted during the flare.</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>===Electric Field: preflare vs postflare===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Electric Field: preflare vs postflare===</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 52:</td>
<td colspan="2" class="diff-lineno">Line 60:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:Fig09.png|700px|thumb|center|Figure 3. Horizontal (arrows) and vertical (grayscale) components of the electric field at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to horizontal fields in areas of positive and negative Ez.]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:Fig09.png|700px|thumb|center|Figure 3. Horizontal (arrows) and vertical (grayscale) components of the electric field at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to horizontal fields in areas of positive and negative Ez.]]</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>We find the photospheric electric field vector, ranging from -2 to 2 V/cm, to increase its magnitude by up to 0.5 V/cm at the PIL and 1 V/cm away from the PIL during the flare (Figure 3). The horizontal component is mostly concentrated along the PIL, while the vertical component is largest at the PIL and in the sunspots’ penumbrae. The presence of a nonzero Ez is related to changes in the vertical current, which is mostly concentrated close to the main PIL (<del class="diffchange diffchange-inline">Petrie 2013; Janvier et al</del>. <del class="diffchange diffchange-inline">2014</del>)<del class="diffchange diffchange-inline">.</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>We find the photospheric electric field vector, ranging from -2 to 2 V/cm, to increase its magnitude by up to 0.5 V/cm at the PIL and 1 V/cm away from the PIL during the flare (Figure 3). The horizontal component is mostly concentrated along the PIL, while the vertical component is largest at the PIL and in the sunspots’ penumbrae. The presence of a nonzero Ez is related to changes in the vertical current, which is mostly concentrated close to the main PIL (<ins class="diffchange diffchange-inline">Ref</ins>. <ins class="diffchange diffchange-inline">[3]</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>===Poynting Flux: preflare vs postflare===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Poynting Flux: preflare vs postflare===</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:Fig10_zoom.png|700px|thumb|<del class="diffchange diffchange-inline">left</del>|Figure 4. Horizontal (arrows) and vertical (background) Poynting vector field components at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to Sh in positive and negative areas of the background Sz. The range of the background Sz is [-1, 1] 1010 erg cm−2 s−1 in the left panels and [-0.4, 0.4] 1010 erg cm−2 s−1 in the right panel.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig10_zoom.png|700px|thumb|<ins class="diffchange diffchange-inline">center</ins>|Figure 4. Horizontal (arrows) and vertical (background) Poynting vector field components at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to Sh in positive and negative areas of the background Sz. The range of the background Sz is [-1, 1] 1010 erg cm−2 s−1 in the left panels and [-0.4, 0.4] 1010 erg cm−2 s−1 in the right panel.]]</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>We find the photospheric Poynting ranging from [-0.6 to 2.3] 10<sup>10</sup> erg cm<sup>-2</sup>s<sup>-1</sup> with majority of the energy flux moving upward into corona. More than half of the total energy input rate is injected from within the range of Sz = [10<sup>9</sup>, 10<sup>10</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>, while the rest of the energy is injected in the range of [10<sup>9</sup>, 10<sup>9</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>. The strongest Poynting flux is concentrated at the PIL.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We find the photospheric Poynting ranging from [-0.6 to 2.3] 10<sup>10</sup> erg cm<sup>-2</sup>s<sup>-1</sup> with majority of the energy flux moving upward into corona. More than half of the total energy input rate is injected from within the range of Sz = [10<sup>9</sup>, 10<sup>10</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>, while the rest of the energy is injected in the range of [10<sup>9</sup>, 10<sup>9</sup> ] erg cm<sup>-2</sup>s<sup>-1</sup>. The strongest Poynting flux is concentrated at the PIL.</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 62:</td>
<td colspan="2" class="diff-lineno">Line 70:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Six-day Evolution of Vertical Energy Flux===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Six-day Evolution of Vertical Energy Flux===</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>Integrating the Poynting flux in time and spatially over the NOAA 11158, we find the total magnetic energy before the flare to be E=[10.6+-3.1] 10<sup>32</sup> erg. In spite of a very different approach, it is consistent within the uncertainty with the total energies from [http://iopscience.iop.org/article/10.1088/0004-637X/761/2/105/meta DAVE4VM], [http://iopscience.iop.org/article/10.1088/0004-637X/770/1/4/meta MCC] and [http://iopscience.iop.org/article/10.1088/0004-637X/748/2/77/meta NLFFF <del class="diffchange diffchange-inline">methods</del>] estimates and larger than the [http://dx.doi.org/10.1088/0004-637X/783/2/102 coronal NLFFF estimates].