https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&feed=atom&action=historyEnergy Partition in Large Solar Eruptive Events - Revision history2024-03-29T14:23:09ZRevision history for this page on the wikiMediaWiki 1.16.0https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=10726&oldid=prevSchriste at 17:23, 22 August 20182018-08-22T17:23:00Z<p></p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 17:23, 22 August 2018</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 6:</td>
<td colspan="2" class="diff-lineno">Line 6:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Brian Dennis</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Brian Dennis</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 5 October 2012</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 5 October 2012</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">Temperature of Photosphere</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::186]]}}</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/New_TGFs_Found_in_the_RHESSI_Data Lightning</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::184]</ins>]<ins class="diffchange diffchange-inline">}}</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>}}</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>}}</div></td></tr>
<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>Schristehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5443&oldid=prevHhudson at 14:39, 19 October 20122012-10-19T14:39:51Z<p></p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 14:39, 19 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 6:</td>
<td colspan="2" class="diff-lineno">Line 6:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Brian Dennis</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = Brian Dennis</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 5 October 2012</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 5 October 2012</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|next_nugget = <del class="diffchange diffchange-inline">TBD</del></div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|next_nugget = <ins class="diffchange diffchange-inline">Temperature of Photosphere</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/New_TGFs_Found_in_the_RHESSI_Data Lightning]</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/New_TGFs_Found_in_the_RHESSI_Data Lightning]</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>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5440&oldid=prevHhudson: some links and one change2012-10-06T07:35:20Z<p>some links and one change</p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 07:35, 6 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 14:</td>
<td colspan="2" class="diff-lineno">Line 14:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Solar eruptive events (SEEs) consist of [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm flares] and their associated coronal mass ejections ([http://solarscience.msfc.nasa.gov/CMEs.shtml CMEs]). They are the most energetic transient events in the solar system. Over a period of tens of seconds to minutes, they can convert upwards of 10<sup>32</sup> ergs of energy stored in current-carrying magnetic fields into accelerated particles, heated [http://en.wikipedia.org/wiki/Plasma_(physics) plasma], and ejected solar material.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Solar eruptive events (SEEs) consist of [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm flares] and their associated coronal mass ejections ([http://solarscience.msfc.nasa.gov/CMEs.shtml CMEs]). They are the most energetic transient events in the solar system. Over a period of tens of seconds to minutes, they can convert upwards of 10<sup>32</sup> ergs of energy stored in current-carrying magnetic fields into accelerated particles, heated [http://en.wikipedia.org/wiki/Plasma_(physics) plasma], and ejected solar material.</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 partition of this released energy amongst these component parts has, until recently, been estimated for only a few events. In a paper to be published in the November 2012 issue of The Astrophysical Journal, observations of thirty-eight large solar eruptive events made with over a dozen different spacecraft instruments have been used to produce the first statistical analysis of the energy partition throughout the various manifestations of an SEE. The paper studied the energy content of eleven different manifestations, namely -</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The partition of this released energy amongst these component parts has, until recently, been estimated for only a few events. In a paper to be published in the November 2012 issue of The Astrophysical Journal <ins class="diffchange diffchange-inline">[1]</ins>, observations of thirty-eight large solar eruptive events made with over a dozen different spacecraft instruments have been used to produce the first statistical analysis of the energy partition throughout the various manifestations of an SEE. The paper studied the energy content of eleven different manifestations, namely -</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># Radiated energy in the GOES 1 - 8 &Aring; band;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># Radiated energy in the GOES 1 - 8 &Aring; band;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># Total radiated energy from the soft-X-ray-emitting plasma;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># Total radiated energy from the soft-X-ray-emitting plasma;</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># Energy in flare-accelerated electrons;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># Energy in flare-accelerated electrons;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># Energy