A5058669988- Pulsars and Gravitational Waves Research
- Astrophysical Phenomena and Observations
- Gamma-ray bursts and supernovae
- Black Holes and Theoretical Physics
- Astrophysics and Cosmic Phenomena
- Cosmology and Gravitation Theories
- Geophysics and Sensor Technology
- Geophysics and Gravity Measurements
- Relativity and Gravitational Theory
- Cold Atom Physics and Bose-Einstein Condensates
- High-pressure geophysics and materials
- Superconducting Materials and Applications
- Radio Astronomy Observations and Technology
- Biofield Effects and Biophysics
- Earth Systems and Cosmic Evolution
- Stellar, planetary, and galactic studies
- Atomic and Subatomic Physics Research
- Particle physics theoretical and experimental studies
- Ophthalmology and Eye Disorders
- Seismology and Earthquake Studies
- Advanced MRI Techniques and Applications
- Advanced Differential Geometry Research
- Geomagnetism and Paleomagnetism Studies
- Advanced Thermodynamic Systems and Engines
- Astro and Planetary Science
University College Dublin
2015-2024
Laboratoire des 2 Infinis Toulouse
2023
Massachusetts Institute of Technology
2015-2016
University of Southampton
2010-2013
We propose a space-based interferometer surveying the gravitational wave (GW) sky in milli-Hz to $\mu$-Hz frequency range. By 2040s', band, bracketed between Laser Interferometer Space Antenna (LISA) and pulsar timing arrays, will constitute largest gap coverage of astrophysically relevant GW spectrum. Yet many outstanding questions related astrophysics cosmology are best answered by observations this band. show that detector be truly overarching observatory for scientific community at...
The gravitational-wave astronomical revolution began in 2015 with LIGO's observation of the coalescence two stellar-mass black holes. Over coming decades, ground-based detectors like laser interferometer observatory (LIGO), Virgo and KAGRA will extend their reach, discovering thousands binaries. In 2030s, space-based space antenna (LISA) enable observations massive holes galactic centres. Between observatories LISA lies unexplored dHz frequency band. Here, we show potential a decihertz (DO)...
We produce gravitational waveforms for nonspinning compact binaries undergoing a quasicircular inspiral. Our approach is based on two-timescale expansion of the Einstein equations in second-order self-force theory, which allows first-principles waveform production tens milliseconds. Although designed extreme mass ratios, our agree remarkably well with those from full numerical relativity, even comparable-mass systems. results will be invaluable accurately modeling extreme-mass-ratio...
We present results from calculations of the orbital evolution in eccentric binaries nonrotating black holes with extreme mass-ratios. Our inspiral model is based on method osculating geodesics, and first to incorporate full gravitational self-force (GSF) effect, including conservative corrections. The GSF information encapsulated an analytic interpolation formula numerical data for over a thousand sample geodesic orbits. assess importance corrections waveform models gravitational-wave searches.
Self-force theory is the leading method of modeling extreme-mass-ratio inspirals (EMRIs), key sources for gravitational-wave detector LISA. It well known that an accurate EMRI model, second-order self-force effects are critical, but calculations these have been beset by obstacles. In this Letter we present first implementation a complete scheme computations, specialized to case quasicircular orbits about Schwarzschild black hole. As demonstration, calculate gravitational binding energy binaries.
The future space mission LISA will observe a wealth of gravitational-wave sources at millihertz frequencies. Of these, the extreme-mass-ratio inspirals compact objects into massive black holes are only that combine challenges strong-field complexity with long-lived signals. Such signals found and characterized by comparing them against large number accurate waveform templates during data analysis, but rapid generation such is hindered computing $\sim10^3$-$10^5$ harmonic modes in fully...
We compute adiabatic waveforms for extreme mass-ratio inspirals (EMRIs) by "stitching" together a long inspiral waveform from sequence of snapshots, each which corresponds to particular geodesic orbit. show that the complicated total can be regarded as sum "voices." Each voice evolves in simple way on timescales, property exploited efficiently produce models faithfully encode properties EMRI systems. look at examples range different orbital geometries: spherical orbits, equatorial eccentric...
