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The origin of the high energy gamma-ray emission from the Crab nebula - clues from the spatial extension and energy spectrum

蟹状星云高能伽马射线发射的起源——空间延伸和能谱的线索

基本信息

批准号：
360780919
负责人：
Professor Dr. Dieter Horns
金额：
--
依托单位：
Institut für Experimentalphysik
依托单位国家：
德国
项目类别：
Research Grants
财政年份：
2017
资助国家：
德国
起止时间：
2016-12-31 至 2020-12-31
项目状态：
已结题

来源：
https://gepris.dfg.de/gepris/projekt/360780919?language=en
关键词：
origin energy gamma ray emission

项目摘要

The Crab nebula is the remnant of a historical supernova from the year 1054. The nebula has been observed in great detail at every accessible energy from radio frequency to gamma-rays at 100 TeV. Most of the observed radiation is synchrotron emission of energetic particles originating in the steady pulsar wind emitted by the Crab pulsar. The energetic particles are deflected by the magnetic field (of largely unknown structure and strength) permeating the nebula. With recent observations of the nebula with Fermi-LAT we have been able to demonstrate that the nebula can be spatially resolved at energies above a few GeV. In this project, we will analyse both the data taken with Fermi-LAT as well as with the H.E.S.S. telescopes in order to determine the energy dependent size of the gamma-nebula. Jointly with the observed integrated spectrum, we will be able to spatially characterize the underlying electron energy distribution. The required assumption is an inverse Compton origin of the gamma-radiation,i.e., energetic electrons up-scatter lower energy photon fields present in the nebula. Given the detailed observations, we will refine the available radiation field estimates to include the emission from the dusty plasma at the boundary of the synchrotron nebula. Finally, we will estimate the magnetic field and its large-scale structure present in the nebula using our estimate of the spatial and spectral distribution of particles. In order to exclude that the results are influenced by additional radiative components at gamma-rays, we will study as an alternative non-thermal Bremsstrahlung emitted from the dense regions of the nebula. The result of the study will be an in-depth understanding of the energy dependent spatial distribution of electrons in the nebula and consequently will be prepared to answer the question on the origin of the gamma-ray emission of the Crab nebula.

蟹状星云是 1054 年历史上超新星的遗迹。该星云在从射频到 100 TeV 伽马射线的各种可用能量中都得到了详细的观测。大多数观测到的辐射是源自蟹状脉冲星发出的稳定脉冲星风的高能粒子的同步加速器发射。高能粒子被遍布星云的磁场（结构和强度很大程度上未知）偏转。通过最近用费米-LAT 对星云的观测，我们已经能够证明星云可以在高于几个 GeV 的能量下进行空间解析。在这个项目中，我们将分析使用 Fermi-LAT 以及 H.E.S.S. 获取的数据。望远镜以确定伽马星云的能量依赖大小。结合观察到的积分光谱，我们将能够在空间上表征潜在的电子能量分布。所需的假设是伽马辐射的逆康普顿原点，即高能电子向上散射星云中存在的较低能量光子场。鉴于详细的观测结果，我们将完善可用的辐射场估计，以包括同步加速器星云边界的尘埃等离子体的发射。最后，我们将使用对粒子空间和光谱分布的估计来估计星云中存在的磁场及其大尺度结构。为了排除结果受到伽马射线额外辐射成分的影响，我们将研究从星云密集区域发射的替代非热轫致辐射。研究的结果将是深入了解星云中电子的能量依赖空间分布，从而准备回答有关蟹状星云伽马射线发射起源的问题。