论文标题
在新生的中子恒星中产生强磁场，以占手性磁效应
Generation of strong magnetic fields in a nascent neutron star accounting for the chiral magnetic effect
论文作者
论文摘要
我们在中子星（NS）中提出了最强磁场生成最强磁场的平均场发电机模型，$ b \ sim 10^{15} \，{\ rm g} $，这是指手性磁效应（CME）由超级Nova（SN）ns的hock驱动的。温度在狭窄的冲击战线上升高，在流入物质中存在的初始磁场急剧上升，是CME的来源，它由于血浆中的库仑碰撞而显着删除了CME。磁场在感应方程中的不稳定性项$ \ nabla \ times（α{\ bf b}）$的冲击后面的生长在成功的SN爆炸后停止，从而抛出了原始恒星的地幔。结果，这种爆炸会中断强磁化等离子体从冲击到NS表面的转移，并导致磁场的饱和度。假设刚性原恒星旋转，我们采用了平均场发电机，该发电机类似于标准磁流失动力学（MHD）中已知的$α^2 $ -DONNAMO。我们模型的新颖性是，$α^2 $ -DONNAMO基于MHD中应用的粒子物理概念，而不是旋转对流中对流涡旋的镜像不对称。
We propose the mean field dynamo model for the generation of strongest magnetic fields, $B\sim 10^{15}\,{\rm G}$, in a neutron star (NS) accounting for the chiral magnetic effect (CME) driven by the shock in a supernova (SN) progenitor of that NS. The temperature jump at a narrow shock front, where an initial magnetic field existing in inflowing matter rises sharply, is the source of the CME that prevails significantly the erasure of the CME due to the spin-flip through Coulomb collisions in plasma. The growth of the magnetic field just behind the shock given by the instability term $\nabla\times (α{\bf B})$ in induction equation, stops after a successful SN explosion that throws out the mantle of a protoneutron star. As a result, such an explosion interrupts the transfer of strongly magnetized plasma from the shock onto NS surface and leads to the saturation of the magnetic field. Assuming the rigid protostar rotation, we employ the mean field dynamo, which is similar to the $α^2$-dynamo known in the standard magnetohydrodynamics (MHD). The novelty of our model is that $α^2$-dynamo is based on concepts of particle physics, applied in MHD, rather than by a mirror asymmetry of convective vortices in the rotating convection.
