Hadron acceleration in luminous cosmic high-energy neutrino and gamma-ray sources

发光宇宙高能中微子和伽马射线源中的强子加速

• 批准号: 66741702
• 负责人: Professor Dr. Wolfgang Rhode
• 金额: --
• 依托单位: Lehrstuhl für Experimentelle Physik V
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2008
• 资助国家: 德国
• 起止时间: 2007-12-31 至 2014-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/66741702?language=en
• 关键词: Hadron; acceleration; luminous; cosmic; energy

Recently, the sensitivity of the AMANDA neutrino detector has reached a level comparable to the Cherenkov telescopes like HEGRA or Whipple in TeV gammas. Therefore, the question if and under which conditions coincident observations of γ-rays and neutrinos are possible, gains increasing importance. Coordinated neutrino and γ-ray observations are crucial to address one of the key questions facing high-energy astrophysics: which primary acceleration mechanism (hadronic or leptonic) is responsible for the increasingly puzzling emission of high luminous active galactic nuclei (AGN). Because of secondary electron production, primary hadronic models always have a strong leptonic component, so that a detailed modeling of mixed leptonic and hadronic acceleration models is required, especially investigating the connection between the neutrino and γ-ray energy spectra and their time behavior. This is the main purpose of this proposal.Systematically, the acceleration of high-energy hadrons by different electromagnetic mechanisms and their transport through the intergalactic matter, radiation and magnetic fields will be calculated. The secondary leptons produced by interactions of the primarily accelerated particles will be tracked to the Earth. Here, the calculated fluxes will be compared to existing measurements of the Cherenkov telescopes like H.E.S.S., MAGIC, VERITAS and the neutrino telescopes like IceCube, Baikal or ANTARES. Special emphasis will be put on the isolation of signatures increasing the sensitivity of multi messenger campaigns connected to different energy ranges, e.g. by setting time windows or requiring certain constrains on the time correlation or anti-correlation of signals at different wavelengths.

最近，阿曼达中微子探测器的灵敏度已经达到了与切伦科夫望远镜（如HEGRA或维普莱）在TeV伽马中相当的水平。因此，γ射线和中微子的同时观测是否以及在何种条件下是可能的问题变得越来越重要。协调中微子和γ射线观测对于解决高能天体物理学面临的一个关键问题至关重要：哪个主要加速机制（强子或轻子）负责高亮度活动星系核（AGN）越来越令人困惑的发射。由于二次电子的产生，原强子模型总是具有很强的轻子成分，因此需要对轻子和强子混合加速模型进行详细的建模，特别是研究中微子和γ射线能谱与它们的时间行为之间的联系。这是本计划的主要目的，将系统地计算高能强子在不同电磁机制下的加速及其在星系际物质、辐射和磁场中的输运。初级加速粒子相互作用产生的次级轻子将被追踪到地球。在这里，计算出的通量将与切伦科夫望远镜（如H.E.S.S.）的现有测量结果进行比较，MAGIC，VERITAS和中微子望远镜，如IceCube，贝加尔湖或ANTARES。将特别强调签名的隔离，以提高与不同能量范围相关的多信使活动的灵敏度，例如通过设置时间窗口或要求对不同波长信号的时间相关性或反相关性进行某些约束。