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Debarati Chatterjee27/10/2025, 09:00Talk
One of the most exciting scientific discoveries in recent times has been the detection of Gravitational Waves from massive compact objects such as Neutron Stars, opening a new window to astronomy beyond multiwavelength telescopes. The ultra-high densities in the interior of Neutron Stars surpass those of terrestrial nuclear and heavy-ion laboratories and provide an ideal environment to study...
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Adriana R Raduta27/10/2025, 10:30Talk
Numerical simulations of core-collapse supernovae, mergers of binary neutron stars and formation of stellar black holes, which employed standard Skyrme interactions, established clear correlations between the evolution of these processes, characteristics of the hot compact objects as well as neutrino and gravitational wave signals and the value of effective nucleon mass at the saturation...
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Mahboubeh Shahrbaf27/10/2025, 10:55Talk
We investigate the equation of state (EOS) and macroscopic properties of neutron stars (NSs) and hyperonic stars within the framework of the lowest order constrained variational (LOCV) method, extended to include interacting Λ hyperons. The ΛN and ΛΛ interactions are described by realistic spin- and parity-dependent potentials fitted to hypernuclear data. Cold, charge-neutral, and...
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Philip Davis27/10/2025, 11:20Talk
We introduce a Python package called ComPyTools, currently under development, that allows the user to work with CompOSE equation-of-state tables. ComPyTools uses an object-oriented approach to provide a user-friendly interface to not only read in tables for analysis workflows, but also to create them in the CompOSE format. Additionally, we have implemented an interface that allows the user to...
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Oliver Eggenberger Andersen27/10/2025, 11:45Talk
Recent advancements in core-collapse supernova modeling are revealing a new black hole (BH) formation channel in which a BH forms within about a second of shock revival yet still results in a successful supernova. The limited body of literature on these black hole supernovae (BHSNe) has mostly focused on highly massive, compact progenitors. I will present a sample of ~40 stars between 19 and...
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Anastasios Theodoropoulos27/10/2025, 12:10Talk
Gravitational wave approximants are widely used in the analysis of Gravitational wave signals. They are highly accurate but they still lack speed. We present an autoencoder based surrogate model for BBH gravitational wave signals. We train our autoencoder on a NR informed surrogate model, we modify it so it can produce waveforms from the initial binary system parameters and then we fine tune...
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Dimitra Tseneklidou27/10/2025, 14:30Talk
Core-collapse supernovae (CCSNe) are one of the most anticipated future gravitational wave (GW) sources. The GW emission is dominated by the oscillation modes of the newly born proto-neutron star (PNS) and the stalled accretion shock. I am going to present a new general relativistic framework for computing the oscillation modes of a PNS, including, for the first time, an accretion flow and a...
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Suprovo Ghosh27/10/2025, 14:55Talk
Next-generation gravitational-wave detectors are expected to constrain the unknown neutron star equation-of-state from static and dynamical tides in binary inspirals. The impact of dissipation on the tides is generally considered negligible, but recent work suggests that the bulk viscosity of exotic phases (e.g. hyperons and deconfined quark matter) can be significant enough to be detectable...
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Miquel Miravet-Tenés27/10/2025, 15:20Talk
The magnetorotational instability (MRI) is considered a leading mechanism for driving angular momentum transport in differentially rotating astrophysical flows, including accretion disks and protoneutron stars. This process is mediated by the exponential amplification of the magnetic field whose final amplitude is envisioned to be limited by secondary (parasitic) instabilities. By relaxing...
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Dorota Rosinska (University of Warsaw)27/10/2025, 16:15Talk
The dynamical stability of differentially rotating neutron stars, including hypermassive neutron stars, is of paramount importance in understanding the fate of the postmerger remnant of binary neutron stars mergers and the formation of a black hole during core-collapse supernovae. We study systematically the dynamical stability of differentially rotating neutron stars within a broad range of...
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Stefano Muzzolon27/10/2025, 16:40Talk
We present a study on the application of two high-order numerical methods for solving the first-order hyperbolic generalized harmonic (GH) formulation of the vacuum Einstein equations of general relativity, introduced in [1], coupled with the Euler equations for matter variables. More precisely, we consider the central WENO Finite Differences method on 3D Cartesian grids, and the ADER...
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José Carlos Olvera Meneses27/10/2025, 17:05Talk
In this talk we discuss a fully 3D numerical evolution code to study neutron stars within the framework of massive-scalar-tensor (MST) theories. Our focus is to study the gravitational collapse of rapidly rotating neutron stars by exploring the parameter space defined by the scalar field couplings and the mass. We investigate how these parameters influence both the dynamical characteristics of...
