https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&feed=atom&action=historyChree Analysis for Flares - Revision history2024-03-28T17:03:19ZRevision history for this page on the wikiMediaWiki 1.16.0https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&diff=11133&oldid=prevSchriste at 02:26, 18 September 20182018-09-18T02:26:42Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>3. Kretzschmar, M. et al. (2010), ''The effect of flares on total solar irradiance'' [http://adsabs.harvard.edu/abs/2010NatPh...6..690K]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>3. Kretzschmar, M. et al. (2010), ''The effect of flares on total solar irradiance'' [http://adsabs.harvard.edu/abs/2010NatPh...6..690K]</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">Category</del>: <del class="diffchange diffchange-inline">Nugget</del>]]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[<ins class="diffchange diffchange-inline">Has article subject</ins>:<ins class="diffchange diffchange-inline">: education</ins>]]</div></td></tr>
</table>Schristehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&diff=3547&oldid=prevHhudson: replaced ref. 3 with a more accessible one2010-10-25T17:09:22Z<p>replaced ref. 3 with a more accessible one</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>2. Reedy, R.C., Arnold, J.R., and Lal, D. (1983), ''Cosmic-ray record in solar system matter'' [http://adsabs.harvard.edu/abs/1983Sci...219..127R]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>2. Reedy, R.C., Arnold, J.R., and Lal, D. (1983), ''Cosmic-ray record in solar system matter'' [http://adsabs.harvard.edu/abs/1983Sci...219..127R]</div></td></tr>
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<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>3. Kretzschmar, M. (<del class="diffchange diffchange-inline">2008</del>), ''<del class="diffchange diffchange-inline">On the total and visible radiative output </del>of <del class="diffchange diffchange-inline">solar </del>flares'' [http://adsabs.harvard.edu/abs/<del class="diffchange diffchange-inline">2008cosp</del>...<del class="diffchange diffchange-inline">37</del>.<del class="diffchange diffchange-inline">1617K</del>]</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>3. Kretzschmar, M<ins class="diffchange diffchange-inline">. et al</ins>. (<ins class="diffchange diffchange-inline">2010</ins>), ''<ins class="diffchange diffchange-inline">The effect </ins>of flares <ins class="diffchange diffchange-inline">on total solar irradiance</ins>'' [http://adsabs.harvard.edu/abs/<ins class="diffchange diffchange-inline">2010NatPh.</ins>..<ins class="diffchange diffchange-inline">6</ins>..<ins class="diffchange diffchange-inline">690K</ins>]</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[Category: Nugget]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>[[Category: Nugget]]</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&diff=2015&oldid=prevSchriste at 18:22, 10 November 20092009-11-10T18:22:21Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = </div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|second_author = </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 30 March 2009</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 30 March 2009</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|next_nugget = Cycle 24 - <del class="diffchange diffchange-inline">time to </del>panic<del class="diffchange diffchange-inline">?</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">[[</ins>Cycle 24 - <ins class="diffchange diffchange-inline">don't </ins>panic <ins class="diffchange diffchange-inline">yet!]]</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [[High Temperatures in Active Regions]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [[High Temperatures in Active Regions]]</div></td></tr>
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</table>Schristehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&diff=995&oldid=prevHhudson at 00:44, 10 April 20092009-04-10T00:44:18Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 30 March 2009</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 30 March 2009</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">(by Nicole Vilmer)</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">Cycle 24 - time to panic?</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [[High Temperatures in Active Regions]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [[High Temperatures in Active Regions]]</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=Chree_Analysis_for_Flares&diff=990&oldid=prevHhudson at 18:53, 31 March 20092009-03-31T18:53:21Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The distribution function follows the power law <math>N(E) = AE^{-\gamma}</math>, where <math>A</math> (the normalization of the number of events per unit time) and <math>\gamma</math> (the power-law index) are constants.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The distribution function follows the power law <math>N(E) = AE^{-\gamma}</math>, where <math>A</math> (the normalization of the number of events per unit time) and <math>\gamma</math> (the power-law index) are constants.</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>One interesting feature of this description (other than its amazing precision) is the flatness of the observed power law, i.e. the smallness of <math>\gamma</math> (it is 1.732 <math>\pm</math> 0.008).</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>One interesting feature of this description (other than its amazing precision) is the flatness of the observed power law, i.e. the smallness of <math>\gamma</math> (it is 1.732 <math>\pm</math> 0.008<ins class="diffchange diffchange-inline">; see Figure 1</ins>).</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>As any math student can show, the integral of this distribution diverges, i.e. it incorrectly "predicts" an infinite flare power since the integral of E.N(E) diverges if <math>\gamma < 2</math>.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>As any math student can show, the integral of this distribution diverges, i.e. it incorrectly "predicts" an infinite flare power since the integral of E.N(E) diverges if <math>\gamma < 2</math>.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This property is somewhat perplexing, since obviously the Sun does not shine by flares alone.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This property is somewhat perplexing, since obviously the Sun does not shine by flares alone.</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&diff=989&oldid=prevHhudson at 18:52, 31 March 20092009-03-31T18:52:04Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The distribution function follows the power law <math>N(E) = AE^{-\gamma}</math>, where <math>A</math> (the normalization of the number of events per unit time) and <math>\gamma</math> (the power-law index) are constants.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The distribution function follows the power law <math>N(E) = AE^{-\gamma}</math>, where <math>A</math> (the normalization of the number of events per unit time) and <math>\gamma</math> (the power-law index) are constants.</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>One interesting feature of this description (other than its amazing precision) is the flatness of the observed power law, i.e. the smallness of <math>\gamma</math> (it is <del class="diffchange diffchange-inline">just less than 2</del>.0).