Conveners
18 - Gal. accel. & pulsars: Galactic accelerators
- Marco Tavani (INAF)
18 - Gal. accel. & pulsars: Galactic accelerators
- Marco Tavani (INAF)
18 - Gal. accel. & pulsars: Pulsars
- Marco Tavani (INAF)
18 - Gal. accel. & pulsars: Pulsars
- Marco Tavani (INAF)
Nukri Komin
(Wits University)
12/14/15, 2:00โฏPM
Talk
The Large Magellanic Cloud (LMC) is an irregular satellite galaxy of the Milky Way, which has been observed extensively at Very-High-Energy (VHE) gamma-rays with the H.E.S.S. telescopes, obtaining a deep exposure of 210 hours. In this talk we will present the results of this campaign.
Besides the already known PWN N 157B, these observations establish significant VHE gamma-ray emission from...
Dr
Thierry Stolarczyk
(IRFU/SAp,CEA Saclay, 91190 Gif-sur-Yvette (FR))
12/14/15, 2:20โฏPM
Talk
CTA is the next generation ground based gamma-ray observatory planned to start operations before the end of the decade. With tens of telescopes on sites in both hemispheres, it will allow probing the Milky Way with an unprecedented sensitivity and angular resolution, in the energy domain from a few tens of GeV to a few hundreds of TeV. I will review the CTA Galactic science program ranging...
Dr
Shiu Hang (Herman) Lee
(ISAS/JAXA)
12/14/15, 2:45โฏPM
Talk
Recent observations by the Large Area Telescope (LAT) onboard the Fermi satellite have revealed bright gamma-ray emission from middle-aged supernova remnants (SNRs) inside our Galaxy. These remnants which also possess bright non-thermal radio shells are often found to be interacting directly with surrounding gas clouds. We explore the non-thermal emission mechanism at these dynamically evolved...
Maria Chernyakova
(DCU)
12/14/15, 3:05โฏPM
Talk
Gamma-ray loud binaries are are a recently identified class of X-ray binaries in which interaction of an outflow from the compact object (black hole or neutron star) with the wind and radiation emitted by a companion star leads to the production of very-high energy (VHE) gamma-ray emission. Only five systems have been firmly detected so far as persistent or regularly variable TeV gamma-ray...
Matteo Balbo
(Universitรฉ de Genรจve)
12/14/15, 3:25โฏPM
Talk
The Fermi Large Area Telescope (LAT) observed for the first time ever two consecutive $\eta$Carinae periastron passages. The large field of view of the instrument, its performing sensitivity and homogeneous exposition offers a continuous observation above 100 MeV of the $\eta$Carinae region on the last 7 years. $\eta$Carinae is a binary system hosted in the Carina nebula. Its luminous blue...
Dr
Takayuki Saito
(Kyoto University)
12/14/15, 4:15โฏPM
Talk
Although more than 150 gamma-ray pulsars are known in GeV band, their spectra roll off above 10 GeV and only two pulsars are detected at about 50 GeV, namely Crab and Vela. There is also a large difference between Crab and Vela. Crab spectrum is extending above 1 TeV, while Vela has a very soft spectrum, becoming almost undetectable at 100 GeV.
In order to further understand the emission...
Chandreyee Maitra
(CEA Saclay)
12/14/15, 4:35โฏPM
Talk
PSR J0855-4644 is a nearby, fast spinning, and energetic radio pulsar spatially coincident with the rim of the supernova remnant RX J0852.0-4622 (aka Vela Jr). XMM Newton observations of the pulsar region have shown an arcmin scale extended emission, the pulsar wind nebula (PWN), around the X-ray counterpart of the pulsar. Here, we present results from the small scale structure of the nebula...
Mr
Simone Giacche`
(Max-Planck Institute for Nuclear Physics)
12/14/15, 5:15โฏPM
Talk
The Pulsar Wind Nebulae (PWNe) PSR B1259-63 has been
observed to emit periodic GeV flares, whose power can be
comparable to the total pulsar spin-down luminosity.
Because of the short timescale involved,
these photons are likely to be
produced via inverse Compton scattering of stellar photons or
Synchrotron radiation by a population of very energetic electrons
(from GeV to TeV energies)...
Dr
Krzysztof Nalewajko
(Stanford University)
12/14/15, 5:55โฏPM
Talk
We will present the results of kinetic particle-in-cell numerical simulations of relativistic harmonic magnetic equilibria, so called "ABC fields". These equilibria have been recently shown by relativistic magnetofluid simulations to be generally unstable. An ideal plasma instability leads to the formation of dynamical current layers where magnetic energy is dissipated via reconnection and...
Jรฉrรดme Pรฉtri
(Universitรฉ de Strasbourg)
12/14/15, 6:15โฏPM
Poster
The magnetic field topology in the surrounding of neutron stars is one of the key questions in pulsar magnetospheric physics. A very extensive literature exists about the assumption of a dipolar magnetic field but very little progress has been made in attempts to include multipolar components in a self-consistent way. In this talk, we study the effect of multipolar electromagnetic fields...