in flare-accelerated ions;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># Energy in flare-accelerated ions;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div># CME kinetic energy in the rest frame of the Sun;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div># CME kinetic energy in the <ins class="diffchange diffchange-inline">[http://en.wikipedia.org/wiki/Rest_frame </ins>rest frame<ins class="diffchange diffchange-inline">] </ins>of the Sun;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># CME kinetic energy in the solar-wind rest frame;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># CME kinetic energy in the solar-wind rest frame;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># CME gravitational potential energy;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div># CME gravitational potential energy;</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 34:</td>
<td colspan="2" class="diff-lineno">Line 34:</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;"></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 panels in Figure 1 also show ellipses that trace the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside these ellipses are regarded as “outliers” and are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12, and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November, 2003. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The panels in Figure 1 also show ellipses that trace the 2σ <ins class="diffchange diffchange-inline">[http://en.wikipedia.org/wiki/Standard_deviation </ins>statistical deviation<ins class="diffchange diffchange-inline">] </ins>limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside these ellipses are regarded as “outliers” and are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12, and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November, 2003. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</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>Only for six of the events studied could all eleven energetic components be measured. Figure 2 shows the (logarithmic) average values of these energetic components, together with their 1σ "uncertainties" determined from the scatter of the values. This figure establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Only for six of the events studied could all eleven energetic components be measured. Figure 2 shows the (logarithmic) average values of these energetic components, together with their 1σ "uncertainties" determined from the scatter of the values. This figure establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 42:</td>
<td colspan="2" class="diff-lineno">Line 42:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>]] </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>]] </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline">All </del>of the energy in the flare-accelerated particles appears to ultimately emerge as radiation across a wide range of wavelengths, from optical to soft X-rays. However, only about one-third of the energy in flare-accelerated particles (~2% of the available stored energy) is ultimately radiated from high-temperature soft X-ray-emitting plasma. The maximum amount of energy stored as enhanced thermal energy in the soft X-ray-emitting plasma is ~1% of that released, and the amount of energy radiated in the diagnostic GOES 1 – 8 &Aring; waveband is only about 5% of the total energy radiated by the SXR-emitting plasma, or a mere one-tenth of a percent of the available magnetic energy. Because of the need for a CME to "overtake" the solar wind and form a shock front where SEPs can be accelerated, only about two-thirds of the kinetic energy carried by the CME (~15% of the available magnetic energy) is available for SEP acceleration. The SEP production process is in turn ~4% efficient, so that only about half a percent of the released magnetic energy ultimately appears in the form of SEPs.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">A major fraction </ins>of the energy in the flare-accelerated particles appears to ultimately emerge as radiation across a wide range of wavelengths, from optical to soft X-rays. However, only about one-third of the energy in flare-accelerated particles (~2% of the available stored energy) is ultimately radiated from high-temperature soft X-ray-emitting plasma. The maximum amount of energy stored as enhanced thermal energy in the soft X-ray-emitting plasma is ~1% of that released, and the amount of energy radiated in the diagnostic GOES 1 – 8 &Aring; waveband is only about 5% of the total energy radiated by the SXR-emitting plasma, or a mere one-tenth of a percent of the available magnetic energy. Because of the need for a CME to "overtake" the solar wind and form a shock front where SEPs can be accelerated, only about two-thirds of the kinetic energy carried by the CME (~15% of the available magnetic energy) is available for SEP acceleration. The SEP production process is in turn ~4% efficient, so that only about half a percent of the released magnetic energy ultimately appears in the form of SEPs.</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>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5439&oldid=prevBdennis: Reformatted table2012-10-05T22:18:40Z<p>Reformatted table</p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 22:18, 5 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 14:</td>
