https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&feed=atom&action=historyMulti-Instrument Solar Flare Observations II: A SC24 retrospective - Revision history2024-03-28T22:48:03ZRevision history for this page on the wikiMediaWiki 1.16.0https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=10778&oldid=prevSchriste at 18:59, 22 August 20182018-08-22T18:59:23Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Jack Ireland</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Jack Ireland</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 10 April 2017</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 10 April 2017</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|next_nugget = <del class="diffchange diffchange-inline">White-light flares</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|next_nugget=<ins class="diffchange diffchange-inline">{{#ask: [[Category:Nugget]] [[RHESSI Nugget Index::299]]}}</ins></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|previous_nugget = [<del class="diffchange diffchange-inline">http</del>:<del class="diffchange diffchange-inline">//sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Multi-Instrument_Solar_Flare_Observations_I</del>:<del class="diffchange diffchange-inline">_Solar_Flare_Finder Multi-Instrument I</del>]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|previous_nugget=<ins class="diffchange diffchange-inline">{{#ask: </ins>[<ins class="diffchange diffchange-inline">[Category</ins>:<ins class="diffchange diffchange-inline">Nugget]] [[RHESSI Nugget Index</ins>:<ins class="diffchange diffchange-inline">:297]</ins>]<ins class="diffchange diffchange-inline">}}</ins></div></td></tr>
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</table>Schristehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9695&oldid=prevHhudson at 07:59, 28 April 20172017-04-28T07:59:45Z<p></p>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|next_nugget = <del class="diffchange diffchange-inline">The thrill of solar minimum</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|next_nugget = <ins class="diffchange diffchange-inline">White-light flares</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Multi-Instrument_Solar_Flare_Observations_I:_Solar_Flare_Finder Multi-Instrument I]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Multi-Instrument_Solar_Flare_Observations_I:_Solar_Flare_Finder Multi-Instrument I]</div></td></tr>
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</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9660&oldid=prevHhudson at 15:37, 10 April 20172017-04-10T15:37:49Z<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>Using the search capabilities of the <del class="diffchange diffchange-inline">]</del>http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Multi-Instrument_Solar_Flare_Observations_I:_Solar_Flare_Finder Solar Flare Finder widget] outlined last week, we can now do a retrospective analysis to see how effective our coordinated observations - either planned or serendipitous - have been during Solar Cycle 24. We consider the first 6.5 years after SDO was launched (1 May 2010<del class="diffchange diffchange-inline">-</del>31 Oct 2016), which encompasses the peak of Solar Cycle 24 as shown by the vertical dotted lines in Figure 1. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Using the search capabilities of the <ins class="diffchange diffchange-inline">[</ins>http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Multi-Instrument_Solar_Flare_Observations_I:_Solar_Flare_Finder Solar Flare Finder widget] outlined last week, we can now do a retrospective analysis to see how effective our coordinated observations - either planned or serendipitous - have been during </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/Solar_cycle_24 </ins>Solar Cycle 24<ins class="diffchange diffchange-inline">]</ins>. We consider the first 6.5 years after <ins class="diffchange diffchange-inline">[https://sdo.gsfc.nasa.gov </ins>SDO<ins class="diffchange diffchange-inline">] </ins>was launched (1 May 2010 <ins class="diffchange diffchange-inline">to </ins>31 Oct 2016), which encompasses the peak of Solar Cycle 24 as shown by the vertical dotted lines in Figure 1. </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:solar_cycle_monthly_ssn.png|600px|thumb|center|Figure 1: Plot of Solar Cycles 23 and 24 (average monthly sunspot number) with mission durations overplotted. The two vertical dotted lines denote the 6.5 year time range considered for this study. Note that SDO/EVE MEGS-A and IRIS only overlapped for ~11 months.]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[File:solar_cycle_monthly_ssn.png|600px|thumb|center|Figure 1: Plot of Solar Cycles <ins class="diffchange diffchange-inline">[https://en.wikipedia.org/wiki/Solar_cycle_23 </ins>23<ins class="diffchange diffchange-inline">] </ins>and </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/Solar_cycle_24 </ins>24<ins class="diffchange diffchange-inline">] </ins>(average monthly sunspot number) with mission durations overplotted. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The two vertical dotted lines denote the 6.5 year time range considered for this study. Note that </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://lasp.colorado.edu/home/missions-projects/quick-facts-sdo-eve/ </ins>SDO/EVE MEGS-A<ins class="diffchange diffchange-inline">] </ins>and </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://iris.lmsal.com </ins>IRIS<ins class="diffchange diffchange-inline">] </ins>only overlapped for ~11 months.]]