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Jade Powell (Swinburne University of Technology)CoCoNuT meeting (9-11 Sept)
We perform 3D simulations of supernovae with a variety of magnetic field strengths and rotation rates with the magnetohydrodynamical version of the CoCoNuT code. We simulate a 39 solar mass progenitor star with rapid rotation and three different magnetic field strengths, and a 15 solar mass progenitor with different equations of state, rotation rates, and weak magnetic fields. We discuss the...
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Adam Griffiths (Keele University)CoCoNuT meeting (9-11 Sept)
The most energetic core-collapse supernovae are thought to arise from rapidly rotating, magnetised progenitors. However, the three-dimensional pre-collapse structure of their angular momentum and magnetic fields remains poorly constrained, limiting the realism of magnetorotational core-collapse simulations.
In this talk, I will present two novel progenitor models for magneto-rotational...
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Rahime Matur (University of Southampton)CoCoNuT meeting (9-11 Sept)
The inclusion of magnetic fields in neutron star merger simulations is essential for understanding a wide range of phenomena, from the efficiency of magnetic field amplification during the merger to the formation of a magnetar and/or jet. Accurate magnetic field evolution is also crucial for modelling the electromagnetic counterparts of these mergers. Current GRMHD codes typically rely either...
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Mr Anastasios Theodoropoulos (University of Valencia)Day-0 meeting on AI for numerical relativity
The generation of accurate waveforms from binary black hole (BBH) mergers is a major effort in Gravitational-Wave Astronomy. In recent years, machine-learning–based surrogate models for BBH waveforms have been proposed. Those offer the potential to dramatically accelerate waveform generation while maintaining accuracy competitive with that of traditional waveform approximants. In this work, we...
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Ramon Jaeger (Universität Potsdam)CoCoNuT meeting (9-11 Sept)
Binary neutron star (BNS) systems are currently understood as prominent sources of heavy elements and electromagnetic signatures originating from nucleosynthetic processes. These processes are highly sensitive to the thermodynamical state of the ejected material. To model such complex systems, numerical relativity has emerged as a suitable framework, which provides the means to assess...
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Raj Kishor Joshi (CAMK, Warsaw, Poland)CoCoNuT meeting (9-11 Sept)
Magnetars are among the most extreme magnetized environments in the universe, and modeling their magnetohydrodynamic (MHD) evolution is central to understanding how their fields are generated, structured, and sustained. While these objects are observed through energetic transients such as Soft Gamma Repeaters and Anomalous X-ray Pulsars, the configuration and longevity of their internal...
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Guillem Fernández -Rodríguez (Univesitat de Valencia)CoCoNuT meeting (9-11 Sept)
Oscillation modes of the proto-neutron star and stalled accretion shock in core-collapse supernovae are a promising gravitational-wave source, potentially detectable at galactic distances. We present progress on a data-driven scheme to sort computed eigenmodes based on their linear similarity, requiring no prior assumptions about the physical origin of each mode. Building on our previous work,...
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Afonso Ávila (University of Coimbra)CoCoNuT meeting (9-11 Sept)
The accumulation of dark matter inside neutron stars may alter their internal structure and tidal deformability, potentially leaving observable imprints on the gravitational-wave signals emitted during binary neutron star mergers. In this work, we investigate the capability of next-generation gravitational-wave detectors, the Einstein Telescope (ET) and Cosmic Explorer (CE), to probe the...
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Giuseppe Rivieccio (Universitat de Valencia)CoCoNuT meeting (9-11 Sept)
This talk examines the impact of nonconvex equations of state (EoS) in binary neutron (BNS) star merger simulations. We extended the work GR et al. 2024 addressing the key distinction between first-order and crossover phase transitions (PT) in the context of the quasi-universal relation $f_{peak}-\Lambda$. We develop a parametrized PT that allows control of its stiffness and convexity. By...
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Osvaldo Gramaxo Freitas (University of Valencia)Day-0 meeting on AI for numerical relativity
Numerical relativity (NR) simulations are considered to provide the most faithful representation of the gravitational wave (GW) radiation emitted by binary black hole (BBH) systems. However, in the context of GW astronomy, tasks such as parameter estimation (PE) can require thousands upon thousands of waveform evaluations per second across the entire parameter space. Since performing full NR...
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Dr Violetta Sagun (University of Southampton)CoCoNuT meeting (9-11 Sept)
Compact stars due to their enormous gravitational field can accumulate a sizable amount of dark matter in their interior. Depending on its nature, accumulated dark matter may affect the properties of neutron stars in quite different ways. I will give an overview of the impact of dark matter on various observable properties of neutron stars, i.e. the mass-radius relation, tidal deformability,...