We model the inspiral of a compact stellar-mass object into massive nonrotating black hole including all dissipative and conservative first-order-in-the-mass-ratio effects on orbital motion. The techniques we develop allow inspirals with initial eccentricities as high $e\sim0.8$ separations large $p\sim 50$ to be evolved through many thousands orbits up onset plunge hole. is computed using an osculating elements scheme driven by hybridized self-force model, which combines Lorenz-gauge...
Within the framework of self-force theory, we compute gravitational-wave energy flux through second order in mass ratio for compact binaries quasicircular orbits. Our results are consistent with post-Newtonian calculations weak field, and they agree remarkably well numerical-relativity simulations comparable-mass strong field. We also find good agreement a spinning secondary or slowly primary. key accurately modeling extreme-mass-ratio inspirals will be useful intermediate-mass-ratio systems.
Black holes are unique among astrophysical sources: they the simplest macroscopic objects in Universe, and extraordinary terms of their ability to convert energy into electromagnetic gravitational radiation. Our capacity probe nature is limited by sensitivity our detectors. The LIGO/Virgo interferometers gravitational-wave equivalent Galileo's telescope. first few detections represent beginning a long journey exploration. At current pace technological progress, it reasonable expect that...
We present the first systematic comparison between gravitational waveforms emitted by inspiralling, quasi-circular and nonspinning black hole binaries computed with three different approaches: second-order self-force (2GSF) theory, as implemented in 1PAT1 model; numerical relativity (NR), SXS collaboration; effective one body (EOB) formalism, TEOBResumS waveform model. To compare models we use both a standard, time-domain alignment gauge-invariant analysis based on dimensionless function...
We leverage recent breakthrough calculations using second-order gravitational self-force (2GSF) theory to improve both the gravitational-mode amplitudes and radiation-reaction force in effective-one-body (EOB) waveform models. achieve this by introducing new calibration parameters SEOBNRv5HM mode amplitudes, matching them newly available 2GSF energy-flux multipolar data for quasicircular nonspinning binary black holes. find that significantly improves energy flux, when compared with...
We investigate the impact of postadiabatic (1PA) terms on parameter estimation for extreme and intermediate mass-ratio inspirals using state-of-the-art waveform models. Our analysis is first to employ Bayesian inference assess systematic errors 1PA waveforms. find that neglecting introduces significant biases (small) mass ratio $\ensuremath{\epsilon}\ensuremath{\gtrsim}{10}^{\ensuremath{-}5}$ quasi circular orbits in Schwarzschild spacetime, which can be mitigated with resummed 3PN...
Extreme Mass Ratio Inspirals (EMRIs) are one of the key sources for future space-based gravitational wave interferometers. Measurements EMRI waves expected to determine characteristics their with sub-percent precision. However, waveform generation is challenging due long duration signal and high harmonic content. Here, we present first ready-to-use Schwarzschild eccentric implementation in frequency domain use either graphics processing units (GPUs) or central (CPUs). We overall test...
We calculate the effect of self-interaction on ``geodetic'' spin precession a compact body in strong-field orbit around black hole. Specifically, we consider angle $\ensuremath{\psi}$ per radian orbital revolution for particle carrying mass $\ensuremath{\mu}$ and $s\ensuremath{\ll}(G/c){\ensuremath{\mu}}^{2}$ circular Schwarzschild hole $M\ensuremath{\gg}\ensuremath{\mu}$. compute through $\mathcal{O}(\ensuremath{\mu}/M)$ perturbation theory, i.e, including correction...
