The Pioneer anomaly in covariant theory of gravitation

Sergey G Fedosin

doi:10.1139/cjp-2015-0134

Abstract

The difference of equations of motion in the covariant theory of gravitation and in the general theory of relativity is used to explain the Pioneer anomaly. Calculation shows that the velocities of a spacecraft in both theories at equal distances can differ by several centimetres per second. This leads also to a possible explanation of the flyby anomaly and comet disturbances, which are not taken into account by the general theory of relativity.

Highlights

The story of the American spacecrafts Pioneer and Pioneer began on March 2, 1972, and, respectively, on April 6, 1973, at the time of their launch
The covariant theory of gravitation (CTG) is an alternative theory for general theory of relativity (GTR) and we present further CTG approach to the problem of the Pioneer anomaly by comparing of calculations of CTG and GTR
As a result the gravitational field does not create the metric similar to electromagnetic field in equation for the metric, and the metric tensor is calibrated with the help of Newton's law of universal gravitation

Summary

Introduction

The story of the American spacecrafts Pioneer and Pioneer began on March 2, 1972, and, respectively, on April 6, 1973, at the time of their launch. Both spacecrafts passed in the plane of the ecliptic the entire Solar system in two opposite directions, passing close to different planets. Starting from the distance of about 20 a.u., when in the Doppler signal from Pioneer 10 the shift of the speed significantly decreased, caused by the pressure of the solar plasma on the spacecraft, after taking into account all other possible causes of acceleration, the residual signal from the spacecraft started to show the presence of an anomalous acceleration towards the Sun, of the order of 8·10–10 m/s2 [1]. Https://mc06.manuscriptcentral.com/cjp-pubs and for the functions B, K , E we assume that they are the functions only of the radial coordinate r as the distance from the center of the massive body (where we placed the origin) to the observation point, located outside the body

M r 2 c4

B GM sinφ r2 dt dτ

A1 βG2 M 2

A4 for radial motion we have:

G M c2

Conclusion