Post-Keplerian motion in Reissner–Nordström spacetime

Yang, Bo; Lin, Wenbin

doi:10.1007/s10714-019-2597-z

Cited by 9 publications

(5 citation statements)

References 51 publications

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“…Hence, we need only to substitute the asymptotic forms (32) and Eq. ( 42) into the expansion (21) and then further expand these functions for large p. Although can be solved easily, their expressions are too lengthy to present here. Finally, substituting all these coefficients, as well as Eqs.…”

Section: F(u)mentioning

confidence: 99%

“…When determining the PS under pure gravity, most previous studies used essentially a type of PN approximation, i.e., they assumed that the trajectory is far from the center and close to an ellipse [14][15][16][17][18][19][20][21][22][23]. However, when the trajectory is close to the center, particularly when the center is a black hole, such as Sgr A * , high order results that were difficult to obtain using the PN approximation might be required to satisfy the required accuracy.…”

Section: Introductionmentioning

confidence: 99%

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Periapsis shift in spherically symmetric spacetimes and effects of electric interactions*

Wang 王,

Jia 贾

2024

Chinese Phys. C

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The periapsis shift of charged test particles in arbitrary static and spherically symmetric charged spacetimes are studied. Two perturbative methods, the near-circular approximation and post-Newtonian methods, are developed, and shown to be very accurate when the results are found to high orders. The former method is more precise when the eccentricity $e$ of the orbit is small while the latter works better when the orbit semilatus rectum $p$ is large. Results from these two methods are shown to agree with each other when both $e$ is small and $p$ is large. These results are then applied to the Reissner-Nordstr"om spacetime, the Einstein-Maxwell-dilation gravity and a charged wormhole spacetime. The effects of various parameters on the periapsis shift, especially that of the electrostatic interaction, are carefully studied. The periapsis shift data of the solar-Mercury is then used to constrain the charges of the Sun and Mercury, and the data of the Sgr A$^*$-S2 periapsis shift is used to find, for the first time using this method, constraints about the charges of Sgr A$^*$ and S2.

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Section: F(u)mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Periapsis shift in spherically symmetric spacetimes and effects of electric interactions*

Wang 王,

Jia 贾

2024

Chinese Phys. C

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“…For example, Bini, Geralico and Ruffini have investigated the circular motion of a charged test particle in the field of the Reissner-Nordström black hole [38,39]. In our previous work, we have shown that the black hole's electric charge can contribute to the orbital perihelion precession at the 1PN order, but not to the orbital period at the same order [40]. It is interesting to further explore the effects of the black hole's charge on the particle's motion including the orbital perihelion precession and period at the higher PN orders.…”

Section: Introductionmentioning

confidence: 98%

“…Although the charged astronomical bodies have not been discovered, the possibility of their existence in the universe may not be ruled out. In fact, the charge effects of the astrophysical black holes and stars have been studied extensively [32][33][34][35][36][37][38][39][40][41]. For example, Bini, Geralico and Ruffini have investigated the circular motion of a charged test particle in the field of the Reissner-Nordström black hole [38,39].…”

Section: Introductionmentioning

confidence: 99%

The second post-Newtonian motion in Reissner-Nordström spacetime

Yang,

Jiang,

Lin

2022

Preprint

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We derived the second post-Newtonian solution for the quasi-Keplerian motion of a charged test particle in the Reissner-Nordström spacetime under the harmonic coordinates. The solution is formulated in terms of the test particle's orbital energy and angular momentum, both of which are constants at the second post-Newtonian order. The charge effects on the test particle's motion including the orbital period and perihelion precession are displayed explicitly. Our results can be applied to the cases in which the test particle has small charge-to-mass ratio, or the test particle has arbitrary charge-to-mass ratio but the multiplication of the test particle and the gravitational source's charge-to-mass-ratios is much smaller than 1.

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“…In our previous work [57,58], we have derived the quasi-Keplerian motion for the neutral test particle in the Reissner-Nordström spacetime, and that for the charged test particle.…”

Section: Introductionmentioning

confidence: 99%

The quasi-Keplerian motion in the regular Bardeen spacetime

Li¹,

Yang²,

Lin³

2022

Preprint

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The second post-Newtonian solution for the quasi-Keplerian motion of a test particle in the gravitational field of regular Bardeen black hole is derived. The solution is formulated in terms of the test particle's orbital energy and angular momentum, as well as the mass and magnetic charge of the Bardeen black hole. The leading effects of the magnetic charge on the test particle's orbit and motion including perihelion precession are displayed explicitly. In particular, it is shown that to the second post-Newtonian order the magnetic charge does not affect the test particle's orbital period.

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Post-Keplerian motion in Reissner–Nordström spacetime

Cited by 9 publications

References 51 publications

Periapsis shift in spherically symmetric spacetimes and effects of electric interactions*

Periapsis shift in spherically symmetric spacetimes and effects of electric interactions*

The second post-Newtonian motion in Reissner-Nordström spacetime

The quasi-Keplerian motion in the regular Bardeen spacetime

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