For a self-gravitating particle of mass $\ensuremath{\mu}$ in orbit around Kerr black hole $M\ensuremath{\gg}\ensuremath{\mu}$, we compute the $\mathcal{O}(\ensuremath{\mu}/M)$ shift frequency innermost stable circular equatorial due to conservative piece gravitational self-force acting on particle. Our treatment is based Hamiltonian formulation dynamics terms geodesic motion certain locally defined effective smooth spacetime. We recover same result using so-called first law binary...
We compute the radiation emitted by a particle on innermost stable circular orbit of rapidly spinning black hole both (a) analytically, working to leading order in deviation from extremality and (b) numerically, with new high-precision Teukolsky code. find excellent agreement between two methods. confirm previous estimates overall scaling power radiated, but show that there are also small oscillations all way extremality. Furthermore, we reveal an intricate mode-by-mode structure flux...
We extend the gravitational self-force approach to encompass `self-interaction' tidal effects for a compact body of mass $\mu$ on quasi-circular orbit around black hole $M \gg \mu$. Specifically, we define and calculate at $O(\mu)$ (conservative) shifts in eigenvalues electric- magnetic-type tensors, (dissipative) shift scalar product between their eigenbases. This yields four gauge-invariant functions, from which one may construct other quantities such as curvature scalars speciality index....
Black hole spacetimes, like the Kerr spacetime, admit both stable and plunging orbits, separated in parameter space by separatrix. Determining location of separatrix is fundamental interest understanding black holes, crucial importance for modeling extreme-mass-ratio inspirals. Previous numerical approaches to locating were not always efficient or across all space. In this paper we show that zero set a single polynomial This gives two main results. First, thoroughly analyze special cases...
We develop the first model for extreme mass-ratio inspirals (EMRIs) into a rotating massive black hole driven by gravitational self-force. Our is based on an action angle formulation of method osculating geodesics eccentric, equatorial (i.e., spin-aligned) motion in Kerr spacetime. The forcing terms are provided efficient spectral interpolation first-order self-force outgoing radiation gauge. apply near-identity (averaging) transformation to eliminate all dependence orbital phases from...
We compare recently computed waveforms from second-order gravitational self-force (GSF) theory to those generated by a new, GSF-informed, effective one body (EOB) waveform model for (spin-aligned, eccentric) inspiralling black hole binaries with large mass ratios. focus on quasicircular, nonspinning, configurations and perform detailed GSF/EOB phasing comparisons, either in the time domain or via gauge-invariant dimensionless function...
We present a numerical code for calculating the self-force on scalar charge moving in bound (eccentric) geodesic equatorial plane of Kerr black hole. work frequency domain and make use method extended homogeneous solutions [Phys. Rev. D 78, 084021 (2008)], conjunction with mode-sum regularization. Our is part program to develop computational architecture fast efficient calculations, alternative time-domain methods. find that our frequency-domain outperforms existing schemes small...
We present a new, fast method for computing the inspiral trajectory and gravitational waves from extreme mass-ratio inspirals that can incorporate all known (and future) self-force results. Using near-identity (averaging) transformations we formulate equations of motion do not explicitly depend upon orbital phases inspiral, making them to evaluate, whose solutions track evolving constants motion, waveform phase full $O(\eta)$, where $\eta$ is (small) mass ratio. As concrete example,...
We calculate the evolution and gravitational-wave emission of a spinning compact object inspiraling into substantially more massive (nonrotating) black hole. extend our previous model for nonspinning binary [Phys. Rev. D 93, 064024 (2016)] to include Mathisson-Papapetrou-Dixon spin-curvature force. For spin-aligned binaries we dephasing inspiral associated waveforms relative models that do not effects. find this can be either positive or negative depending on initial separation binary. in...
The gravitational self-force (GSF) and post-Newtonian (PN) schemes are complementary approximation methods for modeling the dynamics of compact binary systems. Comparison their results in an overlapping domain validity provides a crucial test both can be used to enhance accuracy, e.g. via determination previously unknown PN parameters. Here, first time, we extend such comparisons noncircular orbits---specifically, system two nonspinning objects bound (eccentric) orbit. To enable comparison...