Numerical and analytic modeling of boson star-black hole systems in the nonrelativistic limit, with Fisher analysis indicating LISA sensitivity to ultralight dark matter mass and self-coupling via gravitational wave dephasing.
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LISA Capture Sources: Approximate Waveforms, Signal-to-Noise Ratios, and Parameter Estimation Accuracy
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abstract
Captures of stellar-mass compact objects (COs) by massive ($\sim 10^6 M_\odot$) black holes (MBHs) are potentially an important source for LISA, the proposed space-based gravitational-wave (GW) detector. The orbits of the inspiraling COs are highly complicated; they can remain rather eccentric up until the final plunge, and display extreme versions of relativistic perihelion precession and Lense-Thirring precession of the orbital plane. The strongest capture signals will be ~10 times weaker than LISA's instrumental noise, but in principle (with sufficient computing power) they can be disentangled from the noise by matched filtering. The associated template waveforms are not yet in hand, but theorists will very likely be able to provide them before LISA launches. Here we introduce a family of approximate (post-Newtonian) capture waveforms, given in (nearly) analytic form, for use in advancing LISA studies until more accurate versions are available. Our model waveforms include most of the key qualitative features of true waveforms, and cover the full space of capture-event parameters (including orbital eccentricity and the MBH's spin). Here we use our approximate waveforms to (i) estimate the relative contributions of different harmonics (of the orbital frequency) to the total signal-to-noise ratio, and (ii) estimate the accuracy with which LISA will be able to extract the physical parameters of the capture event from the measured waveform. For a typical source (a $10 M_\odot$ CO captured by a $10^6 M_\odot$ MBH at a signal-to-noise ratio of 30), we find that LISA can determine the MBH and CO masses to within a fractional error of $\sim 10^{-4}$, measure $S/M^2$ (where $S$ and $M$ are the MBH's mass and spin) to within $\sim 10^{-4}$, and determine the sky location of the source to within $\sim 10^{-3}$ stradians.
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representative citing papers
A neural-network-accelerated hierarchical Bayesian pipeline is developed and validated on a phenomenological model to constrain EMRI population parameters from LISA data.
Neglecting transient orbital resonances in EMRIs causes significant SNR losses and biases in recovered parameters, with the sign and amplitude of resonance-induced changes to integrals of motion being critical.
LISA EMRIs can constrain deviations from Kerr equatorial symmetry to 10^{-2} and axial symmetry to 10^{-3} using Analytic Kludge waveforms and Fisher analysis.
LISA can constrain non-axisymmetric mass quadrupole deformations at the 10^{-3} level and axisymmetric mass octupole deformations at the 10^{-2} level in EMRI signals to test fuzzball proposals.
Periodic orbits around a non-rotating Destounis-Suvorov-Kokkotas black hole are taxonomized with integer triplets and their gravitational waveforms are calculated, showing that large deformations eliminate circular orbits and modify wave signals.
The quantum parameter ξ in an asymptotically safe regular black hole shifts the innermost stable orbit, enhances whirl behavior in periodic geodesics, and produces amplitude-modulated millihertz gravitational-wave strains whose peak amplitude grows with ξ, placing them inside the sensitivity bands预计
EMRI waveforms in bumblebee gravity allow LISA to constrain the Lorentz symmetry breaking parameter ell at the level of O(10^{-4}).
EMRI waveforms in a rotating black hole with Dehnen DM halo show amplitude and phase shifts from Kerr, with mismatch rising as DM mass parameter and black hole spin increase.
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Boson Stars Hosting Black Holes
Numerical and analytic modeling of boson star-black hole systems in the nonrelativistic limit, with Fisher analysis indicating LISA sensitivity to ultralight dark matter mass and self-coupling via gravitational wave dephasing.
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Constraints on the extreme mass-ratio inspiral population from LISA data
A neural-network-accelerated hierarchical Bayesian pipeline is developed and validated on a phenomenological model to constrain EMRI population parameters from LISA data.
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Parameter-estimation bias induced by transient orbital resonances in extreme-mass-ratio inspirals
Neglecting transient orbital resonances in EMRIs causes significant SNR losses and biases in recovered parameters, with the sign and amplitude of resonance-induced changes to integrals of motion being critical.
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Probing Kerr Symmetry Breaking with LISA Extreme-Mass-Ratio Inspirals
LISA EMRIs can constrain deviations from Kerr equatorial symmetry to 10^{-2} and axial symmetry to 10^{-3} using Analytic Kludge waveforms and Fisher analysis.
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Are Black Holes Fuzzballs? Probing Horizon-Scale Structure with LISA
LISA can constrain non-axisymmetric mass quadrupole deformations at the 10^{-3} level and axisymmetric mass octupole deformations at the 10^{-2} level in EMRI signals to test fuzzball proposals.
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Taxonomy of periodic orbits and gravitational waves in a non-rotating Destounis-Suvorov-Kokkotas black hole spacetime
Periodic orbits around a non-rotating Destounis-Suvorov-Kokkotas black hole are taxonomized with integer triplets and their gravitational waveforms are calculated, showing that large deformations eliminate circular orbits and modify wave signals.
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Probing Gravitational Wave Signatures from Periodic Orbits of Regular Black Holes in Asymptotically Safe Gravity
The quantum parameter ξ in an asymptotically safe regular black hole shifts the innermost stable orbit, enhances whirl behavior in periodic geodesics, and produces amplitude-modulated millihertz gravitational-wave strains whose peak amplitude grows with ξ, placing them inside the sensitivity bands预计
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Constraining Lorentz symmetry breaking in bumblebee gravity with extreme mass-ratio inspirals
EMRI waveforms in bumblebee gravity allow LISA to constrain the Lorentz symmetry breaking parameter ell at the level of O(10^{-4}).
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Gravitational waves of extreme-mass-ratio inspirals in a rotating black hole with Dehnen dark matter halo
EMRI waveforms in a rotating black hole with Dehnen DM halo show amplitude and phase shifts from Kerr, with mismatch rising as DM mass parameter and black hole spin increase.
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