Proposes APTA with 6 satellites and 10^{-18} relative clock uncertainty at 1s averaging to achieve sensitivity for observing 10^3-10^4 solar-mass black hole mergers in the decihertz band.
Gravitational Waves from a Compact Star in a Circular, Inspiral Orbit, in the Equatorial Plane of a Massive, Spinning Black Hole, as Observed by LISA
5 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
Results are presented from high-precision computations of the orbital evolution and emitted gravitational waves for a stellar-mass object spiraling into a massive black hole in a slowly shrinking, circular, equatorial orbit. The focus of these computations is inspiral near the innermost stable circular orbit (isco)---more particularly, on orbits for which the angular velocity Omega is 0.03 < Omega/Omega_{isco} < 1. The computations are based on the Teukolsky-Sasaki-Nakamura formalism, and the results are tabulated in a set of functions that are of order unity and represent relativistic corrections to low-orbital-velocity formulas. These tables can form a foundation for future design studies for the LISA space-based gravitational-wave mission. A first survey of applications to LISA is presented: Signal to noise ratios S/N are computed and graphed as functions of the time-evolving gravitational-wave frequency for representative values of the hole's mass M and spin a and the inspiraling object's mass \mu, with the distance to Earth chosen to be r_o = 1 Gpc. These S/N's show a very strong dependence on the black-hole spin, as well as on M and \mu. A comparison with predicted event rates shows strong promise for detecting these waves, but not beyond about 1Gpc if the inspiraling object is a white dwarf or neutron star. This argues for a modest lowering of LISA's noise floor. A brief discussion is given of the prospects for extracting information from the observed waves
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A generic open-source code computes rational/irrational timelike orbits and kludge gravitational-wave strains for static spherically symmetric spacetimes, demonstrated in Schwarzschild.
Joint SKA PTA and astrometry analysis improves gravitational wave background detection sensitivity by 10-50%.
LISA can constrain the Lorentz symmetry breaking parameter ell in bumblebee gravity to O(10^{-4}) uncertainty via EMRI waveform analysis in the AAK framework.
A review of existing waveform models for LISA sources and the challenges that must still be overcome.
citing papers explorer
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Artificial Precision Timing Array: bridging the decihertz gravitational-wave sensitivity gap with clock satellites
Proposes APTA with 6 satellites and 10^{-18} relative clock uncertainty at 1s averaging to achieve sensitivity for observing 10^3-10^4 solar-mass black hole mergers in the decihertz band.
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Rational Orbits and Gravitational Waves in Static Spherical Spacetimes: An Open-Source Numerical Framework
A generic open-source code computes rational/irrational timelike orbits and kludge gravitational-wave strains for static spherically symmetric spacetimes, demonstrated in Schwarzschild.
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Synergies Between Pulsar Timing Array and Astrometry
Joint SKA PTA and astrometry analysis improves gravitational wave background detection sensitivity by 10-50%.
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Constraining Lorentz symmetry breaking in bumblebee gravity with extreme mass-ratio inspirals
LISA can constrain the Lorentz symmetry breaking parameter ell in bumblebee gravity to O(10^{-4}) uncertainty via EMRI waveform analysis in the AAK framework.
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Waveform Modelling for the Laser Interferometer Space Antenna
A review of existing waveform models for LISA sources and the challenges that must still be overcome.