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Dimitra Tseneklidou (University of Valencia)CoCoNuT meeting (9-11 Sept)
In this talk, I will present a novel scheme to classify the oscillation modes of a newly born proto-neutron star surrounded by a stalled accretion shock in core-collapse supernovae (CCSNe). Our classification is physically motivated, as it is based on the energy of the restoring forces of the mode. We investigate the nature of the modes by considering the different regions of the CCSN that...
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Ivan Markin (University of Potsdam)CoCoNuT meeting (9-11 Sept)
Recently, there have been significant advances in the development of eccentric gravitational-wave models, so that multiple eccentric models are now available. Real-event reanalysis with these models revealed evidence of nonzero eccentricity in the black hole-neutron star (BHNS) merger GW200105. Such evidence for eccentricity points to a dynamical formation channel in dense environments, rather...
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Han Zhang (Durham University)CoCoNuT meeting (9-11 Sept)
ExaGRyPE is a suite of solvers for numerical relativity based on ExaHyPE 2, our second-generation Exascale Hyperbolic PDE Engine. This code tackles the Einstein equations/relativistic hydrodynamics equations under a 3+1 foliation, with a focus on compact object spacetimes. The implementation utilizes a block-structured Cartesian grid with higher-order Finite Difference schemes and adaptive...
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Laetitia Martel (University of Southampton)CoCoNuT meeting (9-11 Sept)
In 1973, Bardeen, Carter and Hawking announced the celebrated four laws of black hole thermodynamics, by analogy with the laws of thermodynamics. However, recent works suggest that the third law - stating that an extremal black hole cannot be formed from regular conditions in a finite time - could be incorrect.
We investigate the formation of extremal black holes with our null coordinates...
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Oliver Steppohn (Friedrich-Schiller University Jena)CoCoNuT meeting (9-11 Sept)
We investigate the impact of different physics on numerical-relativity simulations of black hole-neutron star (BHNS) mergers. In particular, we are interested in how magnetic fields and the subsequent inclusion of neutrino transport shape the gravitational radiation and ejecta of certain BHNS mergers. The simulations for this study are carried out with the GPU-accelerated code AthenaK.
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Marco Cusinato (University of Valencia)CoCoNuT meeting (9-11 Sept)
Core-collapse supernovae (CCSNe) are among the most energetic phenomena in the Universe and are promising multimessenger sources of gravitational waves (GWs) and neutrinos. The nuclear equation of state (EOS) is a key ingredient in CCSN simulations, as it determines the thermodynamic properties of dense matter, the structure and maximum mass of the proto-neutron star (PNS), and consequently...
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Nicolas Houry (CEA)CoCoNuT meeting (9-11 Sept)
Predicting the outcome of core collapse in massive stars (whether the star explodes as a supernova or collapses into a black hole) remains an open problem. The complex physics involved and the uncertainties in the progenitor structure make it difficult to identify which stars are more likely to explode. Recent studies suggest that the density gradient at the interface between the silicon and...
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Thierry Foglizzo (CEA saclay)CoCoNuT meeting (9-11 Sept)
During the core-collapse of a massive star, the phase of stalled accretion shock following the birth of a proto-neutron star can be directly observed with gravitational waves and neutrinos. Hydrodynamical instabilities responsible for the asymmetric character of this phase, such as the Standing Accretion Shock Instability, produce characteristic oscillation frequencies that can be identified...
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Saurabh Yeole (PhD student at IUCAA)CoCoNuT meeting (9-11 Sept)
Neutron stars are known to have two distinct populations in terms of their surface magnetic fields, viz. low magnetic fields of $10^8–10^{10}$ G such as in millisecond pulsars, and those with higher magnetic fields ($10^{12}$ G), comprising of the bulk of known neutron star population. An accretion induced reprocessing scenario is often invoked to explain the higher spin frequencies of...
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Raphaël Raynaud (Université Paris Cité)CoCoNuT meeting (9-11 Sept)
Magnetars are young, isolated neutron stars that possess exceptionally high magnetic fields. To explain their formation, one plausible scenario relies on a turbulent convective dynamo that develops inside the protoneutron star. However, the short expected duration of the convection phase imposes a stringent constraint on the efficiency of amplification process. We address this question by...
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Nicolas Moraga (Newcastle University)CoCoNuT meeting (9-11 Sept)
Neutrons and protons in neutron-star cores are widely expected to exist in superfluid and superconducting states, respectively. These phases profoundly modify the magnetic evolution through the macroscopic manifestation of the interaction between quantized neutron vortices and proton flux tubes. In the simplest limit, neglecting rotation and entrainment, axisymmetric MHD equilibria have been...
