Mr
Giovanni Camelio
(University of Rome "Sapienza", Physics Department)
15/06/2015, 14:00
I have written a new code for the early evolution of a newly born neutron
star (which is called proto-neutron star, PNS). At each step of the quasi-stationary PNS evolution, the code integrates the Tolman-Oppenheimer-Volkoff equations and then evolves the thermodynamical profiles solving the
energy integrated neutrino diffusion equations. My final aim is to study
the frequencies at which a...
Mr
Mateusz Wisniewicz
(Kepler Institute of Astronomy)
15/06/2015, 14:25
We present numerical calculations of orbital and epicyclic frequencies of nearly circular orbits around rotating neutron stars and strange quark stars. The FPS equation of state was used to describe the structure of neutron stars while the MIT bag model was used to model the equation of state of strange quark stars. All the uniformly rotating stellar configurations were computed in full...
Dr
Julian Leszek Zdunik
(Nicolaus Copernicus Astronomical Center)
15/06/2015, 14:50
Deep crustal heating phenomenon plays important role in explaining some thermal properties
of accreting neutron stars. In soft X-ray transients (SXT) it is used to explain the
relatively high luminosity of neutron star during quiescence,
and in some transient X-ray sources to study the thermal relaxation from accreting
to quiescent state.
To determine the properties of a crust of...
Dr
Jorge Horvath
(IAG-USP)
15/06/2015, 15:15
We calculate the evolution of close binary systems (CBSs) formed by a neutron star (behaving as a radio pulsar) and a normal donor star, evolving either to a helium white dwarf (WD) or ultra short orbital period systems. Some of these systems are expected to evolve into so-called redback and black widow systems. The evolutionary tracks considered X-ray irradiation feedback and evaporation...
Dr
Peter Shternin
(Ioffe Institute)
15/06/2015, 15:40
We calculate the rate of neutrino emission due to modified Urca processes in a nucleon core of a neutron star taking into account in-medium effects on the nuclear interaction. The nuclear interaction is described via the in-medium G-matrix calculated in the Brueckner-Hartree-Fock framework with the continuous choice of the single particle potential. The full Argonne v18 potential with...
Dr
Armen Sedrakian
(Institute for Theoretical Physics, Goethe University, Frankfurt am Main)
15/06/2015, 16:35
I will describe the microphysics, phenomenology, and astrophysical implication of a B-field induced unpairing effect that may occur in magnetars, if the local B-field in the core of a magnetar exceeds a critical value Hc2. The focus will be on modification in the neutrino emissivities of neutron stars as well as their superfluid dynamics.
Albino Perego
(TU-Darmstadt)
15/06/2015, 17:00
Binary neutron star mergers are among the most extreme events happening in the Universe.
These powerful events are expected to release large amounts of energy in form of neutrinos,
gravitational waves and electromagnetic radiation, together with the ejection of a small
fraction of their original mass.
In particular, they are expected to be sites for r-process nucleosynthesis, as well as...
Mr
Marcin Kucaba
(Institute of Astronomy, University of Zielona Gรณra)
15/06/2015, 17:25
Rotating neutron stars are likely sources of gravitational radiation for Advanced Virgo and Ligo detectors. We calculated the gravitational waves background produced by the neutron stars in the Milky Way. To determine the signal we adopt a realistic model of the population of neutron stars taking into account the evolution of the rotation period and the magnetic field of each star. The...
Mr
Dรกniel Barta
(Wigner Research Centre for Physics)
15/06/2015, 17:50
A large number of predicted waveform templates are used by data analysis of targeted search techniques for merging binary black hole sources based upon matched filtering. Waveforms for inspirals are parametrized by a set of intrinsic physical quantities result an eight-dimensional parameter space. The high dimensionality makes gravitational wave searches, parameter estimation, and modeling...
Dr
Ian Jones
(University of Southampton)
16/06/2015, 14:00
Recent X-ray observations have revealed the existence of oscillations during the X-ray bursts of two accreting neutron stars. One possible explanation is that these represent r-mode oscillations. In this talk I explore the r-mode hypothesis, showing that it allows us to place a constraint on the relationship between mass and radius for these two stars. I also discuss what the observations...
Prof.
Dorota Rosinska
(Institute of Astronomy, University of Zielona Gora)
16/06/2015, 14:25
An understanding of differentially rotating relativistic stars is key
to many areas of astrophysics, in particular to the emission of
gravitational waves. A newly born, proto-neutron star or a compact
remnant of neutron stars binary merger are expected to rotate
differentially and to be important sources of gravitational
radiation. A highly accurate, multidomain spectral code is used...
