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Elena Poli (Pitaevskii BEC Center, CNR-INO, Trento, Italy)22/06/2026, 09:00
Since the realization of the first dipolar Bose–Einstein condensate (BEC) of strongly magnetic atoms, long-range and anisotropic dipole–dipole interactions have enabled the emergence of novel quantum phases driven by interaction-induced density modulations. Among these, the most remarkable is the supersolid phase, which simultaneously combines crystalline order with global phase coherence. In...
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Julie Jacob Thomas (Newcastle University)22/06/2026, 09:50
Neutron stars are the collapsed cores of massive stars that have undergone a supernova explosion. They are the densest known astrophysical objects, with a mass typically 1.4 times that of the Sun compressed into a radius of approximately 10 km. Deep within the star, where the density exceeds the nuclear equilibrium density, neutrons become superfluid and protons become superconducting. As a...
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Emil Varga (Univerzita Karlova, Faculty of Mathematics and Physics)22/06/2026, 10:15
I will present work that investigates the dynamics of quantized vortices in superfluid $^4$He confined to nanoscale geometries, where vortex motion is strongly influenced by pinning on disordered substrate surfaces. We present a numerical model for quasi-2D geometries that captures vortex-surface interactions as a velocity-dependent mutual friction; results from our numerical simulations show...
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Bugra Tuzemen (IFPAN)22/06/2026, 11:10Talk
Spin imbalance in ultracold Fermi gases gives rise to a rich variety of structures rooted in the competition between pairing and polarization. I will present a survey of our recent results, starting from the static phase diagram where disordered configurations compete energetically with Larkin-Ovchinnikov-Fulde-Ferrell (LOFF)-type ordered states across a wide range of polarizations. I will...
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Marco ANTONELLI (CNRS - LPC Caen)22/06/2026, 12:00Talk
Quantised vortices and magnetic flux tubes are expected to govern key aspects of neutron star dynamics, but their bulk behaviour is difficult to isolate numerically due to boundary effects in finite domains. Despite an unavoidable topological obstruction, it is possible to study topological defects in periodic domains by relaxing the requirement of periodicity for the condensate's phase....
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erbil gügercinoğlu (Sabancı University)22/06/2026, 12:25Talk
An extended superfluid vortex line–magnetic flux tube interaction model is proposed for the magneto-thermal-rotational evolution of neutron stars. Applications to a sample of 12 radio pulsars with reliably measured braking indices demonstrate significantly improved agreement compared to the preexisting models. The effective moment of inertia change term for glitching pulsars is derived from...
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Riku Rantanen (Aalto University)22/06/2026, 14:30
Vortex dynamics in superfluids is strongly affected by the presence of impurities or obstacles that can act as pinning sites. Pinning of quantized vortices inside a neutron star is predicted to play an important role in its rotational dynamics and can lead to sudden changes in angular velocity known as glitches. In a system with a multicomponent order parameter, such as a spin-triplet...
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Brynmor Haskell (Universita' degli Studi di Milano, Italy)22/06/2026, 15:20
Vortex pinning in neutron stars: i.e. strong interactions between superfluid neutron vortices and normal components of the star, is a key ingredient in theoretical models for astrophysical phenomena such as pulsar glitches.
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In this talk I will describe how we can make progress in understanding the nature of pinning by studying a laboratory analogue system, i.e. superfluid Helium 3 in the... -
Ali Alpar (Sabanci University)22/06/2026, 15:45
Vortex avalanches as distinct from large fluctuations in continuous dynamics require the breaking of scale invariance. A simple model for avalanches, based on intrinsic scales of pinning forces and of substrates sustaining pinning centers is presented. Applications to pulsar glitches and analogue experiments in laboratory condensates are discussed.
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José Ernesto Alba-Arroyo (Warsaw University of Technology)22/06/2026, 16:40
We present a framework for local quantum cooling that can be efficiently applied to large-scale Fermi systems. The method introduces local Hermitian operators as a cooling potential while strictly preserving the unitarity of time evolution. Our formulation scales favorably with system size and can be seamlessly integrated into time-dependent density functional theory frameworks. We demonstrate...
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Klejdja Xhani (Politecnico di Torino, Department of Applied Science and Technology)22/06/2026, 17:05
Josephson junctions provide a fundamental platform to study the interplay between macroscopic phase coherence and dissipation, with relevance ranging from quantum technologies and superconductors to neutron stars. Ultracold atomic gases, with tunable interactions and controllable geometries, enable exploration of Josephson dynamics across the BEC–BCS crossover within a single system.
We...