<td colspan="2" class="diff-lineno">Line 14:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Solar eruptive events (SEEs) consist of [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm flares] and their associated coronal mass ejections ([http://solarscience.msfc.nasa.gov/CMEs.shtml CMEs]). They are the most energetic transient events in the solar system. Over a period of tens of seconds to minutes, they can convert upwards of 10<sup>32</sup> ergs of energy stored in current-carrying magnetic fields into accelerated particles, heated [http://en.wikipedia.org/wiki/Plasma_(physics) plasma], and ejected solar material.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Solar eruptive events (SEEs) consist of [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm flares] and their associated coronal mass ejections ([http://solarscience.msfc.nasa.gov/CMEs.shtml CMEs]). They are the most energetic transient events in the solar system. Over a period of tens of seconds to minutes, they can convert upwards of 10<sup>32</sup> ergs of energy stored in current-carrying magnetic fields into accelerated particles, heated [http://en.wikipedia.org/wiki/Plasma_(physics) plasma], and ejected solar material.</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 partition of this released energy amongst these component parts has, until recently, been estimated for only a few events. In a paper to be published in the November 2012 issue of The Astrophysical Journal, observations of thirty-eight large solar eruptive events made with over a dozen different spacecraft instruments have been used to produce the first statistical analysis of the energy partition throughout the various manifestations of an SEE. The paper studied the energy content of eleven different manifestations, namely</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The partition of this released energy amongst these component parts has, until recently, been estimated for only a few events. In a paper to be published in the November 2012 issue of The Astrophysical Journal, observations of thirty-eight large solar eruptive events made with over a dozen different spacecraft instruments have been used to produce the first statistical analysis of the energy partition throughout the various manifestations of an SEE. The paper studied the energy content of eleven different manifestations, namely <ins class="diffchange diffchange-inline">-</ins></div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div> </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>Radiated energy in the GOES 1 - 8 &Aring; band;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 1. </del>Radiated energy in the GOES 1 - 8 &Aring; band;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>Total radiated energy from the soft-X-ray-emitting plasma;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 2. </del>Total radiated energy from the soft-X-ray-emitting plasma;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>Total (bolometric) radiated output;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 3. </del>Total (bolometric) radiated output;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>Peak thermal energy of the soft-X-ray-emitting plasma;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 4. </del>Peak thermal energy of the soft-X-ray-emitting plasma;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>Energy in flare-accelerated electrons;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 5. </del>Energy in flare-accelerated electrons;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>Energy in flare-accelerated ions;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 6. </del>Energy in flare-accelerated ions;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>CME kinetic energy in the rest frame of the Sun;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 7. </del>CME kinetic energy in the rest frame of the Sun;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>CME kinetic energy in the solar-wind rest frame;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 8. </del>CME kinetic energy in the solar-wind rest frame;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>CME gravitational potential energy;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 9. </del>CME gravitational potential energy;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>Energy in solar energetic particles (SEPs) detected in interplanetary space; and</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 10. </del>Energy in solar energetic particles (SEPs) detected in interplanetary space; and</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline"># </ins>Free (i.e., nonpotential) magnetic energy in the active region.</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div><del class="diffchange diffchange-inline"> 11. </del>Free (i.e., nonpotential) magnetic energy in the active region.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Data Reduction==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Data Reduction==</div></td></tr>
</table>Bdennishttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5438&oldid=prevBdennis: /* Data Reduction */2012-10-05T22:14:12Z<p><span class="autocomment">Data Reduction</span></p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 22:14, 5 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 30:</td>
