首页> 外文期刊>The Astrophysical journal >High-Energy Gamma-Ray Emission from Galactic Kerr-Newman Black Holes. I. The Central Engine
【24h】

High-Energy Gamma-Ray Emission from Galactic Kerr-Newman Black Holes. I. The Central Engine

机译:银河系Kerr-Newman黑洞的高能伽马射线发射。一,中央引擎

获取原文
           

摘要

A model of the central engine of the unidentified high-latitude galactic hard γ-ray (EGRET) sources based on black hole electrodynamics is presented. The γ-ray emission is produced in a bipolar outflow from a charged, rotating black hole (a Kerr-Newman black hole) in a low-density region of the Galaxy, the details of which are provided in a companion paper. The model proposed in this article and its companion is a synthesis of pair creation scenarios for pulsars, the theory of black hole magnetospheres and synchrotron self-Compton large-scale jets. This article describes the physics of the putative central engine. Kerr-Newman black holes are plausible endpoints of the catastrophic gravitational collapse of the most massive magnetized rotating stars. In the following, the ability of a Kerr-Newman black hole to drive a magnetically dominated plasma wind in the charge-starved limit is explored for the first time. Although there are important analogies to magnetohydrodynamic (MHD) wind theory of Kerr (uncharged rotating) black holes, there are also enormous distinctions. However, previous experience with the MHD Kerr case is exploited to render this more complicated problem tractable. The most important parameter for quantifying the wind energy is the magnetic field line angular velocity, ΩF (and unfortunately the most difficult to calculate). The determination of ΩF is tied directly to the process by which a pair plasma is created on large-scale magnetic field lines through high-energy quantum electrodynamic processes typical of pulsar magnetospheres. It is argued in principle how ΩF is determined by the plasma injection mechanism. Furthermore, the most significant result of this effort is the calculation of ΩF for a model that is determined by a plausible set of astronomical parameters. It is essential to realize a distinction from some charge-starved pulsar models: the energy source for the wind is quantified by the field line rotation rate (the cross-field potential), ultimately powered by the rotation of the hole through dissipative gravitomagnetic processes and not the volage drop across the vacuum pair creation gap.
机译:提出了一种基于黑洞电动力学的未知高纬银河硬γ射线(EGRET)源中央发动机模型。 γ射线的发射是从银河系低密度区域中带电的旋转黑洞(Kerr-Newman黑洞)产生的双极流出,其详细信息在随附的论文中提供。本文提出的模型及其伴随模型是对脉冲星对创建方案,黑洞磁层理论和同步加速器自康普顿大型喷气机的综合。本文介绍了假定的中央引擎的物理原理。克尔·纽曼(Kerr-Newman)黑洞是最庞大的磁化自转恒星灾难性引力坍塌的合理终点。在下文中,首次探索了Kerr-Newman黑洞在电荷匮乏的极限下驱动磁场主导的等离子风的能力。尽管与Kerr(不带电的旋转)黑洞的磁流体动力学(MHD)风理论有重要的比喻,但也有很多区别。但是,利用MHD Kerr案例的先前经验可以使这个更复杂的问题变得易于处理。量化风能的最重要参数是磁场线角速度ΩF(不幸的是最难计算)。 ΩF的确定直接取决于通过脉冲星磁层典型的高能量子电动力学过程在大规模磁场线上产生一对等离子体的过程。原则上争论了如何通过等离子体注入机制确定ΩF。此外,这项工作最重要的结果是计算了由合理的一组天文参数确定的模型的ΩF。重要的是,必须与某些电荷匮乏的脉冲星模型区分开来:风的能量由场线旋转速度(交叉场电势)量化,最终通过耗散的重力磁化过程通过空穴的旋转来提供动力。而不是真空对产生间隙中的体积下降。

著录项

获取原文

客服邮箱:kefu@zhangqiaokeyan.com

京公网安备:11010802029741号 ICP备案号:京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有
  • 客服微信

  • 服务号