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José Manuel Alarcón (Universidad de Alcalá)9/21/22, 9:00 AM
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Andreas Nogga (Forschungszentrum Jülich)9/21/22, 9:30 AM
One key quantity for better constraining the contributions of hyperons to the equation of state of neutron matter is the $\Lambda$-neutron interaction. In absence of $\Lambda$-neutron scattering data, isospin symmetry is usually assume and interactions are determined by fitting to $\Lambda$-proton data.
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But charge symmetry breaking (CSB) of the $\Lambda$-nucleon interaction has been well... -
Aleksi Kurkela (University of Stavanger)9/21/22, 10:00 AM
Calculations of equation of state of QCD become reliable at the densities of around 40 saturation densities. These densities are well beyond those that are reached within the cores of even the most massive neutron stars. However, knowing the equation state at these extreme densities still gives us robust information at lower densities because of global requirements imposed by causality,...
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Arnau Rios (Universitat de Barcelona)9/21/22, 10:30 AM
In this talk, I will discuss the thermal index of low-density, high-temperature matter, motivated by gravitational wave observations of neutron-star binaries. We use the virial approximation to include nuclear interaction effects. In pure neutron matter, we find a relatively temperature-independent thermal index close to $\Gamma_\text{th} \approx 5/3$, with a negligible contribution from...
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Prof. Nicolas Chamel (Univ. Libre de Bruxelles)9/21/22, 11:30 AM
Formed in the aftermath of gravitational core-collapse supernova explosions, neutron stars are the most compact observed stars. Their average density exceeds that found inside the heaviest atomic nuclei. Neutron stars are also endowed with the highest magnetic fields known, which can reach millions of billion times that of the Earth. According to our current understanding, a neutron star is...
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Germán Lugones (Universidade Federal do ABC)9/21/22, 12:00 PM
Abstract: Hybrid stars containing a quark matter core and a hadronic mantle may contain a sharp interface if the surface tension of dense matter is sufficiently high. When such a star is perturbed, conversion reactions may occur around the quark-hadron splitting surface. We show that the reaction speed has strong effects on the quasinormal mode spectrum and on stellar stability. In...
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Alessandro Roggero (University of Trento)9/21/22, 12:30 PM
In this presentation I will talk about the prospects of using quantum computing for the simulation of nuclear many-problems. Thanks to the rapid growth of quantum platforms it is already possible to test some simulation schemes on small scale and I will show some recent results obtained for a simple model of light nuclei. I will conclude with a perspective on what we could expect quantum...
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9/21/22, 2:30 PM
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Adriana R. Raduta (IFIN-HH, Bucharest)9/21/22, 3:00 PM
Studies of explosive astrophysical systems as core-collapse supernovae and binary neutron star mergers require equations of state (EOS) covering wide domains of baryon number density 10^{-14} fm^{-3} ≤ n_B ≤ 1.5 fm^{-3} , temperature 0 ≤ T ≤ 100 MeV and electron fraction 0 ≤ Y_e=n_e /n_B ≤ 0.6. Advances in this field during the last decade make that about 100 such EOS are presently available...
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Kostas Glampedakis (Universidad de Murcia)9/21/22, 3:30 PM
This talk is a compact up-to-date review of astrophysical neutron star mass-radius measurements and a discussion of their relevance for the nuclear equation of state physics.
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Eva Lope Oter (Universidad Complutense de Madrid)9/21/22, 4:00 PM
We provide equations of state (EoS) for matter at attainable densities in physical neutron stars at zero and finite temperature. These EoS are derived from current knowledge of the uncertainty bands of chiral effective field theories and pQCD constraints. The results are independent of neutron star observations and can be used to test general relativity as well as theories beyond GR, such as...
