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Constanรงa Providencia (University of Coimbra)15/06/2015, 14:00It will be discussed how the crust-core matching influences the NS radius and the crust thickness within relativistic mean-field nuclear models. A set of models that predict 2$M_\odot$ stars will be considered. It will be proposed an adequate crust-core matching. The inner crust will described in the Thomas-Fermi approximation within the single heavy cluster approach. The effect of...Go to contribution page
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Dr Michaล Bejger (N. Copernicus Astronomical Center, PAS)15/06/2015, 14:25Using a recent equation of state (Benic et al., 2015, A&A 577, A40) I will discuss the stability of rotating neutron stars with strong phase transitions (so-called twin family of neutron stars). The existence of an instability region separating the twin families - a direct outcome of the strong phase transition - creates several astrophysical implications that are interesting from the...Go to contribution page
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Prof. Debades Bandyopadhyay (Saha Institute of Nuclear Physics)15/06/2015, 14:50Supernova explosions are spectacular astronomical events. At the same time, the understanding of the final journey of a massive star after its fuel has been exhausted is a challenging problem. The outcome of it is a core collapse supernova and the residue may take the form of either a neutron star or a black hole. The core collapse supernova explosion mechanism is being investigated over...Go to contribution page
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Dr Helena Pais (University of Coimbra)15/06/2015, 15:15The pasta phase in core-collapse supernova matter (finite temperatures and fixed proton fractions) is studied within relativistic mean field models. Three different calculations are used for comparison, the Thomas-Fermi (TF), the Coexisting Phases (CP) and the Compressible Liquid Drop (CLD) approximations. The effects of including light clusters in nuclear matter and the densities at which...Go to contribution page
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Ms Hai Tan Ngo (Vinatom,Vietnam/IPNLyon, France)15/06/2015, 15:40A consistent Hartree-Fock study of the hot, beta-stable baryonic matter of proto-neutron star (PNS) is done based on several choices of the effective (density dependent) nucleon-nucleon interaction, which have been successfully used in different nuclear structure and reaction studies. The equations of state associated with different behaviors of the symmetry energy at supranuclear densities...Go to contribution page
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Dr Peter Kovacs (Wigner RCP)15/06/2015, 16:35Chiral phase transition is investigated in an $SU(3)_L \times SU(3)_R$ symmetric vector meson extended linear sigma model with additional constituent quarks and Polyakov loops (extended Polyakov quark meson model). The parameterization of the Lagrangian is done at zero temperature in a hybrid approach, where the mesons are treated at tree-level, while the constituent quarks at 1-loop...Go to contribution page
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Dr Matthias Hempel (Basel University)15/06/2015, 17:00Cluster formation is a fundamental aspect of the equation of state (EOS) of warm and dense nuclear matter such as can be found in supernovae (SNe). Similar matter can be studied in heavy-ion collisions (HIC). We use the experimental data of Qin et al. [Phys. Rev. Lett. 108, 172701 (2012)] to test calculations of cluster formation and the role of in-medium modifications of...Go to contribution page
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Dr Takami Kuroda (University of Basel)15/06/2015, 17:25In this talk, we present our recently performed 3D fully relativistic long term simulations (Tpb~300-400ms) of gravitational collapse of massive progenitor stars with adopting several modern EoSs of Hempel et al.'12 and of Steiner et al.'13. Through these multiple EoSs and progenitor models, we found more massive progenitor star and softer equation of state lead to more vigorous SASI activity...Go to contribution page
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Prof. Dubravko KLABUCAR (Physics Department, PMF, Zagreb University)15/06/2015, 17:50The analytic structure of certain Ansaetze for quark propagators in the nonperturbative regime of QCD is investigated. When choosing physically motivated parameterization of the momentum-dependent dressed quark mass function M(p^2), with definite analytic structure, it is highly nontrivial to predict and control the analytic structure of the corresponding nonperturbative quark...Go to contribution page
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Mr Peter Pรณsfay (Eรถtvรถs Lรณrรกnd University)16/06/2015, 14:00Functional renormalization group (FRG) is an exact method for taking into account the effect of quantum fluctuations in the effective action of the system. The FRG method applied to effective theories of nuclear matter yields equation of state witch incorporates quantum fluctuations of the fields. Using the local potential approximation the equation of state for Walecka-type models of...Go to contribution page
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Dr Kristian Petrik (Institute of Physics, Slovak Academy of Sciences)16/06/2015, 14:25Modern and accurate observations of compact stars are invaluable sources of very important information about dense nuclear matter. One of the biggest breakthroughs in this field is definitely an experimental confirmation of the existence of very massive pulsars that brought new and very powerful constraints on all model descriptions. Our aim is to develop a relativistic energy density...Go to contribution page
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Dr Evgeni Kolomeitsev (Matej Bel University)16/06/2015, 14:50The equation of state of cold baryonic matter is studied within a relativistic mean-field model with hadron masses and coupling constants depending on the scalar field. All hadron masses undergo a universal scaling, whereas the coupling constants can scale differently. The proper choice of the scaling function allows to control stiffness of the equation of state in different energy range. The...Go to contribution page
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Dr Anthea Francesca Fantina (Institut d'Astronomie et d'Astrophysique, Universitรฉ Libre de Bruxelles)16/06/2015, 15:15In this talk, a set of unified equations of state (EoSs) of neutron-star matter calculated within the nuclear energy-density functional theory, and based on generalised Skyrme energy-density functionals developed by the Brussels-Montreal collaboration, will be presented. The structure of neutron stars constructed with these EoSs will be discussed in connection with both recent astrophysical...Go to contribution page