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Rena Zieve (University of California, Davis)23/06/2026, 09:00
My lab has begun a superfluid helium experiment designed to exhibit glitch behavior, modeled after the Tsakadze and Tsakadze experiment from the 1970's. We levitate a bucket of helium, rotate the bucket, and let the bucket slow down while monitoring its angular velocity. We do observe glitches in which the angular velocity increases. I will discuss various effects that currently limit the...
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Dr Denys Zhuravel (Bogolyubov Institute for Theoretical Physics of the National Academy of Sciences of Ukraine)23/06/2026, 09:50
The thermodynamic properties of a system of interacting relativistic bosonic particles and antiparticles at high temperatures and densities, in the presence of the Bose-Einstein condensate, are studied. The density functional mean-field model and the scalar field model were used to calculate phase diagrams and thermodynamic quantities for different ratios of attractive to repulsive forces in...
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Giorgia Iori (Università degli Studi di Milano)23/06/2026, 10:15
Understanding vortex dynamics in three-dimensional superfluid systems emerges as a key challenge. Driven by the ultracold quantum gases laboratory that has recently been established in Milan, I will present a work [1] aimed at numerically investigating and controlling three-dimensional vortex ring formation and dynamics in trapped Bose-Einstein condensates.
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In this work, we propose and... -
Dario Ballarini (CNR Nanotec)23/06/2026, 11:10Talk
Universal scaling near phase transitions is one of the central ideas of physics, linking the growth of spatial correlations to the slowing down of dynamics. So far, direct experimental access to this critical behavior has remained largely confined to equilibrium many-body systems, and especially to static critical behavior. Here we probe how universality emerges in a driven quantum fluid of...
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David Nagy (HUN-REN Wigner RCP)23/06/2026, 12:00Talk
Cold atoms trapped in the volume of a high-finesse optical resonator [1] form a hybrid quantum system, where strong atom-light coupling leads to a bistability involving hyperfine ground states [2]. This transition can be exploited both in the preparation and in the detection of atomic quantum states. We experimentally demonstrate an optical bistability between two hyperfine ground states [3]....
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Michał Śliwiński (Warsaw University of Technology)23/06/2026, 12:25Talk
The Kelvin–Helmholtz instability (KHI) in superfluid systems with annular geometry has recently attracted significant attention. While numerical studies based on Gross–Pitaevskii and Zaremba–Nikuni–Griffin models have explained some of its dynamics, the inconsistency persists, as evidenced by incorrect predictions of the instability's growth rates. We employ the SLDA framework to simulate KHI...
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Prof. Thomas Gasenzer (Heidelberg University, Germany)23/06/2026, 14:30
Our work focuses on decaying quantum turbulence in the vicinity of an anomalous non-thermal fixed point (NTFP) characterized by slow, subdiffusive coarsening of a length scale. The NTFP is approached in the temporal evolution of a quasi-2d dilute Bose gas starting from variously sampled initial vortex configurations. The universal dynamics is accompanied by the build-up of an inverse energy...
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Anantharaman Viswanathan (Ashoka University)23/06/2026, 15:20
A neutron star is expected to contain a rotating neutron superfluid, threaded by 10^17 quantized vortices, in an environment with a much larger number of pinning sites. The interaction between these two entities, along with the spin-down of the star's crust, is thought to be the primary driver of pulsar glitches. Given reasonable computational resources, existing Gross-Pitaevskii simulations...
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Alessandro Costanzo23/06/2026, 15:45Poster
Neutron stars glitches, sudden spin-up events observed in their rotation, can be attributed to a transfer of angular momentum from an internal superfluid reservoir through a superfluid vortex-avalanche process. This research extends existing models by introducing new hypotheses in order to achieve a self-consistent description of superfluid vortex dynamics and avalanche probability....
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Lorenzo Frigato (Università degli Studi di Padova)23/06/2026, 15:50Poster
Recent experimental realizations of ultracold atom bubble traps in microgravity conditions have triggered the exploration of quantum many-body physics in curved geometries, beyond the flat-space paradigm. We investigate a two-component Fermi gas on a spherical surface, analyzing how the interplay between curvature and interactions modifies its physical properties, both at finite and zero...
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Henry Harper-Gardner (Newcastle University)23/06/2026, 15:55Poster
Bose-Einstein condensation is a ubiquitous phenomenon, present across a multitude of physical scales, from coherence among some thousands of atoms, to macroscopic superfluidity in liquid helium, up to theorised superfluid-superconducting neutrons and protons responsible for observed glitches in neutron stars. At all of these scales, questions persist around the subject of non-equilibrium...