</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Integrating the Poynting flux in time and spatially over the NOAA 11158, we find the total magnetic energy before the flare to be E=[10.6+-3.1] 10<sup>32</sup> erg. In spite of a very different approach, it is consistent within the uncertainty with the total energies from [http://iopscience.iop.org/article/10.1088/0004-637X/761/2/105/meta DAVE4VM], [http://iopscience.iop.org/article/10.1088/0004-637X/770/1/4/meta MCC] and [http://iopscience.iop.org/article/10.1088/0004-637X/748/2/77/meta NLFFF <ins class="diffchange diffchange-inline">method</ins>] estimates and larger than the [http://dx.doi.org/10.1088/0004-637X/783/2/102 coronal NLFFF estimates].</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>== Conclusion ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Conclusion ==</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>This study is the first application of the PDFI electric field inversion technique to photospheric vector magnetic field and Doppler measurements. We find that the total amount of energy injected through the photosphere before the flare estimated by the PDFI method is consistent with estimates from other approaches, in spite of differing techniques. This agreement is very promising, implying that the PDFI technique is not only capable of describing the coronal energy and helicity budget, but can also provide instantaneous estimates of energy and helicity transferred through the photosphere. We believe that both the derived dataset of PDFI electric fields and the PDFI method itself will be useful to the science community for analysis of the evolution and spatial distribution of the photospheric electric fields, fluxes of energy and helicity, and their relationships with flare activity. In addition, PDFI electric fields can be used as time-dependent boundary conditions for data-driven models of coronal magnetic field evolution. The dataset of magnetic and electric fields and Poynting fluxes in NOAA 11158 is available for downloading on [http://cgem.stanford.edu our website].</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This study is the first application of the PDFI electric field inversion technique to photospheric vector magnetic field and Doppler measurements. We find that the total amount of energy injected through the photosphere before the flare estimated by the PDFI method is consistent with estimates from other approaches, in spite of differing techniques. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This agreement is very promising, implying that the PDFI technique is not only capable of describing the coronal energy and helicity budget, but can also provide instantaneous estimates of energy and helicity transferred through the photosphere. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>We believe that both the derived dataset of PDFI electric fields and the PDFI method itself will be useful to the science community for analysis of the evolution and spatial distribution of the photospheric electric fields, fluxes of energy and helicity, and their relationships with flare activity. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>In addition, PDFI electric fields can be used as time-dependent boundary conditions for data-driven models of coronal magnetic field evolution. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The dataset of magnetic and electric fields and Poynting fluxes in NOAA 11158 is available for downloading on [http://cgem.stanford.edu our website].</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>
<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>[1] [http://cdsads.u-strasbg.fr/abs/2010ApJ...715..242F <del class="diffchange diffchange-inline">Fisher et al</del>. <del class="diffchange diffchange-inline">(2010)</del>]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[1] [http://cdsads.u-strasbg.fr/abs/2010ApJ...715..242F <ins class="diffchange diffchange-inline">"Estimating Electric Fields from Vector Magnetogram Sequences"]</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div> </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">[2] [http://cdsads</ins>.<ins class="diffchange diffchange-inline">u-strasbg.fr/abs/2014ApJ...795...17K "A Comprehensive Method of Estimating Electric Fields from Vector Magnetic Field and Doppler Measurements"]</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div> </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">[3] [http://adsabs.harvard.edu/abs/2013SoPh..287..415P "A Spatio-temporal Description of the Abrupt Changes in the Photospheric Magnetic and Lorentz-Force Vectors During the 15 February 2011 X2.2 Flare"</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">2</del>] [http://cdsads.u-strasbg.fr/abs/<del class="diffchange diffchange-inline">2014ApJ</del>...<del class="diffchange diffchange-inline">795</del>.<del class="diffchange diffchange-inline">..17K Kazachenko et al. 2014</del>]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[<ins class="diffchange diffchange-inline">4</ins>] [http://cdsads.u-strasbg.fr/abs/<ins class="diffchange diffchange-inline">2015SpWea</ins>..<ins class="diffchange diffchange-inline">13</ins>..