-
Dr V Cardoso (IST - University of Lisbon)05/09/2016, 09:05
-
Dr U. Sperhake (University of Cambridge)05/09/2016, 11:00
-
Dr L. Rezzolla (Institute for Theoretical Physics, Frankfurt am Main)05/09/2016, 14:30
-
Dr P Freire (Max Planck Institute - Bonn)05/09/2016, 16:30In this lecture, I will introduce some basic concepts related to neutron stars, radio pulsars and their evolution. I then describe in detail timing of radio pulsars in binary systems, using the results from the first binary pulsar, PSR B1913+16, as an important example. First, I describe how pulsar timing of this system was used to determine the masses of the components, and then I describe...Go to contribution page
-
Dr V Cardoso (IST - University of Lisbon)06/09/2016, 09:00
-
Dr L. Rezzolla (Institute for Theoretical Physics, Frankfurt am Main)06/09/2016, 11:00
-
Dr U. Sperhake (University of Cambridge)06/09/2016, 14:30
-
E. Gourgoulhon (Observatoire de Paris)06/09/2016, 16:30
SageManifolds [1] is an extension of the Python-based modern computer algebra system SageMath [2] towards differential geometry and tensor calculus. We shall use it to perform computations and draw figures regarding neutron star and black hole spacetimes. The School participants are encouraged to install the free software SageMath on their computer prior to the school or to open a free account...
Go to contribution page -
Dr I. Jones (University of Southampton)07/09/2016, 09:00Gravitational Wave source Modelling 1: Basic formalism In this lecture I will present the so-called quadrupole formalism for describing the gravitational wave emission from a neutron star. Within this formalism, General Relativity is treated as a correction to Newtonian physics. I will sketch out the key formulae, and show how they lead to some well known results for the gravitational...Go to contribution page
-
Dr A. Le Tiec (Observatoire de Paris)07/09/2016, 11:00In this lecture, I will give an introduction to the analytical approximation methods that are used to model the orbital dynamics and gravitational-wave emission of binary systems of compact objects (neutrons stars and black holes), namely the post-Newtonian approximation, black hole perturbation theory and the gravitational self-force formalism, and the effective one-body model. The key ideas...Go to contribution page
-
Dr V. Dexheimer (Kent State University)07/09/2016, 14:30I will present a lecture about the modifications introduced in the EOS of dense by the presence of strong magnetic fields. We know that magnetic fields of up to 10^15 G have been measured on the surface of neutron stars and a field of 10^16 have been measured somewhere inside a neutron star. We speculate further that magnetic fields of more than 10^18 Gauss can exist in the center of massive...Go to contribution page
-
Dr M. A. Papa (Max Planck Institute for Gravitational Physics - Hannover)08/09/2016, 09:00
-
Dr I. Jones (University of Southampton)08/09/2016, 11:00
Gravitational Wave source Modelling 2: Applications
In this lecture I will apply the basic formalism described in my previous lecture to the gravitational wave emission from neutron stars in various contexts. In particular I will discuss rotating non-axisymmetric neutron stars, making the connection between neutron star microphysics and possible gravitational wave amplitudes explicit.
Go to contribution page -
Dr F. Burgio (INFN - Catania)08/09/2016, 14:30
-
Dr E. Kantor (Ioffe Physical-Technical Institute of the Russian Academy of Sciences, St.-Petersburg)08/09/2016, 16:30In this lecture I will review the main features of bulk and shear viscosities in application to neutron stars. Starting with the discussion of the main processes contributing to both viscosities in superdense matter I will proceed to the effects of superfluidity. I will show how the baryon superfluidity affects the functional dependences and values of the coefficients and, moreover, how it...Go to contribution page
-
Dr K. Glampedakis (University of Tuebingen)09/09/2016, 09:00This lecture provides a detailed discussion of gravitational wave-driven instabilities in neutron stars and highlights their implications for the photon and gravitational wave astronomy of these objects. The emphasis is given on the analysis of the (most promising) r-mode and f-mode instabilities: we discuss the, occasionaly exotic, physics that determines their instability “windows”,...Go to contribution page
-
Sofija Antic (GSI)09/09/2016, 11:00
The equation of state (EOS) of dense matter is essential for modeling compact astrophysical objects and sets the conditions for the creation of chemical elements in the universe. To provide it, we use the generalized DD-NLD relativistic mean-?field model (RMF) with density-dependent nucleon-meson couplings and higher-order derivative couplings between nucleons and mesons. The model is extended...
Go to contribution page -
Christine Farrugia09/09/2016, 11:30
Abstract: Starting from a Geometrothermodynamics metric for the space of thermodynamic equilibrium states in the mass representation, numerical techniques are used to analyse the thermodynamic geodesics of a supermassive Reissner-Nordström black hole in isolation. Appropriate constraints are obtained by taking into account the processes of Hawking radiation and Schwinger pair-production. It...
Go to contribution page -
Vasiliy Dommes (Ioffe Institute)09/09/2016, 12:00
-
Dr T. Font (University of Valencia)09/09/2016, 14:30
-
Dr A. Schmitt (University of Southampton)09/09/2016, 16:30
I will review and explain calculations of bulk and shear
Go to contribution page
viscosity in various phases of dense quark matter, in unpaired quark
matter as well as in color-superconducting phases such as the
color-flavor locked phase. I will discuss and interpret the results,
which are relevant for instance for the r-mode instability in rotating
stars and thus are measurable, at least indirectly,... -
Choose timezone
Your profile timezone: