相对和绝对恒星像差

Miloš Čojanović
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引用次数: 0

摘要

如果我们谈论恒星像差,那么我们会想到布拉德利首先发现并解释的恒星像差的形式。除了布拉德利的恒星像差,它也可以被定义为相对恒星像差,我们将定义绝对恒星像差仅基于一个测量。在这里,我们将把绝对恒星像差称为$ASA$。我们将试图用几句话解释为什么有必要以这种方式测量和解释恒星像差。假设我们在六个月内对多普勒效应进行了两次测量。如果我们不知道这些测量的结果,而只知道它们之间的差异,那么我们就无法确定观察者相对于恒星运动的径向速度。我们将证明类似的推理可以应用于布拉德利定义的恒星像差的情况。只知道两种恒星像差测量值之间的差异,我们不能确定观察者相对于视线移动的横向速度,而只能确定它们的差异。利用ASA的测量结果,我们将确定一个参考惯性系,然后推导出相对和绝对恒星像差的公式。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Relative and Absolute Stellar Aberration
If we talk about Stellar Aberration, then we think of the form of Stellar Aberration that was first discovered and explained by Bradley. In addition to Bradley's Stellar Aberration, which can also be defined as Relative Stellar Aberration, we will define Absolute Stellar Aberration based on just one measurement. Here after we will refer to the Absolute Stellar Aberration as $ASA$. We will try to explain in a few words why it is necessary to measure and interpret Stellar Aberration in this way. Suppose we performed two measurements of the Doppler Effect within six months. If we don't know the results of those measurements, but only difference between them, then we cannot determine the radial velocities with which the observer moves with respect to the star. We will prove that similar reasoning can be applied in the case of Stellar Aberration as defined by Bradley. Knowing only the difference between the two measurements of the Stellar Aberration, we are not able to determine the transverse velocities the observer moves with respect to the line of sight, but only their difference. Using the results of $ASA$ measurements, we will determine a Reference Inertial Frame and after that derive formulas for Relative and Absolute Stellar Aberration.
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