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Armin Vahdat (University of Tübingen)23/06/2026, 16:00Poster
We present an interactive 3D Particle-In-Cell (PIC) simulation of a global pulsar magnetosphere implemented in a browser-based HTML/WebGL environment. The model self-consistently evolves electromagnetic fields and relativistic plasma by solving Maxwell’s equations on a discretized grid (Yee scheme) coupled to particle dynamics via the Lorentz force. Charged particles are advanced using a...
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Brynmor Haskell (Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences), Davide Castellani (Università degli Studi di Milano)23/06/2026, 16:05Poster
The internal magnetic field configuration of neutron stars remains a key open problem in relativistic astrophysics, with significant implications for their evolution and electromagnetic and gravitational-wave emission. In our work, we investigated the stability of axisymmetric magnetic field configurations in a $n=1$ polytropic neutron star by combining the study of Configurational Entropy...
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Héctor Briongos-Merino (University of Barcelona, ICCUB)23/06/2026, 16:40
Pulsars, i.e. fast rotating neutron stars, exhibit an intriguing phenomenon known as “Glitches”. A glitch refers to a sudden increase of the star rotation frequency, which then eventually relaxes back to its slow-down value. The underlying mechanism governing such a behavior is a big open question in the community. A possible explanation is connected to the stochastic unpinning of quantized...
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DEEPTHI GODABA VENKATA (Birla Institute of Technology and Science, Pilani)23/06/2026, 17:05
Neutron star cores could host various novel phases, ranging from a nucleonic superfluid phase to exotic high-baryon-density quantum chromodynamics (QCD) phases. Several observational signals have been discussed in the literature for such phase transitions. The current work points to a unique phenomenon, the Kibble–Zurek mechanism, in which a superfluid vortex network forms during a phase...
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Tatsuhiro Hattori (Institute of Science Tokyo)23/06/2026, 17:30
Observations of neutron stars have revealed a rapid changing in rotation velocity, known as a “Glitch” phenomenon. The glitching mechanism is thought to be related to neutron superfluidity inside neutron stars. In the inner crust region, neutrons are $^1S_0$ superfluid. While in the outer core, they behave as $^3P_2$ superfluid, which may form half-Integer vortices [1]. Vortices in different...
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Nils Andersson24/06/2026, 09:00
Owing to the extreme densities, pressures and low (on the nuclear physics scale) temperatures of their interiors, neutron stars act as cosmic laboratories for superfluid dynamics. The theoretical motivation for this is well established and pulsar glitches – sudden spin-up events followed by a gradual relaxation – provide convincing observational support. Nevertheless, and despite about half a...
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Dr Andrei Igoshev (Newcastle University)24/06/2026, 09:50
Low-field magnetars have dipolar magnetic fields of $10^{12}$--$10^{13}$ G, 10-100 times weaker than the values of magnetic-field strength $B\approx$ $10^{14}$--$10^{15}$ G used to define classical magnetars, yet they produce similar X-ray bursts and outbursts. Using direct numerical simulations of magnetothermal evolution starting from a dynamo-generated magnetic field, we show that the...
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Clara Dehman (University of Alicante)24/06/2026, 11:10Talk
Neutron stars are ultra-dense remnants of massive stellar cores, observable across the electromagnetic spectrum. Their emission reflects a complex interplay of magnetic, thermal, and structural processes operating under extreme conditions of density, temperature, and magnetic field strength—regimes unattainable in terrestrial laboratories. Understanding isolated neutron stars requires studying...
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Raj Kishor Joshi (CAMK, Warsaw, Poland)24/06/2026, 12:00Talk
Magnetars represent one of the most extreme environments in the universe, where magnetic forces are fundamentally important to understanding their behavior. These objects manifest through energetic transients such as Soft Gamma Repeaters and Anomalous X-ray Pulsars, yet the configuration and longevity of their internal magnetic architecture remain poorly understood.
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I will present results... -
William Cook (FSU Jena)24/06/2026, 12:25Talk
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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Dr Arus Harutyunyan (Byurakan Astrophysical Observatory, Yerevan State University)25/06/2026, 09:00Talk
Bulk viscosity in neutron stars plays an important role in the dynamics of binary neutron star mergers by damping density oscillations in the post-merger remnant. In this talk, I will review the computation of bulk viscosity in the warm, dense, neutrino-transparent cores of neutron stars for two possible compositions: nuclear matter and quark matter. For the nuclear matter equation of state...
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Anirudh Nemmani (Nicolaus Copernicus Astronomical Center, CAMK PAN)25/06/2026, 09:50Talk
Studying isolated asymmetric neutron stars via continuous gravitational waves has become a new approach to understanding neutron star physics, given improvements in detector sensitivity and the upcoming next-generation detectors like the Einstein Telescope, which will make detection of these signals feasible in the near future. In our work, we investigate whether corrections to the...
