Timeline for Extreme Mass Ratio Inspirals and GWs cycles
Current License: CC BY-SA 4.0
9 events
| when toggle format | what | by | license | comment | |
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| Jun 26 at 15:37 | vote | accept | RKerr | ||
| Jun 26 at 15:37 | comment | added | RKerr | Thank you very much! | |
| Jun 26 at 15:18 | history | edited | TimRias | CC BY-SA 4.0 |
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| Jun 26 at 15:15 | comment | added | TimRias | I've added the plot to the post above. The "late inspiral" regime keeps shrinking with increasing PN order until it essentially vanishes at 21.5PN order. Note that as we look further in the strong field regime there is no discernible improvement from going to higher PN order at $r=4GM/c^2$. This is a problem when we consider binaries with spins, which have a much smaller LSO. | |
| Jun 26 at 15:10 | history | edited | TimRias | CC BY-SA 4.0 |
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| Jun 26 at 13:16 | comment | added | RKerr | Thank you! I apologize if I am being bothersome, but I am having trouble reproducing results using Mathematica and the BlackHolePerturbationToolkit. Could you please post the figure using the public data? | |
| Jun 26 at 11:59 | comment | added | TimRias | It is not clear that adding more PN terms would lead to an improvement due to the asymptotic nature of the PN series. You can probably improve at least a bit though. The 5.5PN statement came from private data, but you should be able to reproduce it from public data from the black hole perturbation toolkit, which has numerical flux data: github.com/BlackHolePerturbationToolkit/… and data of the corresponding PN expressions and data for the corresponding PN approximations: bhptoolkit.org/PostNewtonianSelfForce | |
| Jun 26 at 8:20 | comment | added | RKerr | Thank you very much for your detailed answer! I have two more questions: Is it possible to further model the late inspiral phase by incorporating additional PN terms? Could you provide a reference for the relative error in the 5.5PN flux? Thank you again! | |
| Jun 26 at 7:26 | history | answered | TimRias | CC BY-SA 4.0 |