宇宙学磁发电机：再电离时期的Biermann电池效应
Cosmological Magnetogenesis: The Biermann Battery during the Epoch of Reionization
AI总结：
在SPHINX项目中开发保结构的约束传输数值方法研究再电离时期Biermann电池效应，发现三种磁场产生通道，其中超新星外流通道在巨晕周围星际介质中产生高达$10^{-18}$ G的磁场。
摘要：
我们在SPHINX项目框架内，使用宇宙学自适应网格细化（Adaptive Mesh Refinement）模拟研究了再电离时期（Epoch of Reionization, EoR）Biermann电池效应。我们开发了一种新的数值技术，在约束传输（Constrained Transport）方法中求解Biermann电池项，既保持了磁场的零散度，又保证了等温流中不存在Biermann电池效应。我们数值方法的保结构特性在Strömgren球传播和Sedov爆炸波的验证测试中，对于最小化数值误差非常重要。然后，我们使用这种新方法，在RAMSES代码中结合最先进的星系形成模型，模拟了一个2.5和5共动Mpc宇宙学盒子的演化。与之前的发现不同，我们展示了三种不同的Biermann电池通道：第一种与EoR之前的线性扰动有关，第二种是与EoR期间再电离前沿相关的经典Biermann电池，第三种与强烈的超新星驱动外流有关。前两种通道自发产生了强度在或低于$10^{-20}$ G的充满体积的磁场，而后者由于更高的等离子体温度和勉强可分辨的湍流发电机，在巨大晕周围的星际介质中达到了高达$10^{-18}$ G的磁场强度。
英文摘要：
We investigate the effect of the Biermann battery during the Epoch of Reionization (EoR) using cosmological Adaptive Mesh Refinement simulations within the framework of the SPHINX project. We develop a novel numerical technique to solve for the Biermann battery term in the Constrained Transport method, preserving both the zero divergence of the magnetic field and the absence of Biermann battery for isothermal flows. The structure-preserving nature of our numerical method turns out to be very important to minimise numerical errors during validation tests of the propagation of a Strömgren sphere and of a Sedov blast wave. We then use this new method to model the evolution of a 2.5 and 5 co-moving Mpc cosmological box with a state-of-the-art galaxy formation model within the RAMSES code. Contrary to previous findings, we show that three different Biermann battery channels emerge: the first one is associated with linear perturbations before the EoR, the second one is the classical Biermann battery associated with reionization fronts during the EoR, and the third one is associated with strong, supernova-driven outflows. While the two former channels generate spontaneously volume-filling magnetic fields with a strength on the order or below $10^{-20}$ G, the latter, owing to the higher plasma temperature and a marginally-resolved turbulent dynamo, reaches a field strength as high as $10^{-18}$ G in the intergalactic medium around massive haloes.
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