Motion of test particle in rotating boson star

Zhang, Yupeng; Zeng, Yan-Bo; 王, 永强; Wei, Shao-Wen; Liu, Yu-Xiao

doi:10.1103/physrevd.105.044021

Cited by 5 publications

(2 citation statements)

References 64 publications

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“…We have obtained the effective potential (45) of the spinning test particle with the four-momentum pointing toward future and shown that it is dependent on the spin and angular momenta of the test particle. It can be shown that when the particle spin is zero, the effective potential is the same as that of the point particle [38].…”

Section: Effective Potentials and Orbitsmentioning

confidence: 99%

“…Note that, a boson star is everywhere regular and there is no phenomenon that a test particle plunges into the event horizon of a black hole. Such properties ensure that novel orbits will be obtained in the backgrounds of boson stars [10,[35][36][37][38][39]. For example, a test particle with zero orbital angular momentum can pass through the center of the boson star.…”

Section: Introductionmentioning

confidence: 99%

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Equatorial orbits of spinning test particles in rotating boson stars

et al. 2022

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In this paper, we study circular orbits of spinning test particles in the background of a rotating boson star. Using the pole-dipole approximation and neglecting the back-reaction of the spinning test particle on the spacetime, the equation of motion of the spinning test particle is described by the Mathisson–Papapetrou–Dixon equation. We solve this equation under the Tulczyjew spin-supplementary condition and obtain the four-momentum and four-velocity of the spinning test particle. Quite different from the spinless particle, the effective potential of the spinning particle with zero orbital angular momentum goes to infinite at the center of the rotating boson star. This will lead to the fact that the spinning particle can not pass through the center of the boson star. However, when the spin angular momentum and orbital angular momentum satisfy $$2{\bar{s}}+{\bar{l}}=0$$ 2 s ¯ + l ¯ = 0 , the effective potential is not divergent anymore and the spinning particle can pass through the center of the rotating boson star. We still investigate how the spin affects the structure of the circular orbits and we find that the spin will induce the larger or smaller regions of no circular orbits, unstable circular orbits, and stable circular orbits. Moreover, the radius and energy of the circular orbit will be decreased or increased by the particle spin. These results will have an important application in testing the gravitational waves in the boson star background.

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Section: Effective Potentials and Orbitsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Equatorial orbits of spinning test particles in rotating boson stars

et al. 2022

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Experimental studies of black holes: status and future prospects

Genzel,

Eisenhauer,

Gillessen

2024

Astron Astrophys Rev

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More than a century ago, Albert Einstein presented his general theory of gravitation (GR) to the Prussian Academy of Sciences. One of the predictions of the theory is that not only particles and objects with mass, but also the quanta of light, photons, are tied to the curvature of space-time, and thus to gravity. There must be a critical compactness, above which photons cannot escape. These are black holes (henceforth BH). It took 50 years after the theory was announced before possible candidate objects were identified by observational astronomy. And another 50 years have passed, until we finally have in hand detailed and credible experimental evidence that BHs of 10 to $$10^{10}$$ 10 10 times the mass of the Sun exist in the Universe. Three very different experimental techniques, but all based on Michelson interferometry or Fourier-inversion spatial interferometry have enabled the critical experimental breakthroughs. It has now become possible to investigate the space-time structure in the vicinity of the event horizons of BHs. We briefly summarize these interferometric techniques, and discuss the spectacular recent improvements achieved with all three techniques. Finally, we sketch where the path of exploration and inquiry may go on in the next decades.

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Dynamical boson stars

Liebling

Palenzuela

2023

Living Rev Relativ

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The idea of stable, localized bundles of energy has strong appeal as a model for particles. In the 1950s, John Wheeler envisioned such bundles as smooth configurations of electromagnetic energy that he called geons, but none were found. Instead, particle-like solutions were found in the late 1960s with the addition of a scalar field, and these were given the name boson stars. Since then, boson stars find use in a wide variety of models as sources of dark matter, as black hole mimickers, in simple models of binary systems, and as a tool in finding black holes in higher dimensions with only a single Killing vector. We discuss important varieties of boson stars, their dynamic properties, and some of their uses, concentrating on recent efforts.

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Motion of test particle in rotating boson star

Cited by 5 publications

References 64 publications

Equatorial orbits of spinning test particles in rotating boson stars

Equatorial orbits of spinning test particles in rotating boson stars

Experimental studies of black holes: status and future prospects

Dynamical boson stars

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