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Tiziano Abdelsalhin (Sapienza University of Rome)Poster
The lack of information on the nature of the neutron star (NS) core at supra-nuclear densities, has so far prevented a unique description of its equation of state (EoS). Future gravitational wave (GW) detections by second and third-generation of ground-based interferometers will shed new light on this open problem. The income of new and detailed experimental data will help to reconstruct the...
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Mr Marko Sossich (University of Zagreb, Faculty of Electrical Engineering and Computing, Department of Physics)Poster
We study the static spherically symmetric configurations of the perfect fluid described by the polytropic equation of state (EoS) in the $f(T)$ extended theory of gravity. For $f(T) = T$ , where $T$ is the torsion scalar, this gravity theory is equivalent to GR and is known as its teleparallel equivalent (TEGR). In this work, we provide numerical evidence for the existence of the polytropic...
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Mr Eemeli Annala (University of Helsinki)Poster
In this poster, I will present results from a recent study aimed at finding the most plausible Equation of State (EoS) for neutron star matter, combining available first principles calculations with up-to-date observational data. Our EoSs are composed of piecewise polytropes interpolating between known limits from quantum Monte Carlo at low densities and perturbative QCD at high densities....
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Mr Nicolas Baillot d'Etivaux (Institut de Physique Nucléaire de Lyon)Poster
Neutron stars are one of the most compact objects in the universe. They are made of a totally degenerated fermion gas, but their interior composition remains unknown. Several scenarios exist and some of them predict phase transitions from ordinary nuclear matter to mesons condensates, hyperonic matter, quark gluon plasma in the core, or even absolutely stable strange quark matter. In order to...
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Ms zahra Asadi Aghbolaghi (zanjan University)Poster
Equation of state of nuclear matter using AV8’ and AV6’ potentials
Z. Asadi and M. Bigdeli
Department of Physics, University of Zanjan, Zanjan, Iran
Go to contribution pageThe equation of state (EOS) of asymmetric nuclear matter have long been realized as a crucial parameter to understand the structural properties of neutron-rich nuclei and neutron stars. The behavior of the EOS of nuclear matter... -
Mr Sebastian Völkel (University of Tübingen)Poster
With the repeated detection of gravitational waves by LIGO, new frontiers in astrophysics and gravitational physics are waiting to be explored. The work we present is dedicated to the theoretical description of ultra compact objects, more recently also called exotic compact objects (ECOs). Using analytic and semi-analytic techniques we focus on gravitational perturbations, where the associated...
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28. High-frequency noise in GRO J1744−28: Evidence for a radiation-pressure dominated accretion diskJuhani Mönkkönen (University of Turku)Poster
Neutron stars accreting matter via an accretion disk offer a unique way to examine the interaction of radiation and matter under extreme conditions. If the neutron star has an ultra-strong magnetic field, the disk is truncated at the so-called magnetospheric radius and matter is guided onto the neutron star surface where its energy is released in X-rays (so-called X-ray pulsars). The...
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Cosima BreuPoster
The merger of binary neutron stars can result in the formation of a massive, highly magnetized neutron star as remnant.
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We study the magnetically driven wind launched from those objects.
The remnant is modelled as an axisymmetric, differentially rotating supramassive neutron star. A realistic equation of state is employed and neutrino emission is taken into account via a leakage scheme. -
Tuomo Salmi (University of Turku)Poster
We present a method that can be used to constrain masses and radii of neutron stars. The method is suitable for accreting millisecond pulsars, where a rapidly rotating neutron star accretes matter from a relatively low mass companion star onto the magnetic poles of the neutron star. Because of the accretion, we observe radiation from two ”hot spots” on the neutron star surface. This...
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Elias Roland Most (Goethe University Frankfurt)Poster
Binary neutron star mergers are now thought to be a main source of r-process nucleosynthesis, by which most of the heavy elements in our universe have been produced. Furthermore, such systems also constitute a prime candidate for the formation of short gamma ray bursts, which can serve as important electromagnetic counterparts to future gravitational wave detections of such systems.
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Using a... -
Dr Matteo Bugli (Max Planck Institute for Astrophysics)Poster
Geometrically thick tori with constant specific angular momentum have been widely used in the last decades to construct numerical models of accretion flows onto black holes. Such discs are prone to a global non-axisymmetric hydrodynamical instability, known as Papaloizou-Pringle instability (PPI), which can redistribute angular momentum and also lead to an emission of gravitational waves. It...
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Mr Gabriele BozzolaPoster
The stability against gravitational collapse of the remnant left by a merger of binary neutron stars is of great interest in gravitational-wave astronomy. This property can be explored with simulations in full general relativity, which are often computational extremely demanding. A well-established result in this landscape is that the rotation of the remnant is a crucial factor in determining...
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Zahra Altaha MotaharPoster
Neutron stars are some of the most fascinating objects in the universe. Due to their compactness and high density, they represent an ideal laboratory to test alternative theories of gravity. In addition, studying these compact objects will expand our limited knowledge of the properties and the physics of nuclear matter at the very high density found inside neutron stars.
We demonstrate the...
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Weih Lukas (Institute for Theoretical Physics, Goethe University)Poster
Uniformly rotating neutron stars have been part of many studies in theoretical astrophysics. While a stability criterium against gravitational collapse to a black hole is well known for this type of star, it is not for differentially rotating neutron stars, which are thought to be the outcome of binary neutron star mergers. The stability of the merger remnant has important implications on the...
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Mr Simon Giraud (GANIL)Poster
In the last decades the numerical simulations of core-collapse supernovae have greatly improved, treating now general relativity and multi-dimensional hydrodynamic phenomena such as convection, rotation, instabilities, neutrino transport and shock wave propagation. Although the remarkable advances, the best 3D models still fail to reproduce the characteristics of observed core-collapse...
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Mr Oliver Lux (University of Jena)Poster
Knowing neutron star (NS) ages is important to better understand the formation and evolution of the Galactic NS population. The characteristic age is only a rough estimate, based on assumptions like pure magnetic dipole braking and a negligible birth period. Since these assumptions are not justified for many pulsars, we use kinematic simulations for 162 non-recycled pulsars and are able to...
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Ms Kateřina Goluchová (Silesian university in Opava)Poster
Spectroscopic analysis of the radiation of binary stellar systems, which contain a neutron star or a black hole, is still among the most topical areas of relativistic high energy astrophysics. The strong dependence of the spectral profiles on the configuration of the source-observer system suggests that the spectral profiles can carry substantial information about the compact object and its...
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Debora LančovaPoster
Accretion structures in the vicinity of neutron stars are significantly influenced by the radiation emitted from the surface of stars and from the boundary layer. Apart from the radiation pressure, the accreted matter is also affected by the Poynting-Robertson effect, which causes angular momentum loss and therefore acts as an additional source of viscosity in the disk. Using numerical...
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Thomas CarreauPoster
We recently developed a density functional theory based empirical approach using the extended Thomas-Fermi theory, allowing an analytical evaluation of the energy functional of the different components of stellar matter. The main advantage of this unified approach is that the crust-core transition is consistently treated, allowing to estimate upper bounds on observables such as pulsar glitches...
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