</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>One interesting feature of this description (other than its amazing precision) is the flatness of the observed power law, i.e. the smallness of <math>\gamma</math> (it is <ins class="diffchange diffchange-inline">1</ins>.<ins class="diffchange diffchange-inline">732 <math>\pm</math> </ins>0<ins class="diffchange diffchange-inline">.008</ins>).</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>As any math student can show, the integral of this distribution diverges, i.e. it incorrectly "predicts" an infinite flare power since the integral of E.N(E) diverges if <math>\gamma < 2</math>.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>As any math student can show, the integral of this distribution diverges, i.e. it incorrectly "predicts" an infinite flare power since the integral of E.N(E) diverges if <math>\gamma < 2</math>.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This property is somewhat perplexing, since obviously the Sun does not shine by flares alone.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This property is somewhat perplexing, since obviously the Sun does not shine by flares alone.</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&diff=988&oldid=prevHhudson at 18:39, 31 March 20092009-03-31T18:39:59Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The distribution function follows the power law <math>N(E) = AE^{-\gamma}</math>, where <math>A</math> (the normalization of the number of events per unit time) and <math>\gamma</math> (the power-law index) are constants.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The distribution function follows the power law <math>N(E) = AE^{-\gamma}</math>, where <math>A</math> (the normalization of the number of events per unit time) and <math>\gamma</math> (the power-law index) are constants.</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>One interesting feature of this description (other than its amazing precision) is <del class="diffchange diffchange-inline">the </del>the flatness of the observed power law, i.e. the smallness of <math>\gamma</math>.</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>One interesting feature of this description (other than its amazing precision) is the flatness of the observed power law, i.e. the smallness of <math>\gamma</math> <ins class="diffchange diffchange-inline">(it is just less than 2.0)</ins>.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>As any math student can show, the integral of this distribution diverges, i.e. it incorrectly "predicts" an infinite flare power since the integral of E.N(E) diverges if <math>\gamma < 2</math>.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>As any math student can show, the integral of this distribution diverges, i.e. it incorrectly "predicts" an infinite flare power since the integral of E.N(E) diverges if <math>\gamma < 2</math>.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This property is somewhat perplexing, since obviously the Sun does not shine by flares alone.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>This property is somewhat perplexing, since obviously the Sun does not shine by flares alone.</div></td></tr>
</table>Hhudsonhttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&diff=987&oldid=prevHhudson at 17:28, 31 March 20092009-03-31T17:28:42Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 30 March 2009</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|publish_date = 30 March 2009</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>|next_nugget = (Nicole)</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>|next_nugget = (<ins class="diffchange diffchange-inline">by </ins>Nicole <ins class="diffchange diffchange-inline">Vilmer</ins>)</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [[High Temperatures in Active Regions]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>|previous_nugget = [[High Temperatures in Active Regions]]</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=Chree_Analysis_for_Flares&diff=982&oldid=prevSchriste: added category2009-03-30T17:28:00Z<p>added category</p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>3. Kretzschmar, M. (2008), ''On the total and visible radiative output of solar flares'' [http://adsabs.harvard.edu/abs/2008cosp...37.1617K]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>3. Kretzschmar, M. (2008), ''On the total and visible radiative output of solar flares'' [http://adsabs.harvard.edu/abs/2008cosp...37.1617K]</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;">[[Category: Nugget]]</ins></div></td></tr>
</table>Schristehttps://sprg.ssl.berkeley.edu/~tohban/wiki/index.php?title=Chree_Analysis_for_Flares&diff=981&oldid=prevSchriste: /* Signal or noise? */2009-03-30T17:27:13Z<p><span class="autocomment">Signal or noise?</span></p>
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<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The epoch in this case (the maximum, as marked by the arrow in Figure 2) coincides closely with the hard X-ray peak time as observable by RHESSI, although unfortunately not in this case.</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>The epoch in this case (the maximum, as marked by the arrow in Figure 2) coincides closely with the hard X-ray peak time as observable by RHESSI, although unfortunately not in this case.</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>[[Image:98flare_tsi.jpg|400px|thumb|center|'''Figure 2'': Observation of a flare signal in the [http://spot.colorado.edu/~koppg/TSI/ total solar irradiance] (ie, an apparent temporary increase of solar luminosity, as recorded by the [http://lasp.colorado.edu/sorce/index.htm SORCE] satellite. </div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>[[Image:98flare_tsi.jpg|400px|thumb|center|'''Figure 2<ins class="diffchange diffchange-inline">'</ins>'': Observation of a flare signal in the [http://spot.colorado.edu/~koppg/TSI/ total solar irradiance] (ie, an apparent temporary increase of solar luminosity, as recorded by the [http://lasp.colorado.edu/sorce/index.htm SORCE] satellite. </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Note the heavily suppressed zero of the flux scale (W/m<sup>2</sup>).</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>Note the heavily suppressed zero of the flux scale (W/m<sup>2</sup>).</div></td></tr>
<tr><td class='diff-marker'>-</td><td style="background: #ffa; color:black; font-size: smaller;"><div>Also note the <del class="diffchange diffchange-inline">fluctuatiing </del>signals before the flare; this is the background fluctuation (signal for some, but noise for this purpose);</div></td><td class='diff-marker'>+</td><td style="background: #cfc; color:black; font-size: smaller;"><div>Also note the <ins class="diffchange diffchange-inline">fluctuating </ins>signals before the flare; this is the background fluctuation (signal for some, but noise for this purpose);</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>this noise greatly reduces the precision of the flare observation.]]</div></td><td class='diff-marker'> </td><td style="background: #eee; color:black; font-size: smaller;"><div>this noise greatly reduces the precision of the flare observation.]]</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>Schriste