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Owe Philipsen9/22/22, 9:00 AM
Lattice QCD with heavy dynamical quarks reduces to a three-dimensional effective theory of Polyakov loops, after truncated character and strong coupling expansions. This effective theory has a substantially milder sign problem than full QCD, and can either be simulated or treated successfully by analytical methods. This allows for investigations of the heavy QCD phase diagram as a function of...
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Veronica Dexheimer (Kent State University)9/22/22, 9:30 AM
Due to the present large uncertainty in the composition and interactions of dense nuclear matter, there are many different equation of state (EoS) models that can fulfill nuclear and astrophysical constraints. EoS repositories allow for a fast exchange of EoS between providers and simulation users, accelerating our understanding of dense matter. I discuss different EoS repositories, focusing...
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Helena Pais (University of Coimbra)9/22/22, 10:00 AM
Light (e.g. deuterons, tritons, helions, $\alpha-$particles), and heavy (pasta phases) nuclei exist in nature in core-collapse supernova matter and neutron star (NS) mergers, where temperatures of the order of 50 to 100 MeV may be attained. The appearance of these clusters can modify the neutrino transport, and, therefore, consequences on the dynamical evolution of supernovae and on the...
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Theo Motta (Justus Leibig University Gießen)9/22/22, 10:30 AM
For a few decades now, the possibility of spatially inhomogeneous crystalline phases in the QCD phase diagram has been investigated. Studies based on models of QCD such as NJL or quark-meson models do show such phases, however, no unambiguous confirmation that they happen in QCD has been achieved yet. In this talk, I will review the current state of the search for inhomogeneities and discuss...
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Isaac Vidana ( Istituto Nazionale di Fisica Nucleare )9/22/22, 11:30 AM
We will review the present status of the role played by hyperons in determining the properties of neutron and proto-neutron stars. In particular, we review the so-called “hyperon puzzle”, i.e., the problem of strong softening of the equation of state of dense matter due to the presence of hyperons which leads to maximum masses of compact stars that are not compatible with the recent...
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Stefano Burrello (Institut für Kernphysik, Technische Universität Darmstadt, Germany)9/22/22, 12:00 PM
Phenomenological models which make use of energy density functionals (EDFs) represent the reference choice nowadays for an unified treatment of the neutron star matter Equation of State. Nevertheless, the empirical character reduces the predictive power of these approaches, when applied beyond the domain on which they have been determined.
As a common drawback, for example,...
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9/22/22, 2:30 PM
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Juan Nieves (IFIC Valencia)9/22/22, 3:00 PM
A quick overview of the spectroscopy of negative-parity Lambda resonances.
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Dr Mikhail Beznogov (National Institute for Physics and Nuclear Engineering (IFIN-HH))9/22/22, 3:30 PM
We present one of the first results obtained with NSCool 2D Rot, a major upgrade of 1D neutron stars thermal evolution code NSCool by D. Page. Our new code allows to model thermal evolution of axisymmetric rotating neutron stars with arbitrary rotation frequencies up to the mass shedding limit in full general relativity. As an application, we address the question of cooling of rapidly...
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Prof. José Antonio Oller (Universidad de Murcia)9/22/22, 4:00 PM
We resum the ladder diagrams for the calculation of the energy per particle E/A of a spin 1/2 fermion many-body system in terms of any given vacuum two-body scattering amplitudes. The partial-wave decomposition of the in-medium two-body scattering amplitudes is worked out, and the expression for calculating E/A in a partial-wave amplitude expansion is also given. The case of contact...
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José C. Jiménez (University of São Paulo)9/22/22, 5:00 PM
In recent years it has become clear that in order to correctly interpret the many observables obtained for neutron stars (NS) such as their masses, radii and tidal deformabilities, one needs a better understanding of its equation of state at baryon densities of around 5 times the nuclear saturation density where a phase transition between hadronic and quark matter is also possible having...