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Mohsen Bigdeli27/10/2025, 17:30Talk
In this work, we briefly discuss the equation of state (EOS) for the different layers of a neutron star, from the inner core to the crust, employing the Lowest Order Constrained Variational (LOCV) approach. To this end, we investigate the EOS of quark clusters, kaon-condensed matter, and nuclear matter, as well as the equilibrium composition and energy of the Wigner-Seitz cell in the crust. We...
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Fabian Gittins28/10/2025, 09:00Talk
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Santiago Jaraba28/10/2025, 10:30Talk
The accurate modelling of neutron star oscillations is essential as we prepare for the next generation of gravitational-wave detectors, which will be able to probe the rich astrophysical content of post-merger signals. In this talk, I will present recent results obtained with ROXAS, a spectral code that numerically simulates the dynamical evolution of perturbed rotating neutron stars,...
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Arthur Suvorov28/10/2025, 10:55Talk
In the moments leading up to a binary merger, tides can excite a variety of modes inside neutron stars. I will describe how g-modes, and gravitoinertial modes more generally, excite differential rotations inside the stars in such a manner that dynamo activity can amplify an existing magnetic field there. This has implications for precursor flares, tidal dephasing, and various other phenomena...
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Stefanos Tsiopelas28/10/2025, 11:20Talk
The equation of state (EoS) for dense, strongly interacting matter serves as the central input in an array of astrophysical simulations involving isolated compact objects and binary systems across various scenarios. While numerous models exist to describe the composition of cold neutron stars, the range narrows considerably when considering the so-called general-purpose EoS, which encompass...
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Alexis Reboul-Salze28/10/2025, 11:45Talk
For some short gamma-ray bursts, a non-thermal precursor flare can be observed a few seconds before mergers. The luminosity and energy of these precursors can be explained by a surface magnetic dipole of 10^13 G and the release of magnetoelastic energy when the crust breaks. A recently-proposed scenario to explain this magnetic field is that during the last seconds of a binary neutron-star...
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Bikram Keshari Pradhan28/10/2025, 12:10Talk
Gravitational waves (GWs) from binary neutron star (BNS) mergers offer crucial insights into the Neutron Star (NS) interiors and nuclear physics. The inference of NS properties hinges on the GW waveform, and achieving an accurate description of BNS GWs is a key focus of current research. The leading tidal contribution arises from the f-mode oscillation of the NS, for which the mode frequency...
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Gabriele Montefusco28/10/2025, 14:30Talk
Meta-modeling frameworks have emerged as tools for exploring the nuclear equation of state (EoS) in a flexible way. However, current implementations often violate causality at supranuclear densities, resulting in a significant fraction of otherwise viable models being discarded for failing to support the observed maximum neutron star mass with a subluminal sound speed. I will present a refined...
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Bruno Peres28/10/2025, 14:55
The M1 scheme aimed at neutrino treatment in core collapse supernovae codes has numerous advantages. It is a good tradeoff between computational cost and accuracy. The M1 equations are hyperbolic, making it perfectly suitable for GR, and a part of the equations can be treated explicitely. I will show an implementation of the M1 in the CoCoNuT code, along with possibilities of future works in CoCoNuT.
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Nicolas Houry28/10/2025, 15:20Talk
Predicting whether a core-collapse supernova (CCSN) will successfully explode remains a central challenge in astrophysics. While many physical parameters influence the explosion outcome, recent studies have highlighted the structure of the silicon-oxygen (Si/O) interface as a potentially decisive factor in shock revival. In this work, I investigate the role of the Si/O interface by...
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Ernazar Abdikamalov28/10/2025, 16:15Talk
Core-collapse supernovae are sources of strong gravitational waves (GWs). We explore whether GW signals from rapidly rotating supernovae can be used to infer the equation of state (EOS) of high density matter. Focusing on the bounce and early post-bounce phases, we generate a large set of waveforms using general-relativistic hydrodynamics simulations with different EOS models. These are used...
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Giuseppe Rivieccio28/10/2025, 16:40Talk
We study the thermal index of low-density, high-temperature dense matter, using the virial expansion to account for nuclear interaction effects (G.R. et al 2025 ApJ 987 67). We focus on the region of validity of the expansion, which reaches $10^{-3}$ fm$^{-3}$ at $T=5$ MeV up to almost saturation density at $T=50$ MeV.
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In pure neutron matter, we find an analytical expression for the thermal... -
José Carlos Jiménez Apaza28/10/2025, 17:05Talk
We investigate the non-radial gravity-pulsation discontinuity mode (g-mode) in neutron stars with a strong 1st-order phase transition, dubbed twin stars. For this, we consider the standard four categories and employ the constant-speed-of-sound parametrization which accounts for the QCD transition. We find that depending on the category, the relations between g-mode frequencies and...