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Thomas Celora (Institute of Space Sciences)CoCoNuT meeting (9-11 Sept)
Magnetic fields and the associated turbulent dynamics are central to the evolution of binary neutron star merger remnants. In particular, the amplification of magnetic fields from realistic pre-merger seed strengths to the values thought to be required for jet launching, as well as the emergence of large-scale structures sustaining collimated relativistic outflows, remain not well understood....
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Liubov Kovalenko (Stockholm University)CoCoNuT meeting (9-11 Sept)
Rapid rotation and strong magnetic fields can reshape the dynamics, energetics, and multimessenger emission of core-collapse supernovae. We investigate these effects using three-dimensional magnetohydrodynamic simulations together with hydrodynamic control models.
Rotation alone modifies the protoneutron star structure, neutrino emission, post-shock dynamics, and the development of...
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Lik Hang Harry Shum (University of Nottingham)CoCoNuT meeting (9-11 Sept)
In this talk, we will discuss our efforts in numerically modelling viscous effects in neutron stars (NSs) using the recently proposed first-order dissipative hydrodynamics framework by Bemfica, Disconzi, Noronha and Kovtun (known as the BDNK framework). We first demonstrate that under a simplified set up, stable evolutions of spherically symmetric NSs can be achieved in 1+1 spacetime, from...
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Alphonse MOREAUCoCoNuT meeting (9-11 Sept)
When a massive star dies, the collapse of its core forms a proto-neutron star. The accreting envelope creates a hydrodynamical shock that stalls after a few hundred milliseconds. The growth of the Standing Accretion Shock Instability (SASI) contributes to the asymmetric character of the explosion, the production of gravitational waves and a modulation of the neutrino signal.
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In preparation... -
Mr Deepak Kumar (Department of Physics, Chandigarh University, Gharuan Mohali 140413, India)CoCoNuT meeting (9-11 Sept)
Binary neutron star (BNS) mergers are among the most promising multimessenger sources, providing simultaneous insights into strong-field gravity, dense nuclear matter, heavy-element nucleosynthesis, and transient electromagnetic phenomena. Understanding how intrinsic neutron-star properties influence merger outcomes is essential for interpreting current and future observations. In this work,...
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Henrique Leonhard Gieg (University of Potsdam)CoCoNuT meeting (9-11 Sept)
Recent binary-neutron-star-merger (BNSM) literature assumes the leptonic content of neutron-star (NS) matter to be restricted to electron-flavored leptons, and, accordingly, neutrino processes are approached within a three-species prescription. However, at sufficiently high densities, the onset of muons/antimuons is expected, as de-occupation of electron/positron states with energies above the...
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Lami Shetu Suleiman (Deutches Elektronen Synchrotron)CoCoNuT meeting (9-11 Sept)
Neutron star astrophysical observables provide a unique insight into the physics of dense matter. The famous binary neutron star merger GW170817 has particularly provided constraints on the equation of state of dense matter, revealing its softening in the core of neutron stars. Such insight is out of the reach of nuclear theory because of the non-perturbative nature of strong-interaction, and...
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Santiago Jaraba (Observatoire astronomique de Strasbourg - CNRS)CoCoNuT meeting (9-11 Sept)
The oscillation modes of neutron stars encode valuable information about their internal structure and dense-matter equation of state. These signatures can be studied through gravitational waves, with next-generation detectors offering new opportunities thanks to their improved sensitivity, which will provide better access to the post-merger phase of binary neutron stars.
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In this talk, I will... -
Mr Arijit Das (Indian Institute of Science Education and Research, Thiruvananthapuram, India)CoCoNuT meeting (9-11 Sept)
We construct an equation of state for isentropic dark-matter-admixed neutron stars (DMANS) with a hot core and relatively cold crust incorporating self-consistent temperature and DM density profiles for GeV-scale fermionic DM. We show that the enhancement of central stellar density due to DM accumulation, previously reported for cold neutron stars, remains robust. Substantial observable...
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Matteo Stockinger (Max Planck Institute for Gravitational Physics (Albert Einstein insstitute))Day-0 meeting on AI for numerical relativity
The magnetospheres of compact objects are known to be at the origin of many important astrophysical phenomena, going from pulsar emission to jet formation around black holes through the Blandford-Znajek process. Thanks to variety of numerical tools, these phenomena are increasingly well understood. However in the era of multi-messenger astrophysics comes the challenge of understanding the...
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Fabrizio Venturi Piñas (Universitat de València)CoCoNuT meeting (9-11 Sept)
We study the dynamics of the common magnetosphere of black hole-neutron star binaries during their inspiral phase, by means of force-free electrodynamic simulations. Quite generically, for realistic stellar compactness values and tight-enough orbits, we find a spiral arm current sheet (CS) that emerges trailing the neutron star's orbital motion. The intense magnetic reconnections produced at...