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Duncan Neill (University of Bath)25/06/2026, 10:15Talk
Neutron star (NS) asteroseismology is a powerful tool for probing the nature of matter inside NSs, with various oscillation modes being sensitive to different properties of matter in different regions of the star, and thus to different aspects of fundamental nuclear physics. Current asteroseismic studies however focus on particular families of oscillation modes, or rely on phenomenological...
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Wenhao Dong (University of Melbourne & OzGrav)25/06/2026, 11:10Talk
Crust-superfluid coupling plays an important role in neutron star rotation, particularly with respect to timing noise and glitches. Here, we present new timing-noise-based estimates of the crust-superfluid coupling timescale $\tau$ for 105 radio pulsars in the UTMOST dataset, by Kalman filtering the pulse times of arrival. The 105 objects are selected because they favour a two-component,...
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Matthew Ball25/06/2026, 12:00Talk
Rapidly rotating pulsars are known to undergo spontaneous increases in their rotation frequency known as "glitches" which interrupt their normal spindown rate. While the precise mechanism is unknown, this process is believed to be due to an internal exchange of angular momentum. Such a process may cause the emission of gravitational waves across multiple frequency bands and timescales which...
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Ian Jones (University of Southampton)25/06/2026, 12:25Talk
Rotating neutron stars, if deformed away from axisymmetry, produce long-lived gravitational waves. One possible source for such “mountains” is a non-axisymmetric distribution of the neutron superfluid’s vorticity, sustained by vortex pinning to the star’s solid outer crust, or to the magnetic flux tubes in the core. The Magnus force generated distorts the star, giving what we term a “Magnus...
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Gary Liu (Department of Physics, Royal Holloway University of London)25/06/2026, 14:30Talk
Vortex avalanches are believed to cause pulsar glitches, with $10^{17}$ of quantum vortices transferring angular momentum from the inner-crust superfluid to the crust of a pulsar. In this presentation, we investigate the vortex avalanches using the Gross-Pitaevskii model for a system with more than $600$ vortices in a linearly spin-down superfluid. For the first time, we showed that during...
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Nicolas CHAMEL (Université Libre de Bruxelles, Belgium)25/06/2026, 15:20Talk
The neutron superfluid present in the inner crust and outer core of a neutron star is coupled to the rest of the star due to nondissipative entrainment effects of different nature. Such effects could play an important role in the dynamics of the star. In the crust, entrainment effects are measured in terms of the superfluid density, i.e. the density of neutrons that contribute to the...
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Daniel Pęcak (Institute of Physics, Polish Academy of Sciences)25/06/2026, 15:45Talk
Astronomical observations of neutron stars provide information on kilometer scales, while the nuclear interactions that govern their properties operate on femtometer scales. Describing physical processes across such vastly different length scales requires effective theoretical models. The inner crust of a neutron star is a particularly complex system, where a lattice of nuclei strongly...
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Giorgio Almirante25/06/2026, 16:40
Neutron stars are fascinating astrophysical objects, containing matter at densities that exceeds the density of atomic nuclei. Among the most puzzling phenomena associated with them are pulsar glitches. Pulsars are rapidly rotating neutron stars, emitting beams of radiation from their magnetic poles and acting as the most precise clocks in the Universe, even surpassing the accuracy of atomic...
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Armen Sedrakian (University of Wroclaw and FIAS)25/06/2026, 17:05
We demonstrate that the interface between S-wave and P-wave paired
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superfluids in neutron stars induces a neutron supercurrent, a
charge-neutral analog of the Josephson junction effect in electronic
superconductors. The proton supercurrent entrainment by the neutron
superfluid generates, in addition to the neutral supercurrent, a
charged current across the interface. Beyond this... -
Mr Charlie Perkins (Newcastle University)25/06/2026, 17:30
Many neutron stars exhibit rotational 'glitches' caused by the collective depinning of $>10^7$ superfluid vortices. Gross–Pitaevskii (GP) and point-vortex (PV) simulations have demonstrated glitching behaviour via development of vortex avalanches with $500$-$5000$ vortices. Given that a real neuron star contains more than $>10^{13}$ vortices, simulating glitches in a global-scale model...
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Mr Tuhin Malik (CFisUC, Department of Physics, University of Coimbra)26/06/2026, 09:00Talk
The equation of state (EoS) of strongly interacting matter at the densities reached inside neutron stars (NSs) sits at the interface of low-energy nuclear theory, perturbative QCD, and multi-messenger astronomy. In this talk I will first review the current status of the zero-temperature EoS and the constraints that shape it: chiral effective field theory below nuclear saturation, perturbative...
