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pAGN: the one-stop solution for AGN disc modeling
Authors:
Daria Gangardt,
Alessandro Alberto Trani,
Clément Bonnerot,
Davide Gerosa
Abstract:
Models of accretion discs surrounding active galactic nuclei (AGNs) find vast applications in high-energy astrophysics. The broad strategy is to parametrize some of the key disc properties such as gas density and temperature as a function of the radial coordinate from a given set of assumptions on the underlying physics. Two of the most popular approaches in this context were presented by Sirko &…
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Models of accretion discs surrounding active galactic nuclei (AGNs) find vast applications in high-energy astrophysics. The broad strategy is to parametrize some of the key disc properties such as gas density and temperature as a function of the radial coordinate from a given set of assumptions on the underlying physics. Two of the most popular approaches in this context were presented by Sirko & Goodman (2003) and Thompson et al. (2005). We present a critical reanalysis of these widely used models, detailing their assumptions and clarifying some steps in their derivation that were previously left unsaid. Our findings are implemented in the pAGN module for the Python programming language, which is the first public implementation of these accretion-disc models. We further apply pAGN to the evolution of stellar-mass black holes embedded in AGN discs, addressing the potential occurrence of migration traps.
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Submitted 14 May, 2024; v1 submitted 29 February, 2024;
originally announced March 2024.
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Efficient multi-timescale dynamics of precessing black-hole binaries
Authors:
Davide Gerosa,
Giulia Fumagalli,
Matthew Mould,
Giovanni Cavallotto,
Diego Padilla Monroy,
Daria Gangardt,
Viola De Renzis
Abstract:
We present analytical and numerical progress on black-hole binary spin precession at second post-Newtonian order using multi-timescale methods. In addition to the commonly used effective spin which acts as a constant of motion, we exploit the weighted spin difference and show that such reparametrization cures the coordinate singularity that affected the previous formulation for the case of equal-m…
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We present analytical and numerical progress on black-hole binary spin precession at second post-Newtonian order using multi-timescale methods. In addition to the commonly used effective spin which acts as a constant of motion, we exploit the weighted spin difference and show that such reparametrization cures the coordinate singularity that affected the previous formulation for the case of equal-mass binaries. The dynamics on the precession timescale is written down in closed form in both coprecessing and inertial frames. Radiation reaction can then be introduced in a quasi-adiabatic fashion such that, at least for binaries on quasi-circular orbits, gravitational inspirals reduce to solving a single ordinary differential equation. We provide a broad review of the resulting phenomenology and rewrite the relevant physics in terms of the newly adopted parametrization. This includes the spin-orbit resonances, the up-down instability, spin propagation at past time infinity, and new precession estimators to be used in gravitational-wave astronomy. Our findings are implemented in version 2 of the public Python module PRECESSION. Performing a precession-averaged post-Newtonian evolution from/to arbitrarily large separation takes $\lesssim 0.1$ s on a single off-the-shelf processor - a 50x speedup compared to our previous implementation. This allows for a wide variety of applications including propagating gravitational-wave posterior samples as well as population-synthesis predictions of astrophysical nature.
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Submitted 25 July, 2023; v1 submitted 10 April, 2023;
originally announced April 2023.
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Constraining black-hole binary spin precession and nutation with sequential prior conditioning
Authors:
Daria Gangardt,
Davide Gerosa,
Michael Kesden,
Viola De Renzis,
Nathan Steinle
Abstract:
We investigate the detectability of sub-dominant spin effects in merging black-hole binaries using current gravitational-wave data. Using a phenomenological model that separates the spin dynamics into precession (azimuthal motion) and nutation (polar motion), we present constraints on the resulting amplitudes and frequencies. We also explore current constraints on the spin morphologies, indicating…
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We investigate the detectability of sub-dominant spin effects in merging black-hole binaries using current gravitational-wave data. Using a phenomenological model that separates the spin dynamics into precession (azimuthal motion) and nutation (polar motion), we present constraints on the resulting amplitudes and frequencies. We also explore current constraints on the spin morphologies, indicating if binaries are trapped near spin-orbit resonances. We dissect such weak effects from the signals using a sequential prior conditioning approach, where parameters are progressively re-sampled from their posterior distribution. This allows us to investigate whether the data contain additional information beyond what is already provided by quantities that are better measured, namely the masses and the effective spin. For the current catalog of events, we find no significant measurements of weak spin effects such as nutation and spin-orbit locking. We synthesize a source with a high nutational amplitude and show that near-future detections will allow us to place powerful constraints, hinting that we may be at the cusp of detecting spin nutations in gravitational-wave data.