</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Statistics==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Statistics==</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>First we shall take a look at how instruments performed individually. Table 1 shows the breakdown of flares listed in the SSW Latest Events catalog (by class) observed by each instrument. Note that MEGS-A had a 100% duty cycle up until 26 May 2014 when it suffered a power anomaly. Similarly, IRIS was only launched on 27 June 2013 so only flares after this date (in parentheses) were considered.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>First we shall take a look at how instruments performed individually. Table 1 shows the breakdown of flares listed in the </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[http://www.lmsal.com/solarsoft/last_events/ </ins>SSW Latest Events<ins class="diffchange diffchange-inline">] </ins>catalog (by class) observed by each instrument. Note that MEGS-A had a 100% duty cycle up until 26 May 2014 when it suffered a power anomaly. Similarly, IRIS was only launched on 27 June 2013 so only flares after this date (in parentheses) were considered.</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==UpSetR plots==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==UpSetR plots==</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 help visualize these relationships we have used UpSet (Ref 1), a novel tool for visualizing intersecting datasets. This type of plot enables the efficient visualization the common elements of a large number of sets (the more common and familiar Venn diagram approach produces ineffective visualizations). The left hand panel of Figure 2 shows the intersections of the various combinations of dataset ordered by decreasing frequency (i.e. the most common combinations are on the left and decrease towards the right). The right hand panel shows the same information <del class="diffchange diffchange-inline">only </del>now ordered by increasing degree (i.e. flares observed by individual instruments alone come first, with flares observed by all seven on the far right). In each figure, the total number of flares observed by each instrument are given by the horizontal black bars in the bottom left corner. The dots connected by lines at the bottom of each figure denote the combinations of instruments considered, while the histograms above give the number of events corresponding to a given combination. The most common combination of flare datasets was RHESSI+MEGS-A+Hinode/XRT (930 flares), due to their large fields of view and high duty cycles, while only 3 flares out of 934 were simultaneously observed by all 7 instruments.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>To help visualize these relationships we have used UpSet (Ref <ins class="diffchange diffchange-inline">[</ins>1<ins class="diffchange diffchange-inline">]</ins>), a novel tool for visualizing intersecting datasets. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>This type of plot enables the efficient visualization the common elements of a large number of sets (the more common and <ins class="diffchange diffchange-inline">the </ins>familiar </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/Venn_diagram </ins>Venn diagram<ins class="diffchange diffchange-inline">] </ins>approach produces ineffective visualizations). </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The left<ins class="diffchange diffchange-inline">-</ins>hand panel of Figure 2 shows the intersections of the various combinations of dataset ordered by decreasing frequency (i.e. the most common combinations are on the left and decrease towards the right). </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The right<ins class="diffchange diffchange-inline">-</ins>hand panel shows the same information <ins class="diffchange diffchange-inline">but </ins>now ordered by increasing degree (i.e. flares observed by individual instruments alone come first, with flares observed by all seven on the far right). </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>In each figure, the total number of flares observed by each instrument are given by the horizontal black bars in the bottom left corner. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The dots connected by lines at the bottom of each figure denote the combinations of instruments considered, while the histograms above give the number of events corresponding to a given combination. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The most common combination of flare datasets was RHESSI+MEGS-A+Hinode/XRT (930 flares), due to their large fields of view and high duty cycles, while only 3 flares out of 934 were simultaneously observed by all 7 instruments.</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:Upsetr_merged.png|1200px|thumb|center|Figure 2: UpSet plots of the intersection of flare datasets from each instrument as ordered by decreasing frequency (left) and increasing degree (right; zero elements sets not included).]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:Upsetr_merged.png|1200px|thumb|center|Figure 2: UpSet plots of the intersection of flare datasets from each instrument as ordered by decreasing frequency (left) and increasing degree (right; zero elements sets not included).]]</div></td></tr>
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<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 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 paucity of events co-observed by multiple, complementary instruments points to the challenge of observing solar flares ''in <del class="diffchange diffchange-inline">flagrente </del>delicto''. Without a reliable method of predicting when and where a solar flare will occur, we are left with trying to optimize instrumental resources in the face of incomplete information as well as each instruments' operational constraints and competing scientific priorities. This is worth bearing in mind as we approach Solar Cycle 25, and the advent of the Daniel K. Inoue Solar Telescope, Solar Orbiter and Solar Probe Plus.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The paucity of events co-observed by multiple, complementary instruments points to the challenge of observing solar flares ''in <ins class="diffchange diffchange-inline">flagrante </ins>delicto''. Without a reliable method of predicting when and where a solar flare will occur, we are left with trying to optimize instrumental resources in the face of incomplete information as well as each instruments' operational constraints and competing scientific priorities. This is worth bearing in mind as we approach </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/Solar_cycle </ins>Solar Cycle 25<ins class="diffchange diffchange-inline">]</ins>, and the advent of <ins class="diffchange diffchange-inline">some powerful new facilities: </ins>the </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">[https://en.wikipedia.org/wiki/Daniel_Inouye </ins>Daniel K. Inoue<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">[http://dkist.nso.edu </ins>Solar Telescope<ins class="diffchange diffchange-inline">]</ins>, <ins class="diffchange diffchange-inline">[http://sci.esa.int/solar-orbiter/ </ins>Solar Orbiter<ins class="diffchange diffchange-inline">] </ins>and <ins class="diffchange diffchange-inline">[http://solarprobe.jhuapl.edu </ins>Solar Probe Plus<ins class="diffchange diffchange-inline">]</ins>.</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Biographical Note==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Biographical Note==</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9659&oldid=prevHhudson at 13:20, 10 April 20172017-04-10T13:20:41Z<p></p>
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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 = Multi-Instrument Solar Flare Observations I: Solar Flare Finder</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 = 298</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 = Ryan Milligan</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 = Jack Ireland</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 = 10 April 2017</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 = The thrill of solar minimum</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/Multi-Instrument_Solar_Flare_Observations_I:_Solar_Flare_Finder Multi-Instrument I]</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>Using the search capabilities of the Solar Flare Finder widget outlined <del class="diffchange diffchange-inline">in a previous nugget</del>, we can now do a retrospective analysis to see how effective our coordinated observations - either planned or serendipitous - have been during Solar Cycle 24. We consider the first 6.5 years after SDO was launched (1 May 2010-31 Oct 2016), which encompasses the peak of Solar Cycle 24 as shown by the vertical dotted lines in Figure 1. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Using the search capabilities of the <ins class="diffchange diffchange-inline">]http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Multi-Instrument_Solar_Flare_Observations_I:_Solar_Flare_Finder </ins>Solar Flare Finder widget<ins class="diffchange diffchange-inline">] </ins>outlined <ins class="diffchange diffchange-inline">last week</ins>, we can now do a retrospective analysis to see how effective our coordinated observations - either planned or serendipitous - have been during Solar Cycle 24. We consider the first 6.5 years after SDO was launched (1 May 2010-31 Oct 2016), which encompasses the peak of Solar Cycle 24 as shown by the vertical dotted lines in Figure 1. </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:solar_cycle_monthly_ssn.png|600px|thumb|center|Figure 1: Plot of Solar Cycles 23 and 24 (average monthly sunspot number) with mission durations overplotted. The two vertical dotted lines denote the 6.5 year time range considered for this study. Note that SDO/EVE MEGS-A and IRIS only overlapped for ~11 months.]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:solar_cycle_monthly_ssn.png|600px|thumb|center|Figure 1: Plot of Solar Cycles 23 and 24 (average monthly sunspot number) with mission durations overplotted. The two vertical dotted lines denote the 6.5 year time range considered for this study. Note that SDO/EVE MEGS-A and IRIS only overlapped for ~11 months.]]</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Statistics==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Statistics==</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>First we shall take a look at how <del class="diffchange diffchange-inline">instrument </del>performed individually. Table 1 shows the breakdown of flares listed in the SSW Latest Events catalog (by class) observed by each instrument. Note that MEGS-A had a 100% duty cycle up until 26 May 2014 when it suffered a power anomaly. Similarly, IRIS was only launched on 27 June 2013 so only flares after this date (in parentheses) were considered.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>First we shall take a look at how <ins class="diffchange diffchange-inline">instruments </ins>performed individually. Table 1 shows the breakdown of flares listed in the SSW Latest Events catalog (by class) observed by each instrument. Note that MEGS-A had a 100% duty cycle up until 26 May 2014 when it suffered a power anomaly. Similarly, IRIS was only launched on 27 June 2013 so only flares after this date (in parentheses) were considered.</div></td></tr>
