Influence of the gravitational deflection of light on the time of occultation of a star by the moon

1968 ◽  
Vol 55 (2) ◽  
pp. 587-590
Author(s):  
M. Rudkjøbing
Keyword(s):  
The Moon ◽  
Deflection Of Light ◽  
Gravitational Deflection Of Light ◽  
Gravitational Deflection

scholarly journals The Gravitational Deflection of Light in f(R)-Gravity

2014 ◽  
Vol 53 (6) ◽  
pp. 1947-1952 ◽  
Author(s):  
Long Huang ◽  
Feng He ◽  
Hai Huang ◽  
Min Yao
Keyword(s):  
Deflection Of Light ◽  
Gravitational Deflection Of Light ◽  
Gravitational Deflection

scholarly journals Relativistic effect of gravitational deflection of light in binary pulsars

1996 ◽  
Vol 160 ◽  
pp. 131
Author(s):  
Oleg V. Doroshenko ◽  
Sergei M. Kopeikin
Keyword(s):  
Gravitational Field ◽  
Strong Field ◽  
Alternative Theories Of Gravity ◽  
Estimation Of Parameters ◽  
Orbital Inclination ◽  
Binary Pulsars ◽  
Deflection Of Light ◽  
Shapiro Effect ◽  
Gravitational Deflection Of Light ◽  
Gravitational Deflection

Timing formula for data processing of observations of binary pulsars that accounts for the relativistic deflection of light in the gravitational field of the pulsar’s companion is presented, and the measurability of this effect along with its variance estimates is discussed. The deflection of the pulsar’s pulse trajectory in the gravitational field of its companion leads to variation in the pulsar’s rotational phase. This variation appears as a narrow sharp growth of the magnitude of the post-fit residuals in the vicinity of the moment of the superior conjunction of the pulsar with its companion. In contrast to the relativistic Shapiro effect, the amplitude of the effect of gravitational deflection of the pulsar radio beam has two peaks with opposite signs, which become sharper as the inclinationiof the pulsar’s orbit approaches to the right angle. The effect under consideration influences the estimation of parameters of the relativistic Shapiro effect in the binary pulsars with nearly edgewise orbits. Its inclusion in the fitting procedure provides a more careful measurement of the sine of the orbital inclinationi, as well as the masses of the pulsar and its companion. This permits an improved testing of alternative theories of gravity in the strong field regime. The effect of the gravitational deflection of light has been numerically investigated for binary pulsars with nearly edgewise orbits. It is shown that the effect is observed in general only when cosi is less than 0.003. This estimate becomes less restrictive as the pulsar’s spin axis approaches the line of sight.

scholarly journals Deflection of Light Ray Due to a Charged Body Using Material Medium Approach

2017 ◽  
Vol 72 (12) ◽  
pp. 1113-1126 ◽  
Author(s):  
Saswati Roy ◽  
A.K. Sen
Keyword(s):  
Field Approximation ◽  
Weak Field ◽  
Test Case ◽  
Spherically Symmetric ◽  
Theory Of Relativity ◽  
General Theory Of Relativity ◽  
Material Medium ◽  
Deflection Of Light ◽  
Gravitational Deflection Of Light ◽  
Gravitational Deflection

AbstractThe gravitational deflection of light ray is an important prediction of general theory of relativity. In this paper we have developed an analytical expression of the deflection of light ray without any weak field approximation due to a charged gravitating body represented by Reissner-Nordström (RN) and Janis-Newman-Winicour (JNW) space-time geometry, using material medium approach. It is concluded that although both the geometries represent the charged, non-rotating, spherically symmetric gravitating body, the effect of charge on the gravitational deflection is just opposite to each other. The gravitational deflection decreases with charge in the RN geometry and increases with charge in the JNW geometry. The calculations obtained here are compared with other methods done by different authors. The formalism is applied to an arbitrarily selected gravitating body, as a test case and compared with the standard Schwarzschild geometry for comparison purposes.

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