https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&feed=atom&action=historyCORONAS/SPIRIT Mg XII and Nanoflares - Revision history2024-03-29T15:01:07ZRevision history for this page on the wikiMediaWiki 1.16.0https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11306&oldid=prevSchriste at 20:14, 7 December 20182018-12-07T20:14:24Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 22 October 2018</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 22 October 2018</div></td></tr>
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</table>Schristehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11268&oldid=prevHhudson at 08:34, 18 November 20182018-11-18T08:34:12Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 22 October 2018</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 22 October 2018</div></td></tr>
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</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11267&oldid=prevHhudson at 08:33, 18 November 20182018-11-18T08:33:28Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|title = CORONAS/SPIRIT Mg XII and nanoflares </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|title = CORONAS/SPIRIT Mg XII and nanoflares </div></td></tr>
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</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11241&oldid=prevHhudson: /* References */2018-10-26T15:43:37Z<p><span class="autocomment">References</span></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[5] [http://adsabs.harvard.edu/abs/2014ApJ...784...49C "Active Region Emission Measure Distributions and Implications for Nanoflare Heating"]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[5] [http://adsabs.harvard.edu/abs/2014ApJ...784...49C "Active Region Emission Measure Distributions and Implications for Nanoflare Heating"]</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] [http://<del class="diffchange diffchange-inline">sprg</del>.<del class="diffchange diffchange-inline">ssl.berkeley</del>.edu/<del class="diffchange diffchange-inline">~tohban</del>/<del class="diffchange diffchange-inline">wiki/index</del>.<del class="diffchange diffchange-inline">php/CORONAS/SPIRIT_Mg_XII_and_Nanoflares </del>"Estimate of the Upper Limit on Hot Plasma Differential Emission Measure (DEM) in Non-Flaring Active Regions and Nanoflare Frequency Based on the Mg xii Spectroheliograph Data from CORONAS-F/SPIRIT"]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[6] [http://<ins class="diffchange diffchange-inline">adsabs</ins>.<ins class="diffchange diffchange-inline">harvard</ins>.edu/<ins class="diffchange diffchange-inline">cgi-bin</ins>/<ins class="diffchange diffchange-inline">bib_query?arXiv:1810</ins>.<ins class="diffchange diffchange-inline">04952 </ins>"Estimate of the Upper Limit on Hot Plasma Differential Emission Measure (DEM) in Non-Flaring Active Regions and Nanoflare Frequency Based on the Mg xii Spectroheliograph Data from CORONAS-F/SPIRIT"]</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11238&oldid=prevHhudson: /* Results */ links2018-10-23T19:34:06Z<p><span class="autocomment">Results: </span> links</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>To estimate the relative amount of the hot and warm (main temperature</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>To estimate the relative amount of the hot and warm (main temperature</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>component) plasma, we reconstructed the DEM of the non-flaring</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>component) plasma, we reconstructed the DEM of the non-flaring</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>active region NOAA 09833 (see Figure 2). We extracted the fluxes</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>active region <ins class="diffchange diffchange-inline">[https://www.solarmonitor.org/index.php?date=20020220&region=09833&indexnum=1 </ins>NOAA 09833<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>(see Figure 2). </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>We extracted the fluxes</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>of the selected active region from the Mg XII, EIT 171 &Acirc;, 195 &Acirc;, and</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>of the selected active region from the Mg XII, EIT 171 &Acirc;, 195 &Acirc;, and</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>284 &Acirc; channels. Using these four fluxes, we reconstructed the DEM</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>284 &Acirc; channels. Using these four fluxes, we reconstructed the DEM</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11237&oldid=prevHhudson: /* Introduction */ links2018-10-23T19:28:14Z<p><span class="autocomment">Introduction: </span> links</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>It is hard to find faint hot-plasma emission with conventional</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>It is hard to find faint hot-plasma emission with conventional</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>non-monochromatic imagers (like AIA or XRT), because their images</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>non-monochromatic imagers (like <ins class="diffchange diffchange-inline">[https://aia.lmsal.com </ins>AIA<ins class="diffchange diffchange-inline">] </ins>or <ins class="diffchange diffchange-inline">[https://xrt.cfa.harvard.edu </ins>XRT<ins class="diffchange diffchange-inline">]</ins>), because their images</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>contain broad temperature contributions. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>contain broad temperature contributions. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This Nugget describes an upper limit on the hot-plasma DEM using </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This Nugget describes an upper limit on the hot-plasma DEM using </div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11236&oldid=prevHhudson: more fixes2018-10-23T19:25:07Z<p>more fixes</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:335f2.png|600px|thumb|center|Figure 2:</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:335f2.png|600px|thumb|center|Figure 2:</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Non-flaring active region NOAA 09833, which was used to determine</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Non-flaring active region NOAA 09833, which was used to determine</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>the DEM. a) EIT 171&Acirc; image; b) EIT 195&Acirc; image; </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>the DEM. a) EIT 171 &Acirc; image; b) EIT 195 &Acirc; image; </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>c) EIT 284 &Acirc; image.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>c) EIT 284 &Acirc; image.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>d) Spectroheliograph Mg XII image. The rectangle marks the active</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>d) Spectroheliograph Mg XII image. The rectangle marks the active</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Figure 4 shows that the relative amount of hot plasma rapidly</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Figure 4 shows that the relative amount of hot plasma rapidly</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>diminishes with the decrease of the delay between nanoflares. The</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>diminishes with the decrease of the delay between nanoflares. The</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Mg XII data show that this ratio should be lower than <del class="diffchange diffchange-inline">104</del>. Therefore,</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Mg XII data show that this ratio should be lower than <ins class="diffchange diffchange-inline">0.0001</ins>. Therefore,</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the delay between the nanoflares should be shorter than 500 seconds.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the delay between the nanoflares should be shorter than 500 seconds.</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>[[File:335f4.png|600px|thumb|center|Figure 4: The</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:335f4.png|600px|thumb|center|Figure 4: The</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>ratio of DEM10 to the DEM<sub>max</sub> as a function of the average</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>ratio of DEM10 to the DEM<sub>max</sub> as a function of the average</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>time between nanoflares <del class="diffchange diffchange-inline">[N]</del>. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>time between nanoflares. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The data were taken from the simulations of Ref. [5].</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The data were taken from the simulations of Ref. [5].</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The black line denotes the simulations where nanoflares have power-law </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The black line denotes the simulations where nanoflares have power-law </div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>"smoking gun" signature expected for nanoflare heating. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>"smoking gun" signature expected for nanoflare heating. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Because the instrument is uniquely monochromatic, and because of the extent of the data, these constraints are the most direct ones yet published.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Because the instrument is uniquely monochromatic, and because of the extent of the data, these constraints are the most direct ones yet published.</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;">The details of this analysis appear in Ref. [6].</ins></div></td></tr>
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<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>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[5] [http://adsabs.harvard.edu/abs/2014ApJ...784...49C "Active Region Emission Measure Distributions and Implications for Nanoflare Heating"]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[5] [http://adsabs.harvard.edu/abs/2014ApJ...784...49C "Active Region Emission Measure Distributions and Implications for Nanoflare Heating"]</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;">[6] [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/CORONAS/SPIRIT_Mg_XII_and_Nanoflares "Estimate of the Upper Limit on Hot Plasma Differential Emission Measure (DEM) in Non-Flaring Active Regions and Nanoflare Frequency Based on the Mg xii Spectroheliograph Data from CORONAS-F/SPIRIT"]</ins></div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11235&oldid=prevHhudson: some fixes2018-10-23T19:20:12Z<p>some fixes</p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
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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 19:20, 23 October 2018</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 46:</td>
<td colspan="2" class="diff-lineno">Line 46:</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 Mg XII spectroheliograph obtained monochromatic images of the</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The Mg XII spectroheliograph obtained monochromatic images of the</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>solar corona in the Mg XII 8.42&Acirc; line. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>solar corona in the Mg XII 8.42 &Acirc; line. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>This line emits mainly at temperatures higher than <del class="diffchange diffchange-inline">4MK</del>. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This line emits mainly at temperatures higher than <ins class="diffchange diffchange-inline">4 MK</ins>. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The Mg XII images do not contain a solar limb (hence no contribution</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The Mg XII images do not contain a solar limb (hence no contribution</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>from the general corona) or any other low-temperature background.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>from the general corona) or any other low-temperature background.</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 66:</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>These are produced during flares or sequences of</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>These are produced during flares or sequences of</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>microflares. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>microflares. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Their X-ray emission is highly variable <del class="diffchange diffchange-inline">(see Figure 3)</del>. After the flare ended, these large structures faded away.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Their X-ray emission is highly variable. After the flare ended, these large structures faded away.</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>[[File:335f1.png|600px|thumb|center|Figure 1:</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:335f1.png|600px|thumb|center|Figure 1:</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 84:</td>
<td colspan="2" class="diff-lineno">Line 84:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>component) plasma, we reconstructed the DEM of the non-flaring</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>component) plasma, we reconstructed the DEM of the non-flaring</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>active region NOAA 09833 (see Figure 2). We extracted the fluxes</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>active region NOAA 09833 (see Figure 2). We extracted the fluxes</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>of the selected active region from the Mg XII, EIT 171, 195, and</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>of the selected active region from the Mg XII, EIT 171 <ins class="diffchange diffchange-inline">&Acirc;</ins>, 195 <ins class="diffchange diffchange-inline">&Acirc;</ins>, and</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>284 <del class="diffchange diffchange-inline"> </del>channels. Using these four fluxes, we reconstructed the DEM</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>284 <ins class="diffchange diffchange-inline">&Acirc; </ins>channels. Using these four fluxes, we reconstructed the DEM</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>with a genetic algorithm.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>with a genetic algorithm.</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 91:</td>
<td colspan="2" class="diff-lineno">Line 91:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Non-flaring active region NOAA 09833, which was used to determine</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Non-flaring active region NOAA 09833, which was used to determine</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the DEM. a) EIT 171&Acirc; image; b) EIT 195&Acirc; image; </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the DEM. a) EIT 171&Acirc; image; b) EIT 195&Acirc; image; </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>c) EIT 284&Acirc; image.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>c) EIT 284 &Acirc; image.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>d) Spectroheliograph Mg XII image. The rectangle marks the active</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>d) Spectroheliograph Mg XII image. The rectangle marks the active</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>region that was used for DEM measurements</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>region that was used for DEM measurements</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 105:</td>
<td colspan="2" class="diff-lineno">Line 105:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Red shows the DEMs obtained during different runs of a genetic</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Red shows the DEMs obtained during different runs of a genetic</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>algorithm, and black represents their median. The blue-dashdotted</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>algorithm, and black represents their median. The blue-dashdotted</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>DEM-loci show EIT 171&Acirc;, green-dotted DEM-loci are EIT 195&Acirc;, </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>DEM-loci show EIT 171 &Acirc;, green-dotted DEM-loci are EIT 195 &Acirc;, </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>red-dashed DEM-loci show EIT 284&Acirc;, and purple-solid DEM-loci represent </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>red-dashed DEM-loci show EIT 284 &Acirc;, and purple-solid DEM-loci represent </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the Mg XII spectroheliograph.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the Mg XII spectroheliograph.</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 colspan="2" class="diff-lineno">Line 126:</td>
<td colspan="2" class="diff-lineno">Line 126:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the simulations provide DEMs. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>the simulations provide DEMs. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>For each of these plots, we manually measured the ratio of the DEM at</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>For each of these plots, we manually measured the ratio of the DEM at</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>10 MK (DEM10) to the DEM of the main temperature component (<del class="diffchange diffchange-inline">DEMmax</del>).</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>10 MK (DEM10) to the DEM of the main temperature component (<ins class="diffchange diffchange-inline">DEM<sub>max</sub></ins>).</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Then we used the obtained values to build a plot of how this ratio</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Then we used the obtained values to build a plot of how this ratio</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>depends on the delay between the nanoflares (see Figure 4).</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>depends on the delay between the nanoflares (see Figure 4).</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 136:</td>