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Melissa Mendes (Technische Universität Darmstadt)26/06/2026, 09:50Talk
Neutron star interiors are very interesting environments to probe the nuclear matter equation of state (EOS), especially at the limit of high density and temperature. In this talk, I will discuss two approaches to constraining the neutron star EOS. The first approach consists of constraining the EOS with observations of neutron star mass, radius, and tidal deformability. I will explain how...
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Valéria Carvalho26/06/2026, 10:15Talk
The equation of state (EoS) of neutron star matter encodes the relationship between pressure and density at supranuclear densities, fundamentally governing the star’s structure and observable macroscopic properties, such as mass, radius, and tidal deformability. In this work, we apply Neural Posterior Estimation (NPE) with conditional normalising flows to infer the EoS from synthetic...
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Mihailo Cubrovic (Institute of Physics Belgrade)26/06/2026, 11:10Talk
We construct a description of hydrodynamics and superfluidity for a class of strongly coupled conformal (quantum critical) systems within the framework of gauge/gravity duality (holographic duality). We first review the basic idea of holographic duality and the state-of-the-art results on holographic superfluids, which are dual to black holes with thermal horizons. We then extend these results...
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Mr Tiago Custódio26/06/2026, 12:00Talk
Light nuclei are found in core-collapse supernova matter and in binary neutron star mergers. Their abundance can affect the dynamics and properties of supernovae [1-3] and binary neutron star mergers [4-8], both directly through their weak reactions with the surrounding medium, and indirectly through their competition with heavy nuclei [9], which can modify the proton fraction and the size of...
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Milena Albino (University of Coimbra)26/06/2026, 12:25Talk
Neutron stars (NSs) are interesting objects capable of reaching densities unattainable on Earth. The properties of matter under these conditions remain a mystery. Exotic matter, including quark matter, may be present in the NS core. In this work, we explore the possible compositions of NS cores, in particular, the possible existence of large quark cores. We use the relativistic mean-field...
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Saso Grozdanov (University of Edinburgh, University of Ljubljana)26/06/2026, 14:30
In this talk, I will review recent progress in formulating effective field theories for hydrodynamic-like states with higher-form symmetries. These symmetries are associated with the conservation of extended objects that constitute the fluid. One example is a plasma composed of one-dimensional strings, or magnetic flux lines, whose dynamics are described by magnetohydrodynamics. I will discuss...
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Prashant Thakur (Yonsei University)26/06/2026, 15:20
We present an amortized (train-once-use-many) simulation-based inference framework for constraining the nuclear equation of state of neutron stars within density-dependent relativistic mean-field models. The aim is to validate Neural Posterior Estimation (NPE) as a fast alternative to conventional nested-sampling analyses, while preserving full Bayesian posterior quantification. We benchmark...
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Rafael Cardoso (Federal University of Santa Catarina and University of Coimbra)26/06/2026, 15:45
Neutron stars are objects described by the quantum chromodynamics (QCD), which predict a deconfined quark phase for high densities. It is possible that quark matter can be reached in the core of neutron star surrounded by a hadronic phase. For an hybrid star, the two solar mass neutron star constraint requires a stiff equation of state (EoS) for intermediate densities that supports a soft core...
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Luigi Scurto (Laboratori Nazionali del Sud, Infn)26/06/2026, 16:40
In our work, we use bayesian inference to study how the inclusion of a scalar-isovector interaction channel within a RMF framework can affect the threshold for the direct URCA process in the core of neutron stars. We also study the effect of proton pairing by including a simplified model for the proton 1S0 pairing gap. The results show that the inclusion of the new interaction channel can...
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Afonso Ávila (University of Coimbra)26/06/2026, 17:05
We perform a statistical analysis of the thermal evolution of isolated neutron stars (NSs) by confronting theoretical cooling curves with luminosity–age measurements for 24 sources. For each object, we explore five purely nucleonic equations of state—APR4, FSU2R, DD2, IST, and NL3$\omega\rho$—combined with representative models of neutron superfluidity and proton superconductivity, while...
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Thippayawis Cheunchitra (The University of Melbourne)26/06/2026, 17:30
Neutron star glitches may be caused by the sudden unpinning and collective movement of vortices in the superfluid condensate inside the star, also known as vortex avalanches. The metastable vortex configuration between avalanches is determined by the far-from-equilibrium avalanche dynamics and is nonaxisymmetric in general, producing a small but nonzero current quadrupole moment which...
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