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</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9633&oldid=prevRmilligan at 17:05, 22 March 20172017-03-22T17:05:19Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|| Instrument/Database || C-class || M-class || X-class || Total || Success Rate</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|| Instrument/Database || C-class || M-class || X-class || Total || Success Rate</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>! SSW Latest Events !! 6,339 !! 581 !! 33 !! 6,953 !! <del class="diffchange diffchange-inline">N</del>/<del class="diffchange diffchange-inline">A</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>! SSW Latest Events !! 6,339 !! 581 !! 33 !! 6,953 !! <ins class="diffchange diffchange-inline">86% of NOAA</ins>/<ins class="diffchange diffchange-inline">GOES events</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|-</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|-</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| RHESSI || 3,673 || 370 || 23 || 4,066 || 58%</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| RHESSI || 3,673 || 370 || 23 || 4,066 || 58%</div></td></tr>
</table>Rmilliganhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9632&oldid=prevHhudson at 15:25, 22 March 20172017-03-22T15:25:49Z<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 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>Using the search capabilities of the Solar Flare Finder widget outlined in a previous nugget, we can now do a retrospective analysis to see how effective our coordinated observations - either planned or serendipitous - have been during Solar Cycle 24. We consider the first 6.5 years after SDO was launched (1 May 2010-31 Oct 2016), which encompasses the peak of Solar Cycle 24 as shown by the vertical dotted lines in Figure 1. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Using the search capabilities of the Solar Flare Finder widget outlined in a previous nugget, we can now do a retrospective analysis to see how effective our coordinated observations - either planned or serendipitous - have been during Solar Cycle 24. We consider the first 6.5 years after SDO was launched (1 May 2010-31 Oct 2016), which encompasses the peak of Solar Cycle 24 as shown by the vertical dotted lines in Figure 1. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9596&oldid=prevRmilligan at 16:27, 8 March 20172017-03-08T16:27:31Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==UpSetR plots==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==UpSetR plots==</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>To help visualize these relationships we have used UpSet (Ref 1), a novel tool for visualizing intersecting datasets. This type of plot enables the efficient visualization the common elements of a large number of sets (the more common and familiar Venn diagram approach produces ineffective visualizations). The left hand panel of Figure 2 shows the intersections of the various combinations of dataset ordered by decreasing frequency (i.e. the most common combinations are on the left and decrease towards the right). The right hand panel shows the same information only now ordered by increasing degree (i.e. flares observed by individual instruments alone come first, with flares observed by all seven on the far right). In each figure, the total number of flares observed by each instrument are given by the horizontal black bars in the bottom left corner. The dots connected by lines at the bottom of each figure denote the combinations of instruments considered, while the histograms above give the number of events corresponding to a given combination. The most common combination of flare datasets was RHESSI+MEGS-A+Hinode/XRT (930 flares), due to their large fields of view and high duty cycles.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>To help visualize these relationships we have used UpSet (Ref 1), a novel tool for visualizing intersecting datasets. This type of plot enables the efficient visualization the common elements of a large number of sets (the more common and familiar Venn diagram approach produces ineffective visualizations). The left hand panel of Figure 2 shows the intersections of the various combinations of dataset ordered by decreasing frequency (i.e. the most common combinations are on the left and decrease towards the right). The right hand panel shows the same information only now ordered by increasing degree (i.e. flares observed by individual instruments alone come first, with flares observed by all seven on the far right). In each figure, the total number of flares observed by each instrument are given by the horizontal black bars in the bottom left corner. The dots connected by lines at the bottom of each figure denote the combinations of instruments considered, while the histograms above give the number of events corresponding to a given combination. The most common combination of flare datasets was RHESSI+MEGS-A+Hinode/XRT (930 flares), due to their large fields of view and high duty cycles<ins class="diffchange diffchange-inline">, while only 3 flares out of 934 were simultaneously observed by all 7 instruments</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>[[File:Upsetr_merged.png|1200px|thumb|center|Figure 2: UpSet plots of the intersection of flare datasets from each instrument as ordered by decreasing frequency (left) and increasing degree (right; zero elements sets not included).]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:Upsetr_merged.png|1200px|thumb|center|Figure 2: UpSet plots of the intersection of flare datasets from each instrument as ordered by decreasing frequency (left) and increasing degree (right; zero elements sets not included).]]</div></td></tr>