<ins class="diffchange diffchange-inline">369F "The Coronal Global Evolutionary Model: Using HMI Vector Magnetogram and Doppler Data to Model the Buildup of Free Magnetic Energy in the Solar Corona"</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"> </del>[<del class="diffchange diffchange-inline">http://cdsads.u-strasbg.fr/abs/2015SpWea..13..369F Fisher et al. 2015</del>]<del class="diffchange diffchange-inline">, </del>[http://cdsads.u-strasbg.fr/abs/2015arXiv150505974K <del class="diffchange diffchange-inline">Kazachenko et al. 2015</del>])</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[<ins class="diffchange diffchange-inline">5</ins>] [http://cdsads.u-strasbg.fr/abs/2015arXiv150505974K <ins class="diffchange diffchange-inline">"Photospheric Electric Fields and Energy Fluxes in the Eruptive Active Region NOAA 11158"</ins>])</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8413&oldid=prevHhudson: light edits, first half2015-09-11T19:30:30Z<p>light edits, first half</p>
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<td colspan='2' style="background-color: white; color:black;">Revision as of 19:30, 11 September 2015</td>
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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;">{{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 style="color: red; font-weight: bold; text-decoration: none;">|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 style="color: red; font-weight: bold; text-decoration: none;">|title = Photospheric Electric Fields and Energy Fluxes in the Eruptive Active Region NOAA 11158 </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 style="color: red; font-weight: bold; text-decoration: none;">|number = 261</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 style="color: red; font-weight: bold; text-decoration: none;">|first_author = Maria Kazachenko </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 style="color: red; font-weight: bold; text-decoration: none;">|second_author = </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 style="color: red; font-weight: bold; text-decoration: none;">|publish_date = 14 September 2015</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 style="color: red; font-weight: bold; text-decoration: none;">|next_nugget = GOES photometry</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 style="color: red; font-weight: bold; text-decoration: none;">|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/RHESSI and General Relativity]</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 style="color: red; font-weight: bold; text-decoration: none;">}}</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 style="color: red; font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Introduction ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Introduction ==</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">The advent </del>of <del class="diffchange diffchange-inline">high</del>-<del class="diffchange diffchange-inline">cadence vector magnetic field </del>and <del class="diffchange diffchange-inline">Doppler velocity measurements from e.g. [http://hmi.stanford.edu/ HMI/SDO], [http://sot.lmsal.com/ SOT/Hinode] and [http://solis.nso.edu/0/index.html SOLIS], have made </del>the <del class="diffchange diffchange-inline">estimation </del>of <del class="diffchange diffchange-inline">electric fields in the solar photosphere possible. The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. </del>''<del class="diffchange diffchange-inline">First,</del>'' <del class="diffchange diffchange-inline">if we know both electric and magnetic field vectors </del>in the <del class="diffchange diffchange-inline">photosphere, we can estimate both </del>the <del class="diffchange diffchange-inline">Poynting flux </del>of <del class="diffchange diffchange-inline">magnetic </del>energy <del class="diffchange diffchange-inline">and </del>the <del class="diffchange diffchange-inline">flux of relative magnetic helicity entering </del>the corona<del class="diffchange diffchange-inline">. ''Second</del>,<del class="diffchange diffchange-inline">'' knowledge of electric and magnetic fields enables </del>the <del class="diffchange diffchange-inline">driving </del>of <del class="diffchange diffchange-inline">time-dependent simulations of the coronal magnetic field</del>. This is <del class="diffchange diffchange-inline">the goal </del>of <del class="diffchange diffchange-inline">the Coronal Global Evolutionary Model (</del>[<del class="diffchange diffchange-inline">http</del>://<del class="diffchange diffchange-inline">cgem</del>.<del class="diffchange diffchange-inline">stanford</del>.<del class="diffchange diffchange-inline">edu CGEM</del>], [http://<del class="diffchange diffchange-inline">cdsads</del>.<del class="diffchange diffchange-inline">u</del>-<del class="diffchange diffchange-inline">strasbg</del>.<del class="diffchange diffchange-inline">fr</del>/<del class="diffchange diffchange-inline">abs/2015SpWea..13..369F Fisher et al. 2015</del>]<del class="diffchange diffchange-inline">, </del>[http://<del class="diffchange diffchange-inline">cdsads</del>.<del class="diffchange diffchange-inline">u-strasbg</del>.