Annual NewCompStar Conference 2016

Session

Evening session

25 Apr 2016, 16:00

Bogazici University-Rectorate Building (Istanbul)

47. The extraordinary 2011 outburst of the magnetar Swift J1822.3-1606 Magnetar Model for GRBs

Manoneeta Chakraborty (Tata Institute of Fundamental Research)

25/04/2016, 16:00

Magnetars are highly magnetized neutron star and energetic X-ray/ soft gamma ray bursts are often observed from these sources. The most energetic of these bursts,- the giant flares have been observed only from a few sources and exhibit distinct observational characteristics. The 2011 outburst of the relatively low magnetic field magnetar was quite extraordinary because of the unusual timing...

62. Interaction modes of magnetic compact stars with gaseous environment near a supermassive black hole

Dr Vladimir Karas (Astronomical Institute, Czech Academy of Sciences)

25/04/2016, 16:20

standard talk

We examine the role of a dipole-type magnetic field of a compact (neutron) star for its interaction with the ambient interstellar medium, and the resulting drag as the star orbits near a supermassive black hole. The enhancement of the orbital decay is found to be very small in the Galactic centre (the mini-spiral region of Sgr A*), where the environment density is very low, but it becomes...

21. Propeller effect in X-ray pulsars

Dr Sergey Tsygankov

26/04/2016, 16:20

Propeller effect in X-ray pulsars Propeller effect, i.e. centrifugal inhibition of accretion, is an immediate evidence of the presence of a strong dipole magnetic field in accreting neutron stars. Observation of this effect requires high sensitivity of X-ray telescopes and become possible only recently. From the theoretical point of view many aspects of this effect (spectrum formation, matter...

22. On the maximum accretion luminosity of magnetized neutron stars: connecting X-ray pulsars and ultraluminous X-ray sources

Dr Alexander Mushtukov

26/04/2016, 16:40

We study properties of luminous X-ray pulsars using a simplified model of the accretion column based on diffusion approach. The maximal possible luminosity is calculated as a function of the neutron star (NS) magnetic field strength and spin period. It is shown that the luminosity can reach values of the order of 10^{40} erg/s for the magnetar-like magnetic field (B > 10^{14}G) and long spin...

37. Maximum mass, moment of inertia and compactness of relativistic stars

Ms Cosima BREU

28/04/2016, 16:20

A number of recent works have highlighted that it is possible to express the properties of general-relativistic stellar equilibrium configurations in terms of functions that do not depend on the specific equation of state employed to describe matter at nuclear densities. These functions are normally referred to as "universal relations" and have been found to apply, within limits, both to...

38. Artificial entropy viscosity in numerical relativistic hydrodynamics

Mr Federico Guercilena

28/04/2016, 16:40

Artificial entropy viscosity in numerical relativistic hydrodynamics Large scale numerical simulations are one of the most useful tools to shed light on the physics of neutron stars, but due to their high computational cost and great accuracy requirements the research for better numerical methods is constantly ongoing. We present a new fast and accurate numerical scheme called artificial...