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_papers/Zhu:2024dyl.md

@@ -1,5 +1,5 @@
 ---
-title: "Imprints of Changing Mass and Spin on Black Hole Ringdown"
+title: "Imprints of changing mass and spin on black hole ringdown"
 authors:
   - "Zhu, Hengrui"
   - "Pretorius, Frans"
@@ -12,31 +12,35 @@ authors:
   - "Pfeiffer, Harald P."
   - "Scheel, Mark A."
   - "Stein, Leo C."
-jref:
-doi:
+jref: "Phys.Rev.D 110, 124028 (2024)"
+doi: "10.1103/PhysRevD.110.124028"
 date: 2024-04-18
 arxiv: "2404.12424"
-used_spec: true
 abstract: |
   We numerically investigate the imprints of gravitational radiation-
-  reaction driven changes to a black hole's mass and spin on the
+  reaction driven changes to a black hole’s mass and spin on the
   corresponding ringdown waveform. We do so by comparing the dynamics
   of a perturbed black hole evolved with the full (nonlinear) versus
   linearized Einstein equations. As expected, we find that the
   quasinormal mode amplitudes extracted from nonlinear evolution
   deviate from their linear counterparts at third order in initial
   perturbation amplitude. For perturbations leading to a change in the
-  black hole mass and spin of \(\sim 5\%\), which is reasonable for a
-  remnant formed in an astrophysical merger, we find that nonlinear
-  distortions to the complex amplitudes of some quasinormal modes can
-  be as large as \(\sim 50\%\) at the peak of the waveform. Furthermore,
-  the change in the mass and spin results in a drift in the
-  quasinormal mode frequencies, which for large amplitude
-  perturbations causes the nonlinear waveform to rapidly dephase with
-  respect to its linear counterpart. %These two nonlinear effects
-  together create a large distortion in both the amplitude and phase
-  of the ringdown gravitational waveform. Surprisingly, despite these
-  nonlinear effects creating significant deviations in the nonlinear
-  waveform, we show that a linear quasinormal mode model still
-  performs quite well from close to the peak amplitude onwards.
+  black hole mass and spin of <math
+  display="inline"><mo>∼</mo><mn>5</mn><mo>%</mo></math>, which is
+  reasonable for a remnant formed in an astrophysical merger, we find
+  that nonlinear distortions to the complex amplitudes of some
+  quasinormal modes can be as large as <math
+  display="inline"><mo>∼</mo><mn>50</mn><mo>%</mo></math> at the peak
+  of the waveform. Furthermore, the change in the mass and spin
+  results in a drift in the quasinormal mode frequencies, which for
+  large amplitude perturbations causes the nonlinear waveform to
+  rapidly dephase with respect to its linear counterpart.
+  Surprisingly, despite these nonlinear effects creating significant
+  deviations in the nonlinear waveform, we show that a linear
+  quasinormal mode model still performs quite well from close to the
+  peak amplitude onward. Comparing the quality of quasinormal mode
+  fits for the linear and nonlinear waveforms, we show that the main
+  obstruction to measuring high-<math
+  display="inline"><mi>n</mi></math> overtones is the transient part
+  of the waveform, already present at the linear level.
 ---