<p><BR/>Replying to:<BR/><DIV CLASS='Discussion_PostQuote'>I get fustrated when I come to a Mozina post because the discussion is over and it becomes the same damn arguement as every other thread he posts in. Sentence for Sentence breakdown that is 2 pages long. I guess you have to type a lot of words to beat around the bush. Mozina is not interested in disussing scientific results, he is only interested in long debates on nothing.I would like to thank Dr. Rocket for posting that little overview of the discussion you had with the particle physicist. I am not remotely qualified to carry on the discussion, but I do enjoy following along and learning, too bad this discussion is over. <br />Posted by Meric</DIV><br /><br />Well it's not over, I'm trying to save it.</p><p>So, what is the suggested POSSIBLE source to the 300-600 Gev electrons?</p><p>Excerpt from a Review (not the research letter itself)</p><p>"This feature is located at an energy of about 620 GeV (1 GeV is 10<sup>9</sup> electronvolts and, by mass–energy equivalence, corresponds roughly to the mass of a proton). And it is consistent with the type of signal expected when KK WIMP particles interact and annihilate into electron–positron pairs. (The positron is the electron's antiparticle: essentially, an electron but with a positive charge.) The process basically amounts to two KK particles disappearing from 'the dark side' and appearing in our realm in the form of an electron–positron pair. The signature electrons can then be detected and measured.</p><p class="norm">What makes the ATIC detection especially intriguing is that the 620-GeV energy of the peak is roughly the mass of KK WIMPs expected from particle physics theories<sup>
7</sup>. But in a way, the intensity of the signal is almost too high. To explain its strength requires a large enhancement of local dark matter, such that the Solar System would be whizzing through (or at least near) an especially dense clump of dark matter.</p><p class="norm">From Nature Vol 456/20 20 Nov 2008</p><p class="norm"> </p><p class="norm">In the Letter itself, they go into great detail about why this is the most likely among the theoretical possibilities.</p><p class="norm">The "bump" in electrons has a very specific shape indicating a cutoff above 620 Gev, exactly as would be expected.</p><p class="norm">It is also confirmed to some varying extants by observations from AMS, HEAT, BETS, PPB-BETS and emulsion chambers.</p><p class="norm">There is no <em>known</em> baryonic source for such an excess. The closest would be the Geminga pulsar, however the flux from Geminga is about a factor of 60 too low to explain the observations.</p><p class="norm">Direct production of e- e+ from annihilation is supressed for SUSY particles and would have a broad spectrum and decrease in flux up to the particle mass. That is not what it shows. In fact what is expected is a rising flux to the mass of the K-K particles, then a sharp dropoff above that energy. That is precisely what is shown.</p><p class="norm"><br />
<img src="http://sitelife.space.com/ver1.0/Content/images/store/2/1/324a370c-69e2-4c3e-b1e5-8c000fcf0551.Medium.jpg" alt="" /></p><p>The GALPROP general electron spectrum resulting from sources across the galaxy is shown as the dashed line. The dotted curve represents the propagated electrons from the annihilation of a Kaluza–Klein particle. The dotted curve assumes an isothermal dark matter halo of 4-kpc scale height, a local dark matter density of 0.43 GeV cm<sup>-3</sup>, a Kaluza–Klein mass of 620 GeV, and an annihilation cross section rate of 1 X 10<sup>-23</sup> cm<sup>3</sup> s<sup>-1</sup>, which implies a boost factor of ~200. The sum of these signals is the solid curve. Here the spectrum is multiplied by <em>E</em><sup>3.0</sup> for clarity. The solid curve provides a good fit to both the magnetic spectrometer data<sup>
30, </sup><sup>
31</sup> and calorimeter data<sup>
16, </sup><sup>
32</sup> and reproduces all of the measurements from 20 GeV to 2 TeV, including the cut-off in the observed excess. All error bars are one standard deviation.</p><h1 class="page-header">FIGURE 4. <strong>Assuming an annihilation signature of Kaluza–Klein dark matter, all the data can be reproduced.</strong></h1><div class="container-cite"><h2 class="note">From the following article:</h2><p class="atl">
An excess of cosmic ray electrons at energies of 300–800 GeV</p><p class="aug">J. Chang, J. H. Adams, H. S. Ahn, G. L. Bashindzhagyan, M. Christl, O. Ganel, T. G. Guzik, J. Isbert, K. C. Kim, E. N. Kuznetsov, M. I. Panasyuk, A. D. Panov, W. K. H. Schmidt, E. S. Seo, N. V. Sokolskaya, J. W. Watts, J. P. Wefel, J. Wu & V. I. Zatsepin</p><p class="journal"><span class="journalname">Nature </span><span class="journalnumber">456</span>, 362-365(20 November 2008)</p><p class="doi"><span class="doi"><abbr title="Digital Object Identifier">doi</abbr>:10.1038/nature07477</span></p></div><p class="norm"><br /> </p><p> </p> <div class="Discussion_UserSignature"> <p><font color="#000080"><em><font color="#000000">But the Krell forgot one thing John. Monsters. Monsters from the Id.</font></em> </font></p><p><font color="#000080">I really, really, really, really miss the "first unread post" function</font><font color="#000080"> </font></p> </div>