<td colspan="2" class="diff-lineno">Line 136:</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>[[File:335f4.png|600px|thumb|center|Figure 4: The</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:335f4.png|600px|thumb|center|Figure 4: The</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>ratio of DEM10 to the <del class="diffchange diffchange-inline">DEMmax </del>as a function of the average</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>ratio of DEM10 to the <ins class="diffchange diffchange-inline">DEM<sub>max</sub> </ins>as a function of the average</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>time between nanoflares [N]. The data were taken from the simulations </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>time between nanoflares [N]. </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>of Ref. [5].</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The data were taken from the simulations of Ref. [5].</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The black line denotes the simulations where nanoflares have power-law </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The black line denotes the simulations where nanoflares have power-law </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>energy distribution with a slope m = -2.5 and the delay between </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>energy distribution with a slope m = -2.5 and the delay between </div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11234&oldid=prevHhudson: /* Conclusions */ draft2018-10-23T11:05:14Z<p><span class="autocomment">Conclusions: </span> draft</p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
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<col class='diff-marker' />
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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 11:05, 23 October 2018</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 152:</td>
<td colspan="2" class="diff-lineno">Line 152:</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>== Conclusions ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== Conclusions ==</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;">The CORONAS-F/SPIRIT data constrain the high-temperature DEM levels in the solar corona, and do not find any evidence for 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 style="color: red; font-weight: bold; text-decoration: none;">"smoking gun" signature expected for nanoflare heating. </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;">Because the instrument is uniquely monochromatic, and because of the extent of the data, these constraints are the most direct ones yet published.</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== References ==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>== References ==</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=CORONAS/SPIRIT_Mg_XII_and_Nanoflares&diff=11233&oldid=prevHhudson: initial upload of 3352018-10-23T10:56:31Z<p>initial upload of 335</p>
<p><b>New page</b></p><div>{{Infobox Nugget<br />
|name = Nugget<br />
|title = CORONAS/SPIRIT Mg XII and nanoflares <br />
|number = 33j<br />
|first_author = Anton Reva <br />
|second_author = <br />
|publish_date = 22 October 2018<br />
|next_nugget = TBD <br />
|previous_nugget={{#ask: [[Category:Nugget]] [[RHESSI Nugget Index::334]]}}<br />
}}<br />
<br />
== Introduction ==<br />
<br />
The high temperature of the solar corona has several possible explanations,<br />
and correspondingly intense theoretical and observational work trying <br />
to identify the right one(s).<br />
In nanoflare heating theory, the corona is heated by a large number of<br />
small-scale flare-like events (nanoflares). <br />
If the nanoflare frequency is low, then some hot plasma should always exist <br />
in non-flaring active regions, since the apparently steady emission<br />
would reflect the lower average temperature of the nanoflare events.<br />
The detection of hot plasma in non-flaring active regions would therefore be<br />
indirect evidence of low-frequency nanoflare heating (a <br />
[https://en.wikipedia.org/wiki/Chekhov%27s_gun "smoking gun"]). <br />
The absence of the hot emission can help to constrain the nanoflare frequency.<br />
The breadth of the distribution of emission measure if it is not<br />
isothermal, i.e. the "differential emission measure" (DEM), thus reflects<br />
the presence or absence of nanoflares.<br />
<br />
It is hard to find faint hot-plasma emission with conventional<br />
non-monochromatic imagers (like AIA or XRT), because their images<br />
contain broad temperature contributions. <br />
This Nugget describes an upper limit on the hot-plasma DEM using <br />
direct observations of the hot plasma by the Mg XII spectroheliograph <br />
SPIRIT (Ref. [1]) onboard the<br />
[https://space.skyrocket.de/doc_sdat/koronas-foton.htm CORONAS-F]<br />
satellite observatory.<br />
This instrument imaged coronal hot plasma without any low-temperature <br />
background contamination. <br />
We compare the obtained limit<br />
with the result of recent numerical simulations and aim to place<br />
constraints on the parameters of the nanoflare-heating model <br />
(Refs. [2,3]).<br />
<br />
== Experimental Data ==<br />
<br />
The Mg XII spectroheliograph obtained monochromatic images of the<br />
solar corona in the Mg XII 8.42&Acirc; line. <br />
This line emits mainly at temperatures higher than 4MK. <br />
The Mg XII images do not contain a solar limb (hence no contribution<br />
from the general corona) or any other low-temperature background.<br />
<br />