<del class="diffchange diffchange-inline">fr</del>/<del class="diffchange diffchange-inline">abs</del>/<del class="diffchange diffchange-inline">2015arXiv150505974K Kazachenko et al</del>. <del class="diffchange diffchange-inline">2015</del>]<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">Flares, CMEs, and other forms </ins>of <ins class="diffchange diffchange-inline">spontaneous energy release </ins>- <ins class="diffchange diffchange-inline">including hard X-ray </ins>and <ins class="diffchange diffchange-inline">gamma-ray bursts - require </ins>the <ins class="diffchange diffchange-inline">gradual build-up </ins>of ''<ins class="diffchange diffchange-inline">free energy</ins>'' in the <ins class="diffchange diffchange-inline">solar 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">We are sure that this must come from </ins>the <ins class="diffchange diffchange-inline">gradual transport </ins>of energy <ins class="diffchange diffchange-inline">from </ins>the <ins class="diffchange diffchange-inline">interior to </ins>the corona, <ins class="diffchange diffchange-inline">but in </ins>the <ins class="diffchange diffchange-inline">form </ins>of <ins class="diffchange diffchange-inline">plasma effects rather than electromagnetic radiation (light waves)</ins>.</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This is <ins class="diffchange diffchange-inline">describable as a form </ins>of [<ins class="diffchange diffchange-inline">https</ins>://<ins class="diffchange diffchange-inline">en</ins>.<ins class="diffchange diffchange-inline">wikipedia</ins>.<ins class="diffchange diffchange-inline">org/wiki/Poynting%27s_theorem Poynting flux</ins>], <ins class="diffchange diffchange-inline">but one that flows at the </ins>[http://<ins class="diffchange diffchange-inline">www</ins>.<ins class="diffchange diffchange-inline">plasma</ins>-<ins class="diffchange diffchange-inline">universe</ins>.<ins class="diffchange diffchange-inline">com</ins>/<ins class="diffchange diffchange-inline">Alfvén_wave Alfv&eacute;n speed</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">rather than the </ins>[http://<ins class="diffchange diffchange-inline">www</ins>.<ins class="diffchange diffchange-inline">amnh</ins>.<ins class="diffchange diffchange-inline">org/education/resources</ins>/<ins class="diffchange diffchange-inline">rfl</ins>/<ins class="diffchange diffchange-inline">web/essaybooks/cosmic/p_roemer</ins>.<ins class="diffchange diffchange-inline">html speed of light</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">To estimate the Poynting flux one needs information about both the magnetic field in the plasma, and also the electric field - this latter is especially tricky</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">== Method ==</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">The advent of high-cadence vector magnetic field and Doppler velocity measurements from e.g. [http://hmi.stanford.edu/ HMI/SDO], [http://sot.lmsal.com/ SOT/Hinode] and [http://solis.nso.edu/0/index.html SOLIS], have made the estimation of electric fields in the solar photosphere possible. </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">The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. </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,'' if we know both electric and magnetic field vectors in the photosphere, we can estimate both the Poynting flux of magnetic energy and the flux of relative magnetic helicity entering the corona. ''Second,'' knowledge of electric and magnetic fields enables the driving of time-dependent simulations of the coronal magnetic field. </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">This is the goal of the Coronal Global Evolutionary Model ([http://cgem.stanford.edu CGEM],</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">We have recently improved the electric field inversion methods introduced by [http://cdsads.u-strasbg.fr/abs/2010ApJ...715..242F Fisher et al. (2010)], to create a comprehensive technique for calculating photospheric electric fields from vector magnetogram sequences ([http://cdsads.u-strasbg.fr/abs/2014ApJ...795...17K Kazachenko et al. 2014]). The new method, which we dubbed the PDFI (an abbreviation for '''P'''TD-'''D'''oppler-'''F'''LCT-'''I'''deal technique, where PTD </del>and <del class="diffchange diffchange-inline">FLCT stand for Poloidal-Toroidal Decomposition and Fourier Local Correlation Tracking), has been systematically tested for accuracy and robustness, using synthetic data from ANMHD simulations. Here we take the next step forward, and apply the PDFI technique to observations.</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">== Method </ins>and <ins class="diffchange diffchange-inline">Data ==</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">== Dataset ==</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">We have recently improved the electric field inversion methods introduced in Ref. [1] to create a comprehensive technique for calculating photospheric electric fields from </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">[https://en.wikipedia.org/wiki/Vector_magnetograph vector magnetogram] image sequences. </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">The new method, which we dubbed the PDFI (an abbreviation for '''P'''TD-'''D'''oppler-'''F'''LCT-'''I'''deal technique, where PTD and FLCT stand for Poloidal-Toroidal Decomposition </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">and Fourier Local Correlation Tracking, respectively), has been systematically tested for accuracy and robustness, using synthetic data from simulations. </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">Here we take the next step forward, and apply the PDFI technique directly to observations.