Dr
Gergely Debreczeni
(Wigner RCP)
16/06/2015, 14:50
Modern gravitational wave (GW) detectors are hunting for GWs originating from various sources among other from binary neutron star (BNS) coalescence. It is assumed that in some cases it is the coalescence (merging) of such BNS system which is responsible for the creation of gamma-ray bursts (GRBs) - routinely detected by electromagnetic observatories. Since already well before their merging,...
Ms
Magdalena Szkudlarek
(Kepler Institute of Astronomy University of Zielona Gora)
16/06/2015, 15:15
Strange quark stars are considered as a possible alternative to neutron stars as compact objects. We present first fully relativistic calculations of differentially rotating strange quark stars for broad ranges of stellar masses and the degree of differential rotation. A newly born, hot neutron star (or a strange star) formed in a supernova explosion is supposed to rotate differentially....
Dr
Leonardo Gualtieri
(Dipartimento di Fisica, "Sapienza" Universitร di Roma)
16/06/2015, 15:40
Tidal Love numbers carry valuable information on the inner structure of a neutron star, and on its equation of state. This information could be extracted, by IInd and IIIrd generation gravitational wave detectors, from the gravitational wave signal emitted by coalescing neutron star-neutron star binaries. Up to now, the theoretical modelling and computation of Love numbers has been limited to...
Dr
Kostas Glampedakis
(University of Murcia)
16/06/2015, 16:35
In this talk we discuss a parametrised formalism for describing relativistic stars beyond General Relativity, without committing to any particular modified theory of gravity.
We show how the deviations from GR are reflected on the stellar mass-radius and demonstrate the equivalence between this "post-TOV" formalism and an effective GR description.
Dr
Plamen Fiziev
(Sofia University Foundation for Theoretical Physics and Astrophysics)
16/06/2015, 17:00
The well-known serious difficulties in numerical investigation of realistic models of neutron stars (NS) in the modified theories of gravity [1] are surmounted on a general basis. Developing the recent results of the author [2-4] we present a realistic model of static spherically symmetric NS with AMP1 EOS using the correct boundary conditions at the center, at the edge, and at the...
Ms
Szilvia Karsai
(Eรถtvรถs University Budapest)
16/06/2015, 17:25
Theoretical descriptions of compact stars have been extensively studied long time ago. The description of these extreme objects of the Universe are required to handle both the high-energy particle/nuclear physics and the gravitational theory in parallel. A possible theoretical phenomena based on the Kaluza โKlein geometrization of interactions also provides a simply model for the compact...
Mr
Antonio Graziano Pili
(Universitร degli Studi di Firenze)
18/06/2015, 14:00
The morphology of the strong magnetic fields hosted by neutron stars plays a key role in establishing and governing the physics and the observational properties of these extreme astrophysical objects. Hence an accurate description of magnetic fields in neutron stars provides a necessary ingredient to develop realistic physical models able to shed light on the phenomenology of these compact...
Ms
Vanessa Graber
(University of Southampton)
18/06/2015, 14:25
The presence of superconducting and superfluid components in the core of mature neutron stars calls for the rethinking of a number of key magnetohydrodynamical notions like resistivity, the induction equation, magnetic energy and flux-freezing. Using a multi-fluid magnetohydrodynamics formalism, we investigate how the magnetic field evolution is modified when neutron star matter is composed of...
Dr
Michael Gabler
(MPA Garching)
18/06/2015, 14:50
Our numerical simulations show that axisymmetric, torsional, magnetoelastic oscillations of magnetars with a superfluid core can explain the whole range of observed quasiperiodic oscillations (QPOs) in the giant flares of soft gamma-ray repeaters. There exist constant phase QPOs at fโฒ150Hz and resonantly excited high-frequency QPOs (f>500Hz), in good agreement with observations. The range of...
Bruno Giacomazzo
(University of Trento)
18/06/2015, 16:10
I will present results of recent investigations about the possibility to form long-lived or even stable magnetars after the merger of a binary neutron star (BNS) system. BNSs are among the most powerful sources of gravitational waves (GWs) that will be detected by advanced LIGO and Virgo. While the inspiral GW signal is the main target for the first detections, the formation of a long-lived or...
Dr
Justin Elfritz
(Anton Pannekoek Institute, University of Amsterdam)
18/06/2015, 16:35
State-of-the-art 2D simulations of coupled magnetic and temperature evolution have shown us that we can explain different neutron star (NS) classes by varying only magnetic field strength and geometry at birth. In this work we address evolutionary differences that arise as a consequence of including the physics driving magnetic field evolution in the NS core. Forcing in the core arises due to...
Mr
Onur Akbal
(Sabanci University)
18/06/2015, 17:00
Standard glitches are characterized by a positive step in angular velocity and a negative step in the spin-down rate of the pulsar. There are no glitch-associated changes in the electromagnetic signature of rotation- powered pulsars in all cases so far. For the first time, in the last glitch of PSR J1119- 6127, there is clear evidence for changing emission properties coincident with the...