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Jennifer Quinlan (Monash University)CoCoNuT meeting (9-11 Sept)
Core-collapse supernovae from rapidly rotating and strongly magnetised progenitors are promising candidates for producing the highly energetic hypernova explosions we observe in nature. Current theoretical hydrodynamical supernova simulations have yet to reproduce the same high energies beyond $10^{52}$ erg that we associate with the observed hypernova.
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I will present four... -
Michael Müller (University of Greifswald)CoCoNuT meeting (9-11 Sept)
The small-scale dynamics in magnetized accretion disks around rapidly rotating neutron stars is inherently coupled to the large-scale evolution of the disk through the action of a mean-field dynamo and turbulent stresses. The mean-field dynamo leads to the formation of coherent magnetic flux bundles that can migrate from the disk and power a collimated polar outflow as well as magnetic...
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William Cook (FSU Jena)Day-0 meeting on AI for numerical relativity
Turbulence is a key driver of dynamics in both isolated and binary neutron star (BNS) systems, and can be triggered by magnetic field instabilities. In particular the onset of the Kelvin-Helmholtz and Magnetorotational Instabilities plays a key role in the evolution of the magnetic field in a post-merger remnant from a BNS system. Modelling the impact of turbulence directly in numerical...
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Jerome Guilet (CEA Saclay)CoCoNuT meeting (9-11 Sept)
Turbulence and magnetic field amplification in protoneutron stars are important for supernova explosions, their associated multimessenger signal as well as to determine the properties of the neutron stars in particular their rotation and magnetic field. They can be driven by different processes including convection, magnetorotational instability and the Tayler-Spruit dynamo and are sensitive...
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Haakon Andresen (Stockholm University)CoCoNuT meeting (9-11 Sept)
I will present recent results from 60 axisymmetric core-collapse simulations performed with FLASH. I will describe how the power gap, a narrow band of reduced emission observed in predicted gravitational wave signals, correlates with the properties of the numerical simulations. I will give an overview of proposed explanations and how well these explanations work for our set of simulations.
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Ms Marta Piscitelli (University of Tübingen)CoCoNuT meeting (9-11 Sept)
While the external magnetic fields of neutron stars are inferred through electromagnetic observations, the structure and strength of their internal fields remain largely unconstrained. The persistence of strong magnetic fields even in old neutron stars requires that their interior magnetic configuration must remain stable over astrophysical timescales. However, a fully consistent theoretical...
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Vishnu Varma (Keele University)CoCoNuT meeting (9-11 Sept)
Core-collapse supernovae (CCSNe) are some of the brightest, most energetic events in the
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universe. In order to model these phenomena accurately, we need to have a diverse range of physics such as neutrino transport and neutrino interactions, general-relativistic gravity, detailed equations of state (EoS) of dense matter, magnetohydrodynamic (MHD) and detailed progenitor models. When modelling... -
Stefano Muzzolon (University of Trento and Verona)CoCoNuT meeting (9-11 Sept)
We present a study on the application of a family of high-order Central WENO (CWENO) Finite Difference (FD) schemes to simulate Binary Neutron Star (BNS) mergers, where the initial data configurations are generated with the Lorene library following [1].
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The evolution is performed in the framework of the first-order hyperbolic Generalized Harmonic (GH) formulation of the Einstein equations of... -
Fabian Gittins (Utrecht University)CoCoNuT meeting (9-11 Sept)
Third-generation gravitational-wave observatories will transform our ability to constrain dense nuclear matter by measuring the tide in coalescing neutron-star binaries with unprecedented precision. To date, analyses have focused on the dominant static contribution known as the tidal deformability $\Lambda$. However, the increasing orbital frequency during the inspiral will also excite stellar...
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Alexander Haber (University of Southampton, UK)CoCoNuT meeting (9-11 Sept)
Weak interaction (Urca) processes govern neutrino emission, chemical equilibration, and bulk viscosity in neutron stars and their mergers. Standard treatments inconsistently combine direct and modified Urca processes, but suffer from divergencies near the direct Urca threshold and are difficult to extend to finite temperature and strong magnetic fields. In this talk, I will present the Nucleon...
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Jens Mahlmann (Dartmouth College)CoCoNuT meeting (9-11 Sept)
Relativistic plasmas in highly magnetized neutron star (NS) magnetospheres, including binary NS mergers and magnetars, are well described by force-free electrodynamics (FFE) on large scales, yet their observable emission is strongly influenced by kinetic physics. Global 3D FFE simulations of interacting binary NS magnetospheres reveal extended current sheets, Kelvin–Helmholtz–driven...
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