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Modelling Populations of Kilonovae
High Energy Astrophysical Phenomena · Submitted 24 May 2022
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim A comparison with detailed radiative transfer calculations indicates that further improvements are needed to accurately reproduce spectral shapes over the full light curve evolution.
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The abstract, sentence by sentence
The 2017 detection of a kilonova coincident with gravitational-wave emission has identified neutron star mergers as the major source of the heaviest elements, and dramatically constrained alternative theories of gravity. Observing a population of such sources has the potential to transform cosmology, nuclear physics, and astrophysics. However, with only one confident multi-messenger detection currently available, modelling the diversity of signals expected from such a population requires improved theoretical understanding. In particular, models which are quick to evaluate, and are calibrated with more detailed multi-physics simulations, are needed to design observational strategies for kilonovae detection, and to obtain rapid-response interpretations of new observations. We use grey-opacity models to construct populations of kilonovae, spanning ejecta parameters predicted by numerical simulations. Our modelling focuses on wavelengths relevant for upcoming optical surveys, such as the Rubin Observatory Legacy Survey of Space and Time (LSST). In these simulations, we implement heating rates that are based on nuclear reaction network calculations. We create a Gaussian-process emulator for kilonova grey opacities, calibrated with detailed radiative transfer simulations. Using recent fits to numerical relativity simulations, we predict how the ejecta parameters from BNS mergers shape the population of kilonovae, accounting for the viewing-angle dependence. Our simulated population of binary neutron star (BNS) mergers produce peak i-band absolute magnitudes $-20 \leq M_i \leq -11$. A comparison with detailed radiative transfer calculations indicates that further improvements are needed to accurately reproduce spectral shapes over the full light curve evolution.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The 2017 detection of a kilonova coincident with gravitational-wave emission has identified neutron star mergers as the major source of the heaviest elements, and dramatically constrained alternative theories of gravity. | background 1.00 | 0.05 | 0.06 | asserted 1.00 |
| s1 | Observing a population of such sources has the potential to transform cosmology, nuclear physics, and astrophysics. | background 0.92 | 0.05 | 0.05 | hedged possibility 0.99 |
| s2 | However, with only one confident multi-messenger detection currently available, modelling the diversity of signals expected from such a population requires improved theoretical understanding. | gap 0.99 | 0.08 | 0.04 | asserted 0.94 |
| s3 | In particular, models which are quick to evaluate, and are calibrated with more detailed multi-physics simulations, are needed to design observational strategies for kilonovae detection, and to obtain rapid-response interpretations of new observations. | gap 0.93 | 0.05 | 0.06 | asserted 0.93 |
| s4 | We use grey-opacity models to construct populations of kilonovae, spanning ejecta parameters predicted by numerical simulations. | method 0.89 | 0.95 | 0.06 | asserted 1.00 |
| s5 | Our modelling focuses on wavelengths relevant for upcoming optical surveys, such as the Rubin Observatory Legacy Survey of Space and Time (LSST). | method 0.88 | 0.78 | 0.03 | asserted 0.98 |
| s6 | In these simulations, we implement heating rates that are based on nuclear reaction network calculations. | method 0.99 | 0.89 | 0.02 | asserted 1.00 |
| s7 | We create a Gaussian-process emulator for kilonova grey opacities, calibrated with detailed radiative transfer simulations. | method 0.92 | 0.95 | 0.08 | asserted 1.00 |
| s8 | Using recent fits to numerical relativity simulations, we predict how the ejecta parameters from BNS mergers shape the population of kilonovae, accounting for the viewing-angle dependence. | method 0.82 | 0.89 | 0.16 | asserted 0.98 |
| s9 | Our simulated population of binary neutron star (BNS) mergers produce peak i-band absolute magnitudes $-20 \leq M_i \leq -11$. | result 1.00 | 0.94 | 0.19 | asserted 1.00 |
| s10 | A comparison with detailed radiative transfer calculations indicates that further improvements are needed to accurately reproduce spectral shapes over the full light curve evolution. | limitation 0.98 | 0.85 | 0.14 | hedged possibility 0.92 |
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The paper
Original abstract
The 2017 detection of a kilonova coincident with gravitational-wave emission has identified neutron star mergers as the major source of the heaviest elements, and dramatically constrained alternative theories of gravity. Observing a population of such sources has the potential to transform cosmology, nuclear physics, and astrophysics. However, with only one confident multi-messenger detection currently available, modelling the diversity of signals expected from such a population requires improved theoretical understanding. In particular, models which are quick to evaluate, and are calibrated with more detailed multi-physics simulations, are needed to design observational strategies for kilonovae detection, and to obtain rapid-response interpretations of new observations. We use grey-opacity models to construct populations of kilonovae, spanning ejecta parameters predicted by numerical simulations. Our modelling focuses on wavelengths relevant for upcoming optical surveys, such as the Rubin Observatory Legacy Survey of Space and Time (LSST). In these simulations, we implement heating rates that are based on nuclear reaction network calculations. We create a Gaussian-process emulator for kilonova grey opacities, calibrated with detailed radiative transfer simulations. Using recent fits to numerical relativity simulations, we predict how the ejecta parameters from BNS mergers shape the population of kilonovae, accounting for the viewing-angle dependence. Our simulated population of binary neutron star (BNS) mergers produce peak i-band absolute magnitudes $-20 \leq M_i \leq -11$. A comparison with detailed radiative transfer calculations indicates that further improvements are needed to accurately reproduce spectral shapes over the full light curve evolution.
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References
How the literature uses it
6 arXiv papers cite this in 12 sentences
Papers citing it · 7 sentences without a confident label
Uses its method or tool 1 paper
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Specifically, we follow [ref] and adopt the following prescription for the angular dependence of the electron fraction that captures reasonably well the one found in numerical-relativity simulations [ref] : [equation] where $θ$ is the polar angle and $a$ and $b$ are coefficients set to give a desired average $Y̅_e, dyn$.
The critical role of nuclear heating rates, thermalization efficiencies and opacities for kilonova modelling and parameter inference · Input ejecta model · 0.93
Compares with it 2 papers
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Our average absolute magnitude is about 0.4 mags fainter than the brighter peak of [ref] .
Designing an Optimal Kilonova Search using DECam for Gravitational Wave Events · Discussion · 0.95
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The peak magnitudes of the nKLF faint components we obtained are relatively brighter than those obtained by [ref] because the heating from the fallback accretion is considered in our model but not in [ref] .
The luminosity functions of kilonovae from binary neutron star mergers under different equation of states · Kilonova Luminosity Functions · 1.00
What it cites · 1 sentence without a confident label
Uses the method or tool of 1 paper
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We additionally implement time- and density-dependent thermalisation efficiencies following [ref] , and [ref] , and recently summarized in sec. 2.2 of [ref] .
The critical role of nuclear heating rates, thermalization efficiencies and opacities for kilonova modelling and parameter inference · Density-averaged time-dependent thermalisation · 0.98
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