<td colspan="2" class="diff-lineno">Line 30:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Data Reduction==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Data Reduction==</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>Comparing the energy content of the different components with one another provides significant insight into their relative importance in the overall <del class="diffchange diffchange-inline">SEE </del>energy budget. An example is shown in Figure 1(left), where, for each event, the energy in flare-accelerated particles (electrons plus ions) is plotted against the peak energy content in the <del class="diffchange diffchange-inline">hot </del>soft-X-ray-emitting plasma. The points are clustered around their (logarithmic) centroid (indicated by a “bull’s eye” symbol, with its coordinates in units of 10<sup>30</sup> ergs indicated at the top left of the figure<del class="diffchange diffchange-inline">)</del>. Dashed diagonal lines corresponding to ratios of 1%, 10% and 100% are shown. Although the ratio of energy components varies from only a few percent to almost 100%, the position of the centroid shows that, taken as a “forest” rather than individual “trees,” about 10% of the energy content in accelerated particles ends up in hot plasma. Another example is shown in Figure 1(right), which compares the free energy in the magnetic field with the energy in the CME. The points in this figure are clustered more closely than those in the left panel, and the centroid shows that on average about 20% of the available magnetic energy is released in the CME, although the ratio can vary from a few percent to ~50%.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Comparing the energy content of the different <ins class="diffchange diffchange-inline">SEE </ins>components with one another provides significant insight into their relative importance in the overall energy budget. An example is shown in Figure 1(left), where, for each event, the energy in flare-accelerated particles (electrons plus ions) is plotted against the peak energy content in the soft-X-ray-emitting plasma. The points are clustered around their (logarithmic) centroid (indicated by a “bull’s eye” symbol<ins class="diffchange diffchange-inline">)</ins>, with its coordinates in units of 10<sup>30</sup> ergs indicated at the top left of the figure. Dashed diagonal lines corresponding to ratios of 1%, 10% and 100% are shown. Although the ratio of energy components varies from only a few percent to almost 100%, the position of the centroid shows that, taken as a “forest” rather than individual “trees,” about 10% of the energy content in accelerated particles ends up in hot plasma. Another example is shown in Figure 1(right), which compares the free energy in the magnetic field with the energy in the CME. The points in this figure are clustered more closely than those in the left panel, and the centroid shows that on average about 20% of the available magnetic energy is released in the CME, although the ratio can vary from a few percent to ~50%.</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:185f1.png|thumb|center|600px|Figure 1: Left, comparison of the energy in accelerated particles with the energy of the hot plasma (the soft X-ray source); right, similar comparison of the free energy in the magnetic field with the energy of the CME. The left panel shows that roughly 10% of the energy from the particles winds up in the plasma, and the right panel shows that the CME can consume a sizeable fraction of the available free energy estimated for the region. The diagonal lines show ratios of 1%, 10%, and 100%.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:185f1.png|thumb|center|600px|Figure 1: Left, comparison of the energy in accelerated particles with the energy of the hot plasma (the soft X-ray source); right, similar comparison of the free energy in the magnetic field with the energy of the CME. The left panel shows that roughly 10% of the energy from the particles winds up in the plasma, and the right panel shows that the CME can consume a sizeable fraction of the available free energy estimated for the region. The diagonal lines show ratios of 1%, 10%, and 100%.</div></td></tr>
</table>Bdennishttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5437&oldid=prevBdennis: /* Data Reduction */ Minor tweaks2012-10-05T22:04:24Z<p><span class="autocomment">Data Reduction: </span> Minor tweaks</p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 22:04, 5 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 30:</td>
<td colspan="2" class="diff-lineno">Line 30:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Data Reduction==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Data Reduction==</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>Comparing <del class="diffchange diffchange-inline">these </del>energy <del class="diffchange diffchange-inline">contents in pairs </del>provides significant insight into their relative importance in the overall <del class="diffchange diffchange-inline">flare </del>energy budget. An example is shown in Figure 1 (left), <del class="diffchange diffchange-inline">which compares </del>the energy in flare-accelerated particles (electrons <del class="diffchange diffchange-inline">and </del>ions) <del class="diffchange diffchange-inline">with </del>the peak energy content in the hot soft-X-ray-emitting plasma. The points are clustered around their (logarithmic) centroid (indicated by a “bull’s eye” symbol, with its coordinates indicated at the top left of the figure). Dashed diagonal lines corresponding to ratios of 1%, 10% and 100% are shown. Although the ratio of energy components varies <del class="diffchange diffchange-inline"> </del>from only a few percent to almost 100%, the position of the centroid shows that, taken as a “forest” rather than individual “trees,” about 10% of the energy content in accelerated particles ends up in hot plasma. Another example is shown in Figure 1 (right), which compares the free energy in the magnetic field with the energy in the CME. The points in this figure are clustered more closely than those in the left panel, and the centroid shows that on average about 20% of the available magnetic energy is released in the CME, although the ratio can vary from a few percent to <del class="diffchange diffchange-inline">almost </del>50%.