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David Barba González (Univ. of Salamanca)9/22/22, 5:30 PM
We perform microscopic Molecular Dynamics simulations to study crystallization energetics in the outer crust of Neutron Stars (NSs). We consider the approximation of one component plasma (OCP) and multicomponent plasma (MCP) to take into account contamination for accreting objects. We include Ewald summation techniques for screened interactions to allow a more efficient energy calculation and...
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9/22/22, 6:00 PM
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Niko Jokela (University of Helsinki)9/23/22, 11:30 AM
Holographic techniques are particularly fit to analyzing matter at extreme conditions where QCD matter is strongly coupled. Combining predictions of the holographic model with state-of-the-art effective field theory models of nuclear matter, I construct a family of feasible “hybrid” equations of state which cover both the quark matter and nuclear matter phases. The model predicts, among other...
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Carlos Hoyos (Universidad de Oviedo)9/23/22, 12:00 PM
The transport properties of dense QCD matter play a crucial role in the physics of neutron stars and their mergers, but are notoriously difficult to study with traditional quantum field theory tools. Specializing to the case of unpaired quark matter in beta equilibrium, we approach the problem through the machinery of holography, and derive results for the electrical and thermal conductivities...
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Oleksii Ivanytskyi (University of Wroclaw)9/23/22, 12:30 PM
We outline the role that an early deconfinement phase transition from normal nuclear matter to a color superconducting quark-gluon plasma phase plays for the phenomenology of supernova explosions and binary neutron star mergers. To this end we extend the compact star equation of state (EoS) from vanishing to moderately high temperatures that become accessible in the CBM experiment at FAIR. We...
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Mario Martinez (ICREA/IFAE-Barcelona)9/23/22, 2:30 PM
I present the details of the Einstein Telescope Project (ET), its current design, its scientific goals and the first steps towards the definition of the ET Collaboration and its model for governance. Special emphasis is put in aspects related to the Spanish contributions and
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the opportunities for scientific and industrial engagement. -
Edoardo Giangrandi (CFisUC, University of Coimbra)9/23/22, 3:00 PM
We study the impact of asymmetric fermionic and bosonic dark matter on neutron star properties, including tidal deformability, maximum masses, radii, etc. The conditions at which dark matter particles tend to condensate in the core of the star or create an extended halo are presented. We show that dark matter condensed in a core leads to a decrease of the total gravitational mass and tidal...
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Naresh Kumar Patra (BITS Pilani K K Birla Goa Campus, NH-B, South Goa, Goa, Pin-757040)9/23/22, 4:30 PM
We apply Bayesian approach to construct a large number of minimally constrained equations of state (EoSs) and study their correlations with a few selected properties of a neutron star (NS). Our set of minimal constraints includes a few basic properties of saturated nuclear matter and low density pure neutron
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matter EoS which is obtained from a precise next-to-next-to-next-to-leading order... -
Tyler Gorda (TU Darmstadt)9/23/22, 5:00 PM
At asymptotically high densities, the neutron-star-matter equation of state (EOS) must approach the EOS of beta-equilibrated QCD matter, as calculated directly within the fundamental QCD theory. This nontrivial constraint at high density, pressure, and chemical potential impacts the inference of the neutron-star-matter EOS at even lower densities. In this talk, I show within a Bayesian...
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Constança Providência (University of Coimbra)
The general behavior of the nuclear equation of state (EOS), relevant for the description of neutron stars and possible signatures of the presence of hyperons inside neutron stars are studied within a Bayesian approach applied to a set of models based on a density-dependent relativistic mean-field description of nuclear matter. The EOS is subjected to a minimal number of constraints based on...
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Arpan Das (Institute of Nuclear Physics Polish Academy of Sciences Krakow, Poland)
We investigate the effect of dark matter components inside a neutron star using gravitational wave constraints coming from a binary neutron star merger. We study fermionic dark matter interacting with nucleonic matter via the Yukawa interaction inside the neutron star, as well as, density-dependent dark matter components
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inside neutron stars. We argue that the admixture of dark matter inside...
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