We studied the period from 18-28 February 2002. At this time, the<br />
Mg XII spectroheliograph worked with a 105-second cadence almost<br />
without data gaps. In these observations, the Mg XII spectroheliograph<br />
registered binned images with a spatial resolution of 8 arc seconds<br />
and a 37-second exposure time.<br />
<br />
== Results ==<br />
<br />
The Mg XII data (Figure 1) shows that only two types of hot objects<br />
were present on the Sun: the first are small isolated flare-like<br />
phenomena (Ref. [4]). During the period of observations, they occurred at<br />
a rate of about 20 per day. <br />
The second are large hot structures inside active regions. <br />
These are produced during flares or sequences of<br />
microflares. <br />
Their X-ray emission is highly variable (see Figure 3). After the flare ended, these large structures faded away.<br />
<br />
[[File:335f1.png|600px|thumb|center|Figure 1:<br />
Hot plasma observed by the Mg XII spectroheliograph.<br />
Left: EIT image. Right: Mg XII spectroheliograph image (blue and<br />
green correspond to low intensities, red and yellow to high<br />
intensities). 1) Small flare-like objects. 2) Flaring active region<br />
with hot plasma. 3) Non-flaring active region without hot plasma.<br />
]]<br />
<br />
Except for rare microflares, there was no hot plasma in non-flaring<br />
active regions. Below we discuss this fact and try to estimate the<br />
upper limit of the hot-plasma emission measure and nanoflare<br />
frequency, which may be consistent with this lack of signal.<br />
<br />
To estimate the relative amount of the hot and warm (main temperature<br />
component) plasma, we reconstructed the DEM of the non-flaring<br />
active region NOAA 09833 (see Figure 2). We extracted the fluxes<br />
of the selected active region from the Mg XII, EIT 171, 195, and<br />
284 channels. Using these four fluxes, we reconstructed the DEM<br />
with a genetic algorithm.<br />
<br />
[[File:335f2.png|600px|thumb|center|Figure 2:<br />
Non-flaring active region NOAA 09833, which was used to determine<br />
the DEM. a) EIT 171&Acirc; image; b) EIT 195&Acirc; image; <br />
c) EIT 284&Acirc; image.<br />
d) Spectroheliograph Mg XII image. The rectangle marks the active<br />
region that was used for DEM measurements<br />
]]<br />
<br />
The amount of plasma with T =5 MK (logT = 6.7) is four orders of<br />
magnitude lower than the main temperature component, and the amount<br />
of plasma with T = 10 MK is four to five orders lower (see Figure<br />
3).<br />
<br />
[[File:335f3.png|600px|thumb|center|Figure 3: The<br />
DEM of the non-flaring active region marked in Figure 2.<br />
Red shows the DEMs obtained during different runs of a genetic<br />
algorithm, and black represents their median. The blue-dashdotted<br />
DEM-loci show EIT 171&Acirc;, green-dotted DEM-loci are EIT 195&Acirc;, <br />
red-dashed DEM-loci show EIT 284&Acirc;, and purple-solid DEM-loci represent <br />
the Mg XII spectroheliograph.<br />
]]<br />
<br />
At log T > 7.0, only the Mg XII flux constrains the DEM. The DEM<br />
in Figure 3 at log T > 7.0 shows the values that could be added to<br />
the DEM without increasing the Mg XII flux to a level greater than<br />
the noise. These values are the DEM upper limit.<br />
<br />
== Comparison with Simulations ==<br />
<br />
Numerical simulations (Ref. [5]) show how a coronal<br />
loop should react to the sequence of nanoflares depending on the<br />
nanoflare frequency. <br />
The author found that for a low nanoflare frequency, the DEM has a <br />
hot component. <br />
The hot component vanishes for a high nanoflare frequency.<br />
For each different regimes and for different delays between nanoflares,<br />
the simulations provide DEMs. <br />
For each of these plots, we manually measured the ratio of the DEM at<br />
10 MK (DEM10) to the DEM of the main temperature component (DEMmax).<br />
Then we used the obtained values to build a plot of how this ratio<br />
depends on the delay between the nanoflares (see Figure 4).<br />
<br />
Figure 4 shows that the relative amount of hot plasma rapidly<br />
diminishes with the decrease of the delay between nanoflares. The<br />
Mg XII data show that this ratio should be lower than 104. Therefore,<br />
the delay between the nanoflares should be shorter than 500 seconds.<br />
<br />
[[File:335f4.png|600px|thumb|center|Figure 4: The<br />
ratio of DEM10 to the DEMmax as a function of the average<br />
time between nanoflares [N]. The data were taken from the simulations <br />
of Ref. [5].<br />
The black line denotes the simulations where nanoflares have power-law <br />
energy distribution with a slope m = -2.5 and the delay between <br />
nanoflares is proportional to their energy. <br />
The red line denotes the simulations where nanoflares have<br />
a power-law energy distribution with a slope m = -1.5 and the delay<br />
between nanoflares is proportional to their energy. The blue line<br />
denotes the simulations where nanoflares have a power-law energy<br />
distribution with a slope m = -2.5 and the delay between nanoflares<br />
is fixed. The purple line denotes the Mg XII upper limit on the<br />
ratio of the DEMs of the hot and warm components.<br />
]]<br />
<br />
== Conclusions ==<br />
<br />
== References ==<br />
<br />
[1] [http://adsabs.harvard.edu/abs/2003MNRAS.338...67Z "Dynamic 10 MK plasma structures observed in monochromatic full-Sun images by the SPIRIT spectroheliograph on the CORONAS-F mission"]]<br />
<br />
[2] [http://adsabs.harvard.edu/abs/2002AstL...28..401O "Comprehensive Studies of Solar Activity on the CORONAS-F Satellite"]<br />
<br />
[3] [http://adsabs.harvard.edu/abs/2002ESASP.506..915Z "SPIRIT X-ray telescope/spectroheliometer results"]<br />
<br />
[4] [http://adsabs.harvard.edu/abs/2012SoPh..276...97R "Investigation of Hot X-Ray Points (HXPs) Using Spectroheliograph Mg xii Experiment Data from CORONAS-F/SPIRIT"]<br />
<br />
[5] [http://adsabs.harvard.edu/abs/2014ApJ...784...49C "Active Region Emission Measure Distributions and Implications for Nanoflare Heating"]</div>Hhudson