2013/07/10 by Ioannis Haranas, Haranas, Ioannis, O. Ragos +4
Earth and Planetary Sciences · Physics and Astronomy · #Earth and Planetary Astrophysics (astro-ph.EP) #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #Geophysics and Gravity Measurements #Pulsars and Gravitational Waves Research #Solar and Space Plasma Dynamics #astro-ph.EP #gr-qc
paper · pdf · doi:10.48550/arxiv.1307.2935
12 pages, 5 Figures
arxiv created 2013/07/10 · openalex publication_date 2013/07/10 · arxiv updated 2013/07/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In the weak field and slow motion approximation, the general relativistic field equations are linearized, resembling those of the electromagnetic theory. In a way analogous to that of a moving charge generating a magnetic field, a mass energy current can produce a gravitomagnetic field. In this contribution, the motion of a secondary celestial body is studied under the influence of the gravitomagnetic force generated by a spherical primary. More specifically, two equations are derived to approximate the periastron time rate of change and its total variation over one revolution (i.e., the difference between the anomalistic period and the Keplerian period). Kinematically, this influence results to an apsidal motion. The aforementioned quantities are numerically estimated for Mercury, the companion star of the pulsar PSR 1913 plus 16, the companion planet of the star HD 80606 and the artificial Earth satellite GRACE A. The case of the artificial Earth satellite GRACE A is also considered, but the results present a low degree of reliability from a practical standpoint.