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Comparing <ins class="diffchange diffchange-inline">the </ins>energy <ins class="diffchange diffchange-inline">content of the different components with one another </ins>provides significant insight into their relative importance in the overall <ins class="diffchange diffchange-inline">SEE </ins>energy budget. An example is shown in Figure 1(left), <ins class="diffchange diffchange-inline">where, for each event, </ins>the energy in flare-accelerated particles (electrons <ins class="diffchange diffchange-inline">plus </ins>ions) <ins class="diffchange diffchange-inline">is plotted against </ins>the peak energy content in the hot soft-X-ray-emitting plasma. The points are clustered around their (logarithmic) centroid (indicated by a “bull’s eye” symbol, with its coordinates <ins class="diffchange diffchange-inline">in units of 10<sup>30</sup> ergs </ins>indicated at the top left of the figure). Dashed diagonal lines corresponding to ratios of 1%, 10% and 100% are shown. Although the ratio of energy components varies from only a few percent to almost 100%, the position of the centroid shows that, taken as a “forest” rather than individual “trees,” about 10% of the energy content in accelerated particles ends up in hot plasma. Another example is shown in Figure 1(right), which compares the free energy in the magnetic field with the energy in the CME. The points in this figure are clustered more closely than those in the left panel, and the centroid shows that on average about 20% of the available magnetic energy is released in the CME, although the ratio can vary from a few percent to <ins class="diffchange diffchange-inline">~</ins>50%.</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:185f1.png|thumb|center|600px|Figure 1: Left, comparison of the energy in accelerated particles with the energy of the hot plasma (the soft X-ray source); right, similar comparison of the free energy in the magnetic field with the energy of the CME. The left panel shows that roughly 10% of the energy from the particles winds up in the plasma, and the right panel shows that the CME can consume a sizeable fraction of the available free energy estimated for the region. The diagonal lines show ratios of 1%, 10%, and 100%.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:185f1.png|thumb|center|600px|Figure 1: Left, comparison of the energy in accelerated particles with the energy of the hot plasma (the soft X-ray source); right, similar comparison of the free energy in the magnetic field with the energy of the CME. The left panel shows that roughly 10% of the energy from the particles winds up in the plasma, and the right panel shows that the CME can consume a sizeable fraction of the available free energy estimated for the region. The diagonal lines show ratios of 1%, 10%, and 100%.</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;"></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 panels in Figure 1 also show <del class="diffchange diffchange-inline">elliptical loci corresponding to </del>the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside these <del class="diffchange diffchange-inline">loci </del>are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12 and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November, 2003. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The panels in Figure 1 also show <ins class="diffchange diffchange-inline">ellipses that trace </ins>the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside these <ins class="diffchange diffchange-inline">ellipses are regarded as “outliers” and </ins>are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12<ins class="diffchange diffchange-inline">, </ins>and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November, 2003. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</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>Only for six of the events studied could all eleven energetic components be measured. Figure 2 shows the (logarithmic) average values of these energetic components, together with their 1σ "uncertainties" determined from the scatter of the values. This figure establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Only for six of the events studied could all eleven energetic components be measured. Figure 2 shows the (logarithmic) average values of these energetic components, together with their 1σ "uncertainties" determined from the scatter of the values. This figure establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td></tr>
</table>Bdennishttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5436&oldid=prevBdennis: /* Introduction */2012-10-05T21:47:48Z<p><span class="autocomment">Introduction</span></p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 21:47, 5 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 12:</td>
<td colspan="2" class="diff-lineno">Line 12:</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>Solar eruptive events (SEEs) consist of [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm flares] and their associated coronal mass ejections ([http://solarscience.msfc.nasa.gov/CMEs.shtml CMEs]). They are the most energetic transient events in the solar system. Over a period of tens of seconds to minutes, they can convert upwards of 10<sup>32</sup> ergs of energy <del class="diffchange diffchange-inline">carried </del>in current-carrying magnetic fields into accelerated particles, heated [http://en.wikipedia.org/wiki/Plasma_(physics) plasma], and ejected solar material.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Solar eruptive events (SEEs) consist of [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm flares] and their associated coronal mass ejections ([http://solarscience.msfc.nasa.gov/CMEs.shtml CMEs]). They are the most energetic transient events in the solar system. Over a period of tens of seconds to minutes, they can convert upwards of 10<sup>32</sup> ergs of energy <ins class="diffchange diffchange-inline">stored </ins>in current-carrying magnetic fields into accelerated particles, heated [http://en.wikipedia.org/wiki/Plasma_(physics) plasma], and ejected solar material.