PAMELA卫星数据作为非热Wino LSP暗物质信号
PAMELA Satellite Data as a Signal of Non-Thermal Wino LSP Dark Matter
摘要：
越来越多的卫星数据暗示并限制了暗物质物理学的发展。我们认为，有一个很好的动机与暗物质湮灭被观察到的PAMELA卫星探测器的理论预先存在的框架一致。暗物质（主要）是中性的W玻色子超伙伴，质量低于200 GeV的维诺。利用GALPROP程序对湮没产物和本底进行了研究。反物质和伽马射线从湮灭winos贡献低于这个能量。我们解释了为什么PAMELA的数据并不意味着没有反质子信号观察到PAMELA或早期的实验，并解释了为什么反质子分析被误解的早期论文。Wino湮没不能描述费米e ++ e-数据（除了部分低于~100 GeV）。在更高的能量下，我们期待天体物理机制，我们简单地参数化它们，这样组合就可以描述所有的数据。我们强调几个预测的卫星数据来测试维诺的解释，特别是在100 GeV以上的正电子和反质子谱的下调。大多数其他的解释都需要正电子率在100 GeV以上大幅上升。我们专注于研究这种动机良好和长期预测的wino解释，而不是与其他解释进行比较。我们强调，解释也非常强烈地依赖于对宇宙的宇宙学历史的假设，并在银河系中的反质子和正电子的传播。PAMELA观察到的winos起源于一些非热源，如模量衰变，而不是大爆炸后在热平衡中冷却的宇宙。然后，它是适当的规范化的wino密度的当地遗迹密度，并没有“助推因子”需要获得报告的PAMELA率。
英文摘要：
Satellite data is accumulating that suggests and constrains dark matter physics. We argue there is a very well motivated theoretical preexisting framework consistent with dark matter annihilation being observed by the PAMELA satellite detector. The dark matter is (mainly) the neutral W boson superpartner, the wino with mass below 200 GeV. Using the program GALPROP we study the annihilation products and backgrounds together. Antimatter and gammas from annihilating winos contribute below this energy. We explain why PAMELA data does not imply no antiproton signal was observed by PAMELA or earlier experiments, and explain why the antiproton analysis was misunderstood by earlier papers. Wino annihilation does not describe the Fermi e+ + e- data (except partially below ~ 100 GeV). At higher energies we expect astrophysical mechanisms, and we simply parameterize them so the combination can describe all the data. We emphasize several predictions for satellite data to test the wino interpretation, particularly the turndown of the positron and antiproton spectra above 100 GeV. Most other interpretations require a large rise in the positron rates above 100 GeV. We focus on studying this well-motivated and long predicted wino interpretation, rather than comparisons with other interpretations. We emphasize that interpretations also depend very strongly on assumptions about the cosmological history of the universe, and on propagation of antiprotons and positrons in the galaxy. The winos PAMELA is observing arose from some non-thermal sources such as moduli decay rather than a universe that cooled in thermal equilibrium after the big bang. Then it is appropriate to normalize the wino density to the local relic density, and no "boost factors" are needed to obtain the reported PAMELA rates.
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