Eccentric self-forced inspirals into a rotating black hole
Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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Eccentric self-forced inspirals into a rotating black hole. / Lynch, Philip; van de Meent, Maarten; Warburton, Niels.
I: Classical and Quantum Gravity, Bind 39, Nr. 14, 145004, 21.07.2022.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Eccentric self-forced inspirals into a rotating black hole
AU - Lynch, Philip
AU - van de Meent, Maarten
AU - Warburton, Niels
PY - 2022/7/21
Y1 - 2022/7/21
N2 - We develop the first model for extreme mass-ratio inspirals (EMRIs) into a rotating massive black hole driven by the gravitational self-force (GSF). Our model is based on an action angle formulation of the method of osculating geodesics for eccentric, equatorial (i.e., spin-aligned) motion in Kerr space-time. The forcing terms are provided by an efficient spectral interpolation of the first-order GSF in the outgoing radiation gauge. We apply a near-identity (averaging) transformation to eliminate all dependence of the orbital phases from the equations of motion, while maintaining all secular effects of the first-order GSF at post-adiabatic order. This implies that the model can be evolved without having to resolve all O(10(5)) orbit cycles of an EMRI, yielding an inspiral model that can be evaluated in less than a second for any mass-ratio. In the case of a non-rotating central black hole, we compare inspirals evolved using self-force data computed in the Lorenz and radiation gauges. We find that the two gauges generally produce differing inspirals with a deviation of comparable magnitude to the conservative self-force correction. This emphasizes the need for including the (currently unknown) dissipative second order self-force to obtain gauge independent, post-adiabatic waveforms.
AB - We develop the first model for extreme mass-ratio inspirals (EMRIs) into a rotating massive black hole driven by the gravitational self-force (GSF). Our model is based on an action angle formulation of the method of osculating geodesics for eccentric, equatorial (i.e., spin-aligned) motion in Kerr space-time. The forcing terms are provided by an efficient spectral interpolation of the first-order GSF in the outgoing radiation gauge. We apply a near-identity (averaging) transformation to eliminate all dependence of the orbital phases from the equations of motion, while maintaining all secular effects of the first-order GSF at post-adiabatic order. This implies that the model can be evolved without having to resolve all O(10(5)) orbit cycles of an EMRI, yielding an inspiral model that can be evaluated in less than a second for any mass-ratio. In the case of a non-rotating central black hole, we compare inspirals evolved using self-force data computed in the Lorenz and radiation gauges. We find that the two gauges generally produce differing inspirals with a deviation of comparable magnitude to the conservative self-force correction. This emphasizes the need for including the (currently unknown) dissipative second order self-force to obtain gauge independent, post-adiabatic waveforms.
KW - extreme mass ratio inspirals
KW - gravitational self force
KW - relativistic celestial mechanics
KW - gravitational waveform modeling
KW - eccentricity
KW - GRAVITATIONAL-RADIATION REACTION
KW - TEUKOLSKY EQUATION
KW - ANALYTIC SOLUTIONS
KW - PERTURBATIONS
KW - WAVES
U2 - 10.1088/1361-6382/ac7507
DO - 10.1088/1361-6382/ac7507
M3 - Journal article
VL - 39
JO - Classical and Quantum Gravity
JF - Classical and Quantum Gravity
SN - 0264-9381
IS - 14
M1 - 145004
ER -
ID: 334655406