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The partition of this released energy amongst these component parts has, until recently, been estimated for only a few events. In a paper to be published in the November 2012 issue of The Astrophysical Journal, observations of thirty-eight large solar eruptive events made with over a dozen different spacecraft instruments have been used to produce the first statistical analysis of the energy partition throughout the various manifestations of an SEE. The paper studied the energy content of eleven different manifestations, namely</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The partition of this released energy amongst these component parts has, until recently, been estimated for only a few events. In a paper to be published in the November 2012 issue of The Astrophysical Journal, observations of thirty-eight large solar eruptive events made with over a dozen different spacecraft instruments have been used to produce the first statistical analysis of the energy partition throughout the various manifestations of an SEE. The paper studied the energy content of eleven different manifestations, namely</div></td></tr>
</table>Bdennishttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5435&oldid=prevBdennis: Minor tweaks.2012-10-05T21:45:02Z<p>Minor tweaks.</p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 21:45, 5 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 12:</td>
<td colspan="2" class="diff-lineno">Line 12:</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>Solar eruptive events (SEEs) consist of [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm flares] and their associated coronal ejections ([http://solarscience.msfc.nasa.gov/CMEs.shtml CMEs]). They are the most energetic <del class="diffchange diffchange-inline">occurrences </del>in the solar system. Over a period of tens of seconds to minutes, they can convert upwards of 10<sup>32</sup> ergs of energy carried in current-carrying magnetic fields into accelerated particles, heated [http://en.wikipedia.org/wiki/Plasma_(physics) plasma], and ejected solar material.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Solar eruptive events (SEEs) consist of [http://hesperia.gsfc.nasa.gov/sftheory/flare.htm flares] and their associated coronal <ins class="diffchange diffchange-inline">mass </ins>ejections ([http://solarscience.msfc.nasa.gov/CMEs.shtml CMEs]). They are the most energetic <ins class="diffchange diffchange-inline">transient events </ins>in the solar system. Over a period of tens of seconds to minutes, they can convert upwards of 10<sup>32</sup> ergs of energy carried in current-carrying magnetic fields into accelerated particles, heated [http://en.wikipedia.org/wiki/Plasma_(physics) plasma], and ejected solar material.</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 partition of this released energy amongst these component parts has until recently been estimated for only a few events. In a paper to be published in the November 2012 issue of The Astrophysical Journal, <del class="diffchange diffchange-inline">data from </del>over a dozen different spacecraft instruments <del class="diffchange diffchange-inline">has </del>been used to produce the first statistical analysis of energy partition throughout the various manifestations of an SEE<del class="diffchange diffchange-inline">, for thirty-eight large events</del>. The paper studied the energy content of eleven different manifestations, namely</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The partition of this released energy amongst these component parts has<ins class="diffchange diffchange-inline">, </ins>until recently<ins class="diffchange diffchange-inline">, </ins>been estimated for only a few events. In a paper to be published in the November 2012 issue of The Astrophysical Journal, <ins class="diffchange diffchange-inline">observations of thirty-eight large solar eruptive events made with </ins>over a dozen different spacecraft instruments <ins class="diffchange diffchange-inline">have </ins>been used to produce the first statistical analysis of <ins class="diffchange diffchange-inline">the </ins>energy partition throughout the various manifestations of an SEE. The paper studied the energy content of eleven different manifestations, namely</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> 1. Radiated energy in the GOES 1 - 8 &Aring; band;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 1. Radiated energy in the GOES 1 - 8 &Aring; band;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div> 2. Total radiated energy from the soft X-ray-emitting plasma;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div> 2. Total radiated energy from the soft<ins class="diffchange diffchange-inline">-</ins>X-ray-emitting plasma;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 3. Total (bolometric) radiated output;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 3. Total (bolometric) radiated output;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div> 4. Peak thermal energy of the soft X-ray-emitting plasma;</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div> 4. Peak thermal energy of the soft<ins class="diffchange diffchange-inline">-</ins>X-ray-emitting plasma;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 5. Energy in flare-accelerated electrons;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 5. Energy in flare-accelerated electrons;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 6. Energy in flare-accelerated ions;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 6. Energy in flare-accelerated ions;</div></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 25:</td>