</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 flare-productive active region (AR) NOAA 11158 was observed by <del class="diffchange diffchange-inline">HMI </del>nearly continuously for a six-day period over 2011 February 10–16 from its emergence (see <del class="diffchange diffchange-inline">Bz</del>-snapshots in Figure 1). We used <del class="diffchange diffchange-inline">the </del>sequence of 770 vector magnetic field <del class="diffchange diffchange-inline">B </del>and <del class="diffchange diffchange-inline">Doppler field </del>measurements to derive the temporal evolution of electric fields E and Poynting <del class="diffchange diffchange-inline">S </del>fluxes during these six days.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The flare-productive active region (AR) <ins class="diffchange diffchange-inline">[http://www.solarmonitor.org/index.php?date=20110213&region=11158 </ins>NOAA 11158<ins class="diffchange diffchange-inline">] </ins>was observed by <ins class="diffchange diffchange-inline">the </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://hmi.stanford.edu Solar Dynamics Observatory] </ins>nearly continuously for a six-day period over 2011 February 10–16<ins class="diffchange diffchange-inline">, right </ins>from its <ins class="diffchange diffchange-inline">first </ins>emergence (see <ins class="diffchange diffchange-inline">the B<sub>z</sub></ins>-snapshots in Figure 1<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">these show the vertical component of the solar magnetic field at the photosphere</ins>).</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>We used <ins class="diffchange diffchange-inline">this </ins>sequence of 770 vector magnetic field and <ins class="diffchange diffchange-inline">velocity </ins>measurements to derive the temporal evolution of electric fields E and Poynting fluxes <ins class="diffchange diffchange-inline">S </ins>during these six days.</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:Fig06.png|700px|thumb|<del class="diffchange diffchange-inline">left</del>|Figure 1: (A)–(D): HMI vertical magnetic field (Bz) maps at four different times of NOAA 11158 evolution. Panel (E): positive/negative vertical magnetic fluxes during the 6-day interval. Diamonds indicate the times of images on the left. An X2.2 flare is marked with the dashed line. ]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig06.png|700px|thumb|<ins class="diffchange diffchange-inline">center</ins>|Figure 1: (A)–(D): HMI vertical magnetic field (Bz) maps at four different times of NOAA 11158 evolution. Panel (E): positive/negative vertical magnetic fluxes during the 6-day interval. Diamonds indicate the times of images on the left. An X2.2 flare is marked with the dashed line. ]]</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>==Results==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Results==</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 19:</td>
<td colspan="2" class="diff-lineno">Line 44:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Magnetic Field: preflare vs postflare===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Magnetic Field: preflare vs postflare===</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:Fig07 bz zoom.png|700px|thumb|<del class="diffchange diffchange-inline">left</del>|Figure 2. Horizontal (arrows) and vertical (grayscale) components of the magnetic field in NOAA 11158 at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to horizontal fields in areas of positive and negative Bz.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig07 bz zoom.png|700px|thumb|<ins class="diffchange diffchange-inline">center</ins>|Figure 2. Horizontal (arrows) and vertical (grayscale) components of the magnetic field in NOAA 11158 at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to horizontal fields in areas of positive and negative Bz.]]</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>Pre- and post-flare snapshots of the vertical magnetic field (Figure 2) show that the horizontal magnetic field close to PIL increased by over 300 G during the X2.2 flare (see arrows), while the vertical magnetic field remained nearly constant, consistent with the field implosion scenario. On the difference image (right panel) we also notice two circular patterns, directed counter-clockwise in negative and clockwise in positive polarities, implying that the field connecting those polarities becomes less twisted during the flare.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Pre- and post-flare snapshots of the vertical magnetic field (Figure 2) show that the horizontal magnetic field close to PIL increased by over 300 G during the X2.2 flare (see arrows), while the vertical magnetic field remained nearly constant, consistent with the field implosion scenario. On the difference image (right panel) we also notice two circular patterns, directed counter-clockwise in negative and clockwise in positive polarities, implying that the field connecting those polarities becomes less twisted during the flare.</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 25:</td>