Aurรฉlien Sourie
(LUTH - Observatoire de Paris)
12/15/15, 2:00โฏPM
Talk
We present a realistic numerical model for rotating superfluid neutron stars in a full general relativistic framework. Following the work initiated by Prix, Novak & Comer [1], we compute stationary axisymmetric configurations of neutron stars composed of two fluids, namely superfluid neutrons and charged particles (protons and electrons), which are free to rotate around a common axis with...
Brynmor Haskell
(The University of Melbourne)
12/15/15, 2:21โฏPM
Talk
Neutron stars are an exceptional fundamental physics laboratory, and provide us with the only opportunity to study the strong interaction at high densities and low temperatures. These objects are, in fact, not only very dense (with central densities surpassing nuclear saturation density), but also cold, as their thermal energy is generally negligible compared to the Fermi energy of the...
Benoit Cerutti
(Princeton University)
12/15/15, 2:42โฏPM
Talk
Pulsars shine throughout the electromagnetic spectrum, from radio waves to energetic gamma rays. The radio emission is thought to originate from the discharge of the polar-cap and the formation of copious electron-positron pairs. Gamma rays are traditionally associated with particle acceleration in electrostatic gaps within the light cylinder. The recent development of global Particle-In-Cell...
Dr
Jaroslaw Dyks
(Nicolaus Copernicus Astronomical Center)
12/15/15, 3:02โฏPM
Talk
The knowledge of radio emission geometry is crucial
for interpreting their gamma-ray profiles, and for
establishing the orientation of their tilted magnetic field.
I will review the continually increasing evidence against the most popular (nested cone) radio beam geometry.
It will be shown that several features of pulse profiles,
which have normally been considered as signatures of the...
Lucia Pavan
(University of Geneva)
12/15/15, 3:22โฏPM
Talk
Despite jets are detected in all kind of accreting systems, bright and elongated jets are known to be formed also by isolated rotationally powered pulsars.
PSR J1101-6101 in the Lighthouse Nebula is an isolated pulsar which is powering a bright wind nebula and two jets, while travelling at supersonic velocity in the interstellar medium. Extending over 15 pc, the jets are more than 10 times...
Lab Saha
(Nicolaus Copernicus Astronomical Center, Torun, Poland)
12/15/15, 3:42โฏPM
Poster
Average profiles
of some radio pulsars contain
weak emission components which cover large intervals of pulse phase
as well as localised emission or absorption features.
The polarisation-angle (PA) under such features exhibits
local distortions which cannot be explained through the rotating vector model
and other effects such as the special relativistic effects or
modification of...
Norbert Schartel
(ESA)
12/15/15, 4:15โฏPM
Talk
With about 300 refereed papers published each year, XMM-Newton is one of the most
successful scientific missions of ESA ever. Neutron stars are classical targets of X-ray
observatories and consequently huge expectations were accompanying the lunch of
the spacecraft. Contrary to expectations, the spectra of neutron stars were generally
found continuum dominated exclusive any spectral...
Jรฉrรดme Pรฉtri
(Universitรฉ de Strasbourg)
12/15/15, 4:35โฏPM
Talk
Pulsar magnetospheres are shaped by ultra-relativistic electron/positron plasmas flowing in a strong magnetic field and subject to strong gravitational fields. The former induces magnetospheric currents and space charges responsible for the distortion of the electromagnetic field based on pure electrodynamics. The latter induces other perturbations in these fields based on space-time...
Mikhail Belyaev
(UC Berkeley/TAC)
12/15/15, 5:15โฏPM
Talk
We perform 2.5D axisymmetric simulations of the pulsar magnetosphere (aligned dipole rotator) using the charge conservative, relativistic, electromagnetic particle in cell code PICsar. The particle in cell method is a powerful tool for studying the pulsar magnetosphere, because it can handle the force-free and vacuum limits as well as magnetic reconnection. In particular, dissipative regions...
Jรฉrรดme Pรฉtri
(Universitรฉ de Strasbourg)
12/15/15, 5:35โฏPM
Talk
Geodetic precession has been observed directly in the double-pulsar PSR J0737-3039. Its rate has even been measured and agrees with predictions of general relativity. Very recently, the double pulsar has been detected in X-rays and gamma-rays. This fuels the hope observing geodetic precession in its high-energy pulse profile. Unfortunately, the geometric configuration of the binary renders any...
Guillaume Belanger
(ESA)
12/15/15, 5:55โฏPM
Poster
We present here the results of an analysis of 15 years of regular XMM-Newton EPIC pn observations of the Crab pulsar. The analysis of its pulse profile is based on a multi-harmonic decomposition using a new periodogram statistic which is ideally suited for studying the details of the characteristics of peaked pulse profiles such as the Crabโs, especially in time-tagged event data. The...