<td colspan="2" class="diff-lineno">Line 25:</td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 8. CME kinetic energy in the solar-wind rest frame;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 8. CME kinetic energy in the solar-wind rest frame;</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 9. CME gravitational potential energy;</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 9. CME gravitational potential energy;</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div> 10. Energy in solar energetic particles (SEPs) <del class="diffchange diffchange-inline">produced </del>in interplanetary space; and</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div> 10. Energy in solar energetic particles (SEPs) <ins class="diffchange diffchange-inline">detected </ins>in interplanetary space; and</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 11. Free (i.e., nonpotential) magnetic energy in the active region.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div> 11. Free (i.e., nonpotential) magnetic energy in the active region.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 35:</td>
<td colspan="2" class="diff-lineno">Line 35:</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;"></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 panels in Figure 1 also show elliptical loci corresponding to the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside these loci are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12 and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November <del class="diffchange diffchange-inline">of that year</del>. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>The panels in Figure 1 also show elliptical loci corresponding to the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside these loci are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12 and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November<ins class="diffchange diffchange-inline">, 2003</ins>. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</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>Only for six of the events studied could all eleven energetic components be measured. <del class="diffchange diffchange-inline">The </del>(logarithmic) average values of these energetic components, together with their 1σ uncertainties<del class="diffchange diffchange-inline">, are shown in Figure 2</del>. This <del class="diffchange diffchange-inline">Figure </del>establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Only for six of the events studied could all eleven energetic components be measured. <ins class="diffchange diffchange-inline">Figure 2 shows the </ins>(logarithmic) average values of these energetic components, together with their 1σ <ins class="diffchange diffchange-inline">"</ins>uncertainties<ins class="diffchange diffchange-inline">" determined from the scatter of the values</ins>. This <ins class="diffchange diffchange-inline">figure </ins>establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </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:185f2.png|thumb|center|600px|Figure 2: </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[File:185f2.png|thumb|center|600px|Figure 2: </div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Average (logarithmic) values of the energetic components, together with their uncertainties, for the events <del class="diffchange diffchange-inline">in </del>which all <del class="diffchange diffchange-inline">components </del>could be </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Average (logarithmic) values of the energetic components, together with their <ins class="diffchange diffchange-inline">1σ "</ins>uncertainties<ins class="diffchange diffchange-inline">" determined from the scatter of the values</ins>, for the <ins class="diffchange diffchange-inline">six </ins>events <ins class="diffchange diffchange-inline">for </ins>which all <ins class="diffchange diffchange-inline">component eneergies </ins>could be determined.</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>determined.</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>]] </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>]] </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"></td></tr>
<tr><td colspan="2" class="diff-lineno">Line 48:</td>
<td colspan="2" class="diff-lineno">Line 47:</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>As well as establishing the above general partitioning of energy amongst its various manifestations in large SEEs, the paper also concludes that the energy radiated by the SXR-emitting plasma exceeds, by about half an order of magnitude, the peak energy content of the thermal plasma that produces this radiation, a situation that requires continuous re-energization of the hot plasma throughout the flare. Also, the energy contents in flare-accelerated electrons and ions are comparable, and together they are sufficient to supply the bolometric energy radiated across all wavelengths throughout the event. Finally, the paper finds that, in general, the available magnetic energy is sufficient to power the CME, the flare-accelerated particles, and the hot thermal plasma. This reaffirms the generally-held belief that the fundamental power source for SEEs lies in stressed active region magnetic fields.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>As well as establishing the above general partitioning of energy amongst its various manifestations in large SEEs, the paper also concludes that the energy radiated by the SXR-emitting plasma exceeds, by about half an order of magnitude, the peak energy content of the thermal plasma that produces this radiation, a situation that requires continuous re-energization of the hot plasma throughout the flare. Also, the energy contents in flare-accelerated electrons and ions are comparable, and together they are sufficient to supply the bolometric energy radiated across all wavelengths throughout the event. Finally, the paper finds that, in general, the available magnetic energy is sufficient to power the CME, the flare-accelerated particles, and the hot thermal plasma. This reaffirms the generally-held belief that the fundamental power source for SEEs lies in stressed active<ins class="diffchange diffchange-inline">-</ins>region magnetic fields.</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>==Reference==</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>==Reference==</div></td></tr>
