dc.contributor.author |
Prerna Rana |
|
dc.contributor.author |
Mangalam, A |
|
dc.date.accessioned |
2023-02-02T08:54:06Z |
|
dc.date.available |
2023-02-02T08:54:06Z |
|
dc.date.issued |
2022 |
|
dc.identifier.citation |
The Fifteenth Marcel Grossmann Meeting on General Relativity, edited by Elia S. Battistelli, Robert T. Jantzen and Remo Ruffini, pp. 858-864 |
en_US |
dc.identifier.isbn |
9789811258251 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/8133 |
|
dc.description |
Open Access |
en_US |
dc.description |
This is an Open Access volume published by World Scientific Publishing Company. It is distributed under the terms of the Creative Commons Attribution-Non Commercial 4.0 (CC BY-NC) License. Further distribution of this work is permitted, provided the original work is properly cited. |
|
dc.description.abstract |
We derive the conditions for a non-equatorial eccentric bound orbit to exist around a Kerrblack hole in two-parameter spaces: the energy, angular momentum of the test particle,spin of the black hole, and Carter’s constant space (E,L,a,Q), and eccentricity, inverse-latus rectum space (e,μ,a,Q). These conditions distribute various kinds of bound orbitsin different regions of the (E,L)and(e,μ) planes, depending on which pair of rootsof the effective potential forms a bound orbit. We provide a prescription to select theseparameters for bound orbits, which are useful inputs to study bound trajectory evolutionin various astrophysical applications like simulations of gravitational wave emission fromextreme-mass ratio inspirals, relativistic precession around black holes, and the study ofgyroscope precession as a test of general relativity |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
World Scientific Publishing |
en_US |
dc.relation.uri |
https://doi.org/10.1142/9789811258251_0116 |
|
dc.rights |
© World Scientific Publishing |
|
dc.subject |
Classical black holes |
en_US |
dc.subject |
Relativity and Gravitation |
en_US |
dc.subject |
Bound orbit trajectories |
en_US |
dc.title |
Bound orbit domains in the phase space of the Kerr geometry |
en_US |
dc.type |
Article |
en_US |