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Aurore Betranhandy28/10/2025, 17:30Talk
Gravitational waves are an important messenger to observe the first milliseconds of a core-collapse supernova, as radiations are still trapped and cannot convey any signal from the deeper part of the explosion. As such detections are only possible in the context of a galactic supernova, we have not yet been able to observe GWs from CCSN, and thus need to rely on simulations to decipher the...
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Michał Bejger29/10/2025, 09:00Talk
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29/10/2025, 10:00
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Armen Sedrakian29/10/2025, 10:30Talk
We present a general-relativistic study of strongly magnetized neutron stars (NSs), using the XNS code to solve the coupled Einstein–Maxwell equations, focusing on (i) examining equilibrium configurations with both toroidal and poloidal magnetic field geometries, (ii) incorporating complex many-body effects through microscopically derived pairing gaps for proton superconductor, and (iii)...
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Yong Gao29/10/2025, 10:55Talk
Dynamical tides of neutron stars in the late stages of binary inspirals provide a viable probe into dense matter through gravitational waves, and potentially trigger electromagnetic precursors. We model the tidal response as a set of driven harmonic oscillators, where the natural frequencies are given by the quasinormal modes of a nonrotating neutron star. These modes are calculated in general...
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Liubov Kovalenko29/10/2025, 11:20Talk
Core-collapse supernovae are among the most energetic explosions in the universe. Their evolution is shaped by the hydrodynamics, neutrino transport, and magnetic fields at work in the first seconds after the collapse. We investigate these processes through 3D simulations of an extremely compact 39-Msun progenitor using the FLASH M1 magnetohydrodynamics code. Our study explores three models –...
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Arus Harutyunyan29/10/2025, 11:45Talk
This work investigates the bulk viscosity of warm, dense, neutrino-transparent, color-superconducting quark matter, where damping of density oscillations in the kHz frequency range arises from weak-interaction-driven direct Urca processes involving quarks. We study the two-flavor red-green paired color-superconducting (2SC) phase, while allowing for the presence of unpaired strange quarks and...
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Guillem Fernández Rodríguez29/10/2025, 12:10Talk
The gravitational radiation from core-collapse supernovae (CCSNe) is dominated by the oscillation modes of the proto-neutron star associated and the stalled accretion shock, and can be detectable in the case of galactic distances. These modes have been computed by several methods [1, 2, 3]. In this talk, we present the first steps of a potential alternative method to classify the different...
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Lap-Ming Lin29/10/2025, 14:30Talk
Numerical simulation of strange quark stars is challenging due to the strong density discontinuity at the stellar surface. In this talk, we shall present our successful simulations of rapidly rotating quark stars and study their oscillation modes in full general relativity.
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Gaël Servignat29/10/2025, 14:55Talk
The spatial gravitational waves observatory LISA has been officially adopted by ESA in January 2024 and its launch is currently planned for 2035, leaving a decade to face all the data analysis challenges posed by the expected data. In this presentation I will present the various sources of LISA with their associated science cases and how this leads to new challenges in gravitational data...
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Fatemeh Hossein Nouri29/10/2025, 15:20Talk
We present new simulations performed with Spritz, a general-relativistic magnetohydrodynamics (GRMHD) code designed for high-precision studies of binary neutron star (BNS) mergers with realistic nuclear equations of state (EOS). We evolve both magnetized and non-magnetized equal-mass binaries, employing two tabulated EOS modeled after the GW170817 event. Our analysis focuses on the...
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Davood Rafiei Karkevandi29/10/2025, 15:45Talk
We investigate the impact of a hypothetical bosonic dark matter (DM) candidate, the sexaquark, on the fundamental (f-mode) oscillations of neutron stars (NSs). By varying the DM particle mass and considering different core compositions including hypernuclear matter, sexaquark DM, and deconfined quark matter (QM), we construct hybrid equations of state (EOS) with a smooth hadron-quark crossover...
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Dimitra TseneklidouTalk
Core-collapse supernovae (CCSNe) are one of the most anticipated future gravitational wave (GW) sources. The GW emission is dominated by the oscillation modes of the newly born proto-neutron star (PNS) and the stalled accretion shock. I am going to present a new general relativistic framework for computing the oscillation modes of a PNS, including, for the first time, an accretion flow and a...
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Milton RuizTalk
Neutron stars are the most compact horizonless objects in the Universe, exhibiting the strongest known magnetic fields. They are potential sources of coincident gravitational waves and electromagnetic radiation across the entire spectrum. However, the internal configuration of their magnetic fields and the mechanisms that stabilize them remain open questions. As a stepforward understanding the...
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José Carlos Olvera MenesesTalk
In this talk we discuss a fully 3D numerical evolution code to study neutron stars within the framework of massive-scalar-tensor (MST) theories. Our focus is to study the gravitational collapse of rapidly rotating neutron stars by exploring the parameter space defined by the scalar field couplings and the mass. We investigate how these parameters influence both the dynamical characteristics of...
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