</table>Rmilliganhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9595&oldid=prevRmilligan at 16:25, 8 March 20172017-03-08T16:25:11Z<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: #ffa; color:black; font-size: smaller;"><div>Using the search capabilities <del class="diffchange diffchange-inline">outlines </del>in a previous nugget, we can now do a retrospective analysis to see how effective our coordinated observations - either planned or serendipitous - have been during Solar Cycle 24. We consider the first 6.5 years after SDO was launched (1 May 2010-31 Oct 2016), which encompasses the peak of Solar Cycle 24 <del class="diffchange diffchange-inline">(</del>vertical dotted lines in Figure 1<del class="diffchange diffchange-inline">)</del>. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Using the search capabilities <ins class="diffchange diffchange-inline">of the Solar Flare Finder widget outlined </ins>in a previous nugget, we can now do a retrospective analysis to see how effective our coordinated observations - either planned or serendipitous - have been during Solar Cycle 24. We consider the first 6.5 years after SDO was launched (1 May 2010-31 Oct 2016), which encompasses the peak of Solar Cycle 24 <ins class="diffchange diffchange-inline">as shown by the </ins>vertical dotted lines in Figure 1. </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:solar_cycle_monthly_ssn.png|600px|thumb|center|Figure 1: Plot of Solar Cycles 23 and 24 (average monthly sunspot number) with mission durations overplotted. The two vertical dotted lines denote the 6.5 year time range considered for this study. Note that SDO/EVE MEGS-A and IRIS only overlapped for ~11 months.]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:solar_cycle_monthly_ssn.png|600px|thumb|center|Figure 1: Plot of Solar Cycles 23 and 24 (average monthly sunspot number) with mission durations overplotted. The two vertical dotted lines denote the 6.5 year time range considered for this study. Note that SDO/EVE MEGS-A and IRIS only overlapped for ~11 months.]]</div></td></tr>
</table>Rmilliganhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9590&oldid=prevRmilligan at 10:53, 7 March 20172017-03-07T10:53:16Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>! SSW Latest Events !! 6,339 !! 581 !! 33 !! 6,953 !! N/A</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>! SSW Latest Events !! 6,339 !! 581 !! 33 !! 6,953 !! N/A</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|<del class="diffchange diffchange-inline">- </del>-</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>| RHESSI || 3,673 || 370 || 23 || 4,066 || 58%</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>| RHESSI || 3,673 || 370 || 23 || 4,066 || 58%</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">Now we look at </del>how many flares (of all classes) were observed by various combinations (degree) of instruments. Again note that all 7 instruments were only operational together for 11 months, and the number of flares duration this time are given in parentheses. From this we can calculate that - on average - each flare was observed by 2.4 instruments. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">Table 2 shows </ins>how many flares (of all classes) were observed by various combinations (degree) of instruments. Again note that all 7 instruments were only operational together for 11 months, and the number of flares duration this time are given in parentheses. From this we can calculate that - on average - each flare was observed by 2.4 instruments. </div></td></tr>
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</table>Rmilliganhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Multi-Instrument_Solar_Flare_Observations_II:_A_SC24_retrospective&diff=9589&oldid=prevRmilligan at 10:30, 7 March 20172017-03-07T10:30:32Z<p></p>
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<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>Now we look at how many flares (of all classes) were observed by various combinations (degree) of instruments. Again note that all 7 instruments were only operational together for 11 months, and the number of flares duration this time are given in parentheses. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Now we look at how many flares (of all classes) were observed by various combinations (degree) of instruments. Again note that all 7 instruments were only operational together for 11 months, and the number of flares duration this time are given in parentheses<ins class="diffchange diffchange-inline">. From this we can calculate that - on average - each flare was observed by 2.4 instruments</ins>. </div></td></tr>
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</table>Rmilligan