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Dr David Alvarez-Castillo (Joint Institute for Nuclear Research)16/06/2015, 15:40In order to prove the existence of a critical end point (CEP) in the QCD phase diagram it is sufficient to demonstrate that at zero temperature $T=0$ a first order phase transition exists as a function of the baryochemical potential $\mu$, since it is established knowledge from ab-initio lattice QCD simulations that at $\mu=0$ the transition on the temperature axis is a crossover. We...Go to contribution page
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Dr Aleksi Vuorinen (University of Helsinki)16/06/2015, 16:35I will describe what is currently known about the behavior of the Equation of State (EoS) of cold and dense quark matter based on first principles calculations utilizing perturbation theory in the deconfined phase of QCD. In addition, I will argue that by combining this information with known results on the EoS of low-density nuclear matter, it is possible to very efficiently constrain the...Go to contribution page
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Dr Isaac Vidana (University of Coimbra)16/06/2015, 17:00We construct two-meson exchange three-baryon potentials between two nucleons and one hyperon (NNY). Our NNY potentials are built in order to be consistent with the most recent version of the two-body nucleon- hyperon (NY) potential of the Juelich group. In particular, we focus on the NNฮ and NNฮฃ forces since the ฮ and ฮฃโ are the first hyperons expected to appear in microscopic...Go to contribution page
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144. Properties of neutron-star crusts with accurately calibrated nuclear energy density functionalsDr Nicolas Chamel (Universitรฉ Libre de Bruxelles)16/06/2015, 17:25Observations from ground- and space-based instruments have lead to the discovery of remarkable astrophysical phenomena that are thought to be intimately related to the physics of neutron-star crusts like pulsar sudden spin-ups (so called โglitchesโ), quasi-periodic oscillations in the giant flares from soft gamma-ray repeaters, X-ray bursts and superbursts, or the cooling of quasi-persistent...Go to contribution page
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Mr Erbil GรGERCINOGLU (Istanbul University Astronomy and Space Sciences Department)16/06/2015, 17:50As theoretical calculations and recent simulations indicate, neutron stars must have a stronger toroidal field component in the outer core which surrounds the poloidal field. Then, this toroidal field in the form of flux lines will offer pinning sites for vortex lines similar to the conditions in the inner crust. As we have shown, the moment of inertia of the corresponding region can be larger...Go to contribution page
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Mr Francesco Coti Zelati (Anton Pannekoek Institute for Astronomy, University of Amsterdam)18/06/2015, 14:00In 2013 April a new magnetar, SGR 1745โ2900, was discovered as it entered an outburst at only 2.4 arcsec angular distance from Sagittarius Aโ, the supermassive black hole at the centre of the Milky Way. The new source was detected both in the radio and X-ray bands, with a peak X-ray luminosity L_X โผ 5 ร 10^{35} erg s^{โ1}. I will present the results of the long-term Chandra (25 observations)...Go to contribution page
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Dr Brynmor Haskell (University of Melbourne)18/06/2015, 14:25Pulsar glitches, i.e. sudden jumps in the frequency of spinning down pulsars, are thought to be the direct manifestation of a superfluid component in the pulsar interior. The exact mechanisms that gives rise to these phenomena has, however, remained a mystery for over 40 years. The wealth of data that is now available suggests that glitches may be the consequence of the superfluid being in a...Go to contribution page
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Dr Lorenzo Ducci (University of Tuebingen)18/06/2015, 14:50Glitches have been observed in isolated pulsars, while a clear detection in accretion-powered X-ray pulsars is still lacking. We use the "snowplow" model for pulsar glitches of Pizzochero (2011) and starquake models to determine for the first time the expected properties of glitches in accreting pulsars and their observability. We also investigate the possibility that anti-glitches occur in...Go to contribution page
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Dr Anna Bilous (Radboud University Nijmegen)18/06/2015, 15:15PSR B0943+10 is one of the best examples of the rare class of mode-switching pulsars. Unlike most of the pulsar population, PSR B0943+10 has two stable modes of radio emission, each with its own distinct radio profile morphology and sinlge-pulse behaviour. The pulsar switches between "Bright" and "Quiet" modes once every few hours and the transition takes less than a few stellar rotations. The...Go to contribution page
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Ms Alice Borghese (Anton Pannekoek Institute for Astronomy)18/06/2015, 16:10In this talk I would like to report the discovery of a narrow phase-dependent absorption feature in the X-ray spectrum of the nearby X-ray Dim Isolated Neutron Star RX J0720.4-3125. This feature was discovered performing a detailed phase-resolved spectral analysis using XMM-Newton observations which cover 12 years. The line seems to be stable in time over this timespan and is present in...Go to contribution page
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Dr Blagoy Rangelov (The George Washington University)18/06/2015, 16:35It is extremely rare when a binary is found to be associated with supernova remnant. It is also rare when a high-mass binary is bright in gamma-rays. SNR G284.3-1.8 appears to be a unique remnant hosting such a binary. We present results from Chandra and XMM-Newton observations of the SNR and the binary. G284.3-1.8 has asymmetrically distributed Mg-rich ejecta, which has only been observed in...Go to contribution page
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Mr Gregory Ashton (University of Southamton)18/06/2015, 17:00Variability in the arrival times of pulsars, often collectively known as timing noise, poses a significant opportunity to learn about the physics of neutron stars. The diversity of observed timing noise is matched by the number of the models attempting to explain the phenomenon, but no single model can claim to provide a complete explanation. Recent results in the literature suggest that...Go to contribution page
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Dr Rana Nandi (FIAS)18/06/2015, 17:25We study the structure of nuclear matter at sub-saturation densties by quantum molecular dyanamics simulations. In particular, we investigate the role of nuclear symmetry energy and its slope on the properties of pasta phases.Go to contribution page
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