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Submitted 26 May, 2023; v1 submitted 31 March, 2022;
originally announced April 2022.
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A taxonomy of black-hole binary spin precession and nutation
Authors:
Daria Gangardt,
Nathan Steinle,
Michael Kesden,
Davide Gerosa,
Evangelos Stoikos
Abstract:
Binary black holes with misaligned spins will generically induce both precession and nutation of the orbital angular momentum $\bf{L}$ about the total angular momentum $\bf{J}$. These phenomena modulate the phase and amplitude of the gravitational waves emitted as the binary inspirals to merger. We introduce a "taxonomy" of binary black-hole spin precession that encompasses all the known phenomeno…
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Binary black holes with misaligned spins will generically induce both precession and nutation of the orbital angular momentum $\bf{L}$ about the total angular momentum $\bf{J}$. These phenomena modulate the phase and amplitude of the gravitational waves emitted as the binary inspirals to merger. We introduce a "taxonomy" of binary black-hole spin precession that encompasses all the known phenomenology, then present five new phenomenological parameters that describe generic precession and constitute potential building blocks for future gravitational waveform models. These are the precession amplitude $\langleθ_L\rangle$, the precession frequency $\langle Ω_L\rangle$, the nutation amplitude $Δθ_L$, the nutation frequency $ω$, and the precession-frequency variation $ΔΩ_L$. We investigate the evolution of these five parameters during the inspiral and explore their statistical properties for sources with isotropic spins. In particular, we find that nutation of $\bf{L}$ is most prominent for binaries with high spins ($χ\gtrsim 0.5$) and moderate mass ratios ($q \sim 0.6$).
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Submitted 14 June, 2021; v1 submitted 5 March, 2021;
originally announced March 2021.
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A generalized precession parameter $χ_\mathrm{p}$ to interpret gravitational-wave data
Authors:
Davide Gerosa,
Matthew Mould,
Daria Gangardt,
Patricia Schmidt,
Geraint Pratten,
Lucy M. Thomas
Abstract:
Originally designed for waveform approximants, the effective precession parameter $χ_\mathrm{p}$ is the most commonly used quantity to characterize spin-precession effects in gravitational-wave observations of black-hole binary coalescences. We point out that the current definition of $χ_\mathrm{p}$ retains some, but not all, variations taking place on the precession timescale. We rectify this inc…
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Originally designed for waveform approximants, the effective precession parameter $χ_\mathrm{p}$ is the most commonly used quantity to characterize spin-precession effects in gravitational-wave observations of black-hole binary coalescences. We point out that the current definition of $χ_\mathrm{p}$ retains some, but not all, variations taking place on the precession timescale. We rectify this inconsistency and propose more general definitions that either fully consider or fully average those oscillations. Our generalized parameter $χ_\mathrm{p}\in[0,2]$ presents an exclusive region $χ_\mathrm{p}>1$ that can only be populated by binaries with two precessing spins. We apply our prescriptions to current LIGO/Virgo events and find that posterior distributions of $χ_\mathrm{p}$ tend to show longer tails at larger values. This appears to be a generic feature, implying that (i) current $χ_\mathrm{p}$ measurement errors might be underestimated, but also that (ii) evidence for spin precession in current data might be stronger than previously inferred. Among the gravitational-wave events released to date, that which shows the most striking behavior is GW190521.
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Submitted 25 March, 2021; v1 submitted 24 November, 2020;
originally announced November 2020.