<td colspan="2" class="diff-lineno">Line 50:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Electric Field: preflare vs postflare===</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>===Electric Field: preflare vs postflare===</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:Fig09.png|700px|thumb|<del class="diffchange diffchange-inline">left</del>|Figure 3. Horizontal (arrows) and vertical (grayscale) components of the electric field at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to horizontal fields in areas of positive and negative Ez.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:Fig09.png|700px|thumb|<ins class="diffchange diffchange-inline">center</ins>|Figure 3. Horizontal (arrows) and vertical (grayscale) components of the electric field at preflare (top left) and postflare times (bottom left), and the difference image between the two (right panel). The blue and red colors correspond to horizontal fields in areas of positive and negative Ez.]]</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>We find the photospheric electric field vector, ranging from -2 to 2 V/cm, to increase its magnitude by up to 0.5 V/cm at the PIL and 1 V/cm away from the PIL during the flare (Figure 3). The horizontal component is mostly concentrated along the PIL, while the vertical component is largest at the PIL and in the sunspots’ penumbrae. The presence of a nonzero Ez is related to changes in the vertical current, which is mostly concentrated close to the main PIL (Petrie 2013; Janvier et al. 2014).</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>We find the photospheric electric field vector, ranging from -2 to 2 V/cm, to increase its magnitude by up to 0.5 V/cm at the PIL and 1 V/cm away from the PIL during the flare (Figure 3). The horizontal component is mostly concentrated along the PIL, while the vertical component is largest at the PIL and in the sunspots’ penumbrae. The presence of a nonzero Ez is related to changes in the vertical current, which is mostly concentrated close to the main PIL (Petrie 2013; Janvier et al. 2014).</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This study is the first application of the PDFI electric field inversion technique to photospheric vector magnetic field and Doppler measurements. We find that the total amount of energy injected through the photosphere before the flare estimated by the PDFI method is consistent with estimates from other approaches, in spite of differing techniques. This agreement is very promising, implying that the PDFI technique is not only capable of describing the coronal energy and helicity budget, but can also provide instantaneous estimates of energy and helicity transferred through the photosphere. We believe that both the derived dataset of PDFI electric fields and the PDFI method itself will be useful to the science community for analysis of the evolution and spatial distribution of the photospheric electric fields, fluxes of energy and helicity, and their relationships with flare activity. In addition, PDFI electric fields can be used as time-dependent boundary conditions for data-driven models of coronal magnetic field evolution. The dataset of magnetic and electric fields and Poynting fluxes in NOAA 11158 is available for downloading on [http://cgem.stanford.edu our website].</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This study is the first application of the PDFI electric field inversion technique to photospheric vector magnetic field and Doppler measurements. We find that the total amount of energy injected through the photosphere before the flare estimated by the PDFI method is consistent with estimates from other approaches, in spite of differing techniques. This agreement is very promising, implying that the PDFI technique is not only capable of describing the coronal energy and helicity budget, but can also provide instantaneous estimates of energy and helicity transferred through the photosphere. We believe that both the derived dataset of PDFI electric fields and the PDFI method itself will be useful to the science community for analysis of the evolution and spatial distribution of the photospheric electric fields, fluxes of energy and helicity, and their relationships with flare activity. In addition, PDFI electric fields can be used as time-dependent boundary conditions for data-driven models of coronal magnetic field evolution. The dataset of magnetic and electric fields and Poynting fluxes in NOAA 11158 is available for downloading on [http://cgem.stanford.edu our website].</div></td></tr>
<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;"></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 style="color: red; font-weight: bold; text-decoration: none;">== References ==</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 style="color: red; font-weight: bold; text-decoration: none;"></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 style="color: red; font-weight: bold; text-decoration: none;">[1] [http://cdsads.u-strasbg.fr/abs/2010ApJ...715..242F Fisher et al. (2010)]</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 style="color: red; font-weight: bold; text-decoration: none;"></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 style="color: red; font-weight: bold; text-decoration: none;">[2] [http://cdsads.u-strasbg.fr/abs/2014ApJ...795...17K Kazachenko et al. 2014]</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 style="color: red; font-weight: bold; text-decoration: none;"></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 style="color: red; font-weight: bold; text-decoration: none;"> [http://cdsads.u-strasbg.fr/abs/2015SpWea..13..369F Fisher et al. 2015], [http://cdsads.u-strasbg.fr/abs/2015arXiv150505974K Kazachenko et al. 2015])</ins></div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8401&oldid=prevMariaKazachenko at 22:24, 9 September 20152015-09-09T22:24:01Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Introduction ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Introduction ==</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 advent of high-cadence vector magnetic field and Doppler velocity measurements from e.g. [http://hmi.stanford.edu/ HMI/SDO], [http://sot.lmsal.com/ SOT/Hinode] and [http://solis.nso.edu/0/index.html SOLIS], have made the estimation of electric fields in the solar photosphere possible. The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. ''First,'' if we know both electric and magnetic field vectors in the photosphere, we can estimate both the Poynting flux of magnetic energy and the flux of relative magnetic helicity entering the corona. ''Second,'' knowledge of electric and magnetic fields enables the driving of time-dependent simulations of the coronal magnetic field. This is the goal of the Coronal Global Evolutionary Model ([http://cgem.stanford.edu CGEM], [http://cdsads.u-strasbg.fr/abs/2015SpWea..13..369F Fisher et al. 2015]).</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The advent of high-cadence vector magnetic field and Doppler velocity measurements from e.g. [http://hmi.stanford.edu/ HMI/SDO], [http://sot.lmsal.com/ SOT/Hinode] and [http://solis.nso.edu/0/index.html SOLIS], have made the estimation of electric fields in the solar photosphere possible. The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. ''First,'' if we know both electric and magnetic field vectors in the photosphere, we can estimate both the Poynting flux of magnetic energy and the flux of relative magnetic helicity entering the corona. ''Second,'' knowledge of electric and magnetic fields enables the driving of time-dependent simulations of the coronal magnetic field. This is the goal of the Coronal Global Evolutionary Model ([http://cgem.stanford.edu CGEM], [http://cdsads.u-strasbg.fr/abs/2015SpWea..13..369F Fisher <ins class="diffchange diffchange-inline">et al. 2015], [http://cdsads.u-strasbg.fr/abs/2015arXiv150505974K Kazachenko </ins>et al. 2015]).</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Method ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Method ==</div></td></tr>
</table>MariaKazachenkohttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Photospheric_Electric_Fields_and_Energy_Fluxes_in_the_Eruptive_Active_Region_NOAA_11158&diff=8400&oldid=prevMariaKazachenko at 22:16, 9 September 20152015-09-09T22:16:43Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Conclusion ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Conclusion ==</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>This study is the first application of the PDFI electric field inversion technique to photospheric vector magnetic field and Doppler measurements. We find that the total amount of energy injected through the photosphere before the flare estimated by the PDFI method is consistent with estimates from other approaches, in spite of differing techniques. This agreement is very promising, implying that the PDFI technique is not only capable of describing the coronal energy and helicity budget, but can also provide instantaneous estimates of energy and helicity transferred through the photosphere. We believe that both the derived dataset of PDFI electric fields and the PDFI method itself will be useful to the science community for analysis of the evolution and spatial distribution of the photospheric electric fields, fluxes of energy and helicity, and their relationships with flare activity. In addition, PDFI electric fields can be used as time-dependent boundary conditions for data-driven models of coronal magnetic field evolution. The dataset <del class="diffchange diffchange-inline">for </del>NOAA 11158 is available for downloading on [http://cgem.stanford.edu our website].</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This study is the first application of the PDFI electric field inversion technique to photospheric vector magnetic field and Doppler measurements. We find that the total amount of energy injected through the photosphere before the flare estimated by the PDFI method is consistent with estimates from other approaches, in spite of differing techniques. This agreement is very promising, implying that the PDFI technique is not only capable of describing the coronal energy and helicity budget, but can also provide instantaneous estimates of energy and helicity transferred through the photosphere. We believe that both the derived dataset of PDFI electric fields and the PDFI method itself will be useful to the science community for analysis of the evolution and spatial distribution of the photospheric electric fields, fluxes of energy and helicity, and their relationships with flare activity. In addition, PDFI electric fields can be used as time-dependent boundary conditions for data-driven models of coronal magnetic field evolution. The dataset <ins class="diffchange diffchange-inline">of magnetic and electric fields and Poynting fluxes in </ins>NOAA 11158 is available for downloading on [http://cgem.stanford.edu our website].</div></td></tr>
</table>MariaKazachenko