论文标题
引入脉冲星风云的HD+B模型：一种混合流体动力学/辐射方法
Introducing the HD+B model for pulsar wind nebulae: a hybrid hydrodynamics/radiative approach
论文作者
论文摘要
快速增加的脉冲星星云的识别和表征是，并且将继续是高能量伽玛射线天体物理学的挑战。鉴于到目前为止，这种系统构成了TEV制度中最预期的人群，因此这种特征不仅重要，不仅是从个人和人群的角度了解来源本身，而且也能够与其他频率的观察结果联系起来，尤其是在广播和X射线中。同样，我们需要在高度混乱的天空中删除星云的发射，以揭示其他潜在的发射器。在本文中，我们提出了一种用于脉冲星风云的理论建模的新方法：一种能够再现形态特征和源光谱的混合流动动力学模型，其数值成本相对有限。
Identification and characterization of a rapidly increasing number of pulsar wind nebulae is, and will continue to be, a challenge of high-energy gamma-ray astrophysics. Given that such systems constitute -- by far -- the most numerous expected population in the TeV regime, such characterization is important not only to learn about the sources per se from an individual and population perspective, but also to be able to connect them with observations at other frequencies, especially in radio and X-rays. Also, we need to remove the emission from nebulae in highly confused regions of the sky for revealing other underlying emitters. In this paper we present a new approach for theoretical modelling of pulsar wind nebulae: a hybrid hydrodynamic-radiative model able to reproduce morphological features and spectra of the sources, with relatively limited numerical cost.
