论文标题
带有天体可观察物的旋转黑洞阴影的重访
A revisit of rotating black hole shadow with astrometric observables
论文作者
论文摘要
事件地平线望远镜拍摄的M87银河系中黑洞的第一张图像表明，对超级质量黑洞的定向观察将是测试强力野外状态中一般相对性的一种有希望的方法。为了计算有限距离处的观察者旋转黑洞的阴影，在先前的作品中已经引入了正交四位。但是，人们注意到，不同的四局选择不会导致近区域的观察者的阴影形状相同。在本文中，我们或使用天文观测值的公式来计算相对于这些观察者的一般旋转黑洞的阴影。为了直观，我们还将Kerr-De保姆黑洞视为一个代表性的例子。在这个时空中，Kerr-De Sitter的大小和形状黑洞阴影表示为黑洞和观察者之间距离的函数。预测，阴影的失真会随着距离而增加。
The first image of black hole in M87 galaxy taken by Event Horizon Telescope shows that directed observation of supermassive black holes would be a promising way to test general relativity in strong gravity field regime. In order to calculate shadow of rotating black holes with respect to observers located at finite distance, orthonormal tetrads have been introduced in previous works. However, it is noticed that different choice of tetrads does not lead to the same shape of shadow for observers in near regions. In this paper, we alternatively use formula of astrometric observables for calculating the shadow of a general rotating black hole with respect to these observers. For the sake of intuitive, we also consider Kerr-de Sitter black holes as a representative example. In this space-time, size and shape of Kerr-de Sitter black hole shadows are expressed as functions of distance between the black hole and observer. It is forecasted that the distortion of shadow would increase with distance.