</table>Bdennishttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5434&oldid=prevGordonEmslie at 14:51, 5 October 20122012-10-05T14:51:42Z<p></p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 14:51, 5 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 35:</td>
<td colspan="2" class="diff-lineno">Line 35:</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;"></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>Figure 1 also show elliptical loci corresponding to the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside <del class="diffchange diffchange-inline">this locus </del>are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12 and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November of that year. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div><ins class="diffchange diffchange-inline">The panels in </ins>Figure 1 also show elliptical loci corresponding to the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside <ins class="diffchange diffchange-inline">these loci </ins>are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12 and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November of that year. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</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>Only for six of the events studied could all eleven energetic components be measured. The (logarithmic) average values of these energetic components, together with their 1σ uncertainties, are shown in Figure 2. This Figure establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Only for six of the events studied could all eleven energetic components be measured. The (logarithmic) average values of these energetic components, together with their 1σ uncertainties, are shown in Figure 2. This Figure establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td></tr>
</table>GordonEmsliehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Energy_Partition_in_Large_Solar_Eruptive_Events&diff=5433&oldid=prevGordonEmslie at 14:49, 5 October 20122012-10-05T14:49:40Z<p></p>
<table style="background-color: white; color:black;">
<col class='diff-marker' />
<col class='diff-content' />
<col class='diff-marker' />
<col class='diff-content' />
<tr valign='top'>
<td colspan='2' style="background-color: white; color:black;">← Older revision</td>
<td colspan='2' style="background-color: white; color:black;">Revision as of 14:49, 5 October 2012</td>
</tr><tr><td colspan="2" class="diff-lineno">Line 35:</td>
<td colspan="2" class="diff-lineno">Line 35:</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;"></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>Figure 1 <del class="diffchange diffchange-inline">(left) </del>also show elliptical loci corresponding to the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside this locus are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12 and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November of that year. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Figure 1 also show elliptical loci corresponding to the 2σ statistical deviation limit in both overall event size S = √(XY) and ratio R = Y/X. Events that lie outside this locus are labeled by the event numbers assigned in the paper, rather than generically by triangles. For example, in Figure 1 (right), events 1, 12 and 25 are “outliers.” For event 1 (2002 February 20, 05:52 UT), this simply indicates a relatively low conversion of magnetic energy into CME energy. For event 12 (2003 October 28, 09:51 UT), it indicates an unusually large event, one of the very large events in the “Halloween flares” of October/November of that year. However, the reasons for the unusually low ratio of CME energy to magnetic energy in event 25 (2005 January 20, 06:36 UT) are more intriguing. This event also had a very high ratio of SEP to CME energy and was the only event studied that had a bolometric radiated energy that was larger than the energy in the CME. It has therefore been suggested that the SEPs in this event were accelerated not in a CME-driven shock, but rather in the flare itself.</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>Only for six of the events studied could all eleven energetic components be measured. The (logarithmic) average values of these energetic components, together with their 1σ uncertainties, are shown in Figure 2. This Figure establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Only for six of the events studied could all eleven energetic components be measured. The (logarithmic) average values of these energetic components, together with their 1σ uncertainties, are shown in Figure 2. This Figure establishes the following energy budgets for a “typical” large SEE. Of the ~10<sup>33</sup> ergs of available magnetic energy, approximately 30% is released in the SEE, with the remainder staying in the active region as stored magnetic energy. Of the ~30% that is released, some 80% (~25% of the available energy) is released in the CME (mostly as kinetic energy) and approximately 20% (~5% of the available energy) is released as flare-accelerated particles, roughly evenly distributed between electrons and ions. </div></td></tr>
</table>GordonEmslie