Light deflection in the post-linear gravitational field of bounded point-like masses
Light deflection in the post-linear gravitational field of bounded point-like masses
复制标题
有界点状质量的后线性引力场中的光偏转
DOI：
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发表时间：
2005
期刊：
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通讯作者：
Michael H. Brugmann
中科院分区：
文献类型：
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作者：
Michael H. Brugmann
本文讨论了两个有界点状质量的后线性引力fi场中的光De-De-Position问题。假定光源和观测者都位于空间中的渐近fifl中。在G/c2中，光传输方程被显式积分到二阶。一些积分是利用相对分离距离与碰撞参数之比(r12/ξ)的幂展开来计算的。讨论了在G/C~2展开式中必须保留哪些阶次。结果表明，在给定的阶数下，本文得到的光学角的表达式与Kopeikin和fl的公式完全等价。对于最初垂直于具有相同质量的双星的轨道平面传播的光线，Defl对射角具有特别简单的形式。对双脉冲星PSRJ0737-3039Defl角公式的应用表明，当撞击参数fi比双星各分量的相对间隔距离大5倍时，约10−6角秒的EPSTEIN-Shapiro光对射角的修正范围在10 PSR7到10 PSR8角之间。
Light deflection in the post-linear gravitational field of two bounded point-like masses is treated. Both the light source and the observer are assumed to be located at infinity in an asymptotically flat space. The equations of light propagation are explicitly integrated to the second order in G/c 2 . Some of the integrals are evaluated by making use of an expansion in powers of the ratio of the relative separation distance to the impact parameter ( r 12 /ξ ). A discussion of which orders must be retained to be consistent with the expansion in terms of G/c 2 is given. It is shown that the expression obtained in this paper for the angle of light deflection is fully equivalent to the expression obtained by Kopeikin and Sch¨afer up to the order given there. The deflection angle takes a particularly simple form for a light ray originally propagating orthogonal to the orbital plane of a binary with equal masses. Application of the formulae for the deflection angle to the double pulsar PSR J0737-3039 for an impact parameter five times greater than the relative separation distance of the binary’s components shows that the corrections to the Epstein-Shapiro light deflection angle of about 10 − 6 arcsec lie between 10 − 7 and 10 − 8 arcsec.