Description
CHAIR: D. BUSONERO
Imaging Air Cherenkov Telescopes (IACTs) play a crucial role in the field of ultra-high energy astrophysics (E > 10GeV), bringing a fundamental contribution to the study of cosmic gamma-ray sources. As the sensitivity and complexity of IACT systems increase, so does the demand for efficient data reduction techniques and computational resources to handle the ever-growing data volumes. This...
Pulsar Wind Nebulae are powered by the relativistic, magnetized and cold wind emanating from a rapidly rotating neutron star (the pulsar) that interacts with the ambient medium. They are visible as bright non-thermal sources at a very broad range of energies, from radio to gamma-rays, with a variety of different morphologies.
Pulsar Wind Nebulae are perfect places where to look at for...
I will introduce the DEMNUni simulation set, which accounts for different cosmologies with massive neutrinos and dynamical dark-energy. I will briefly present the scientific results obtained up to now. Then, I will focus on the computational resources (both ISCRA and MoU CINECA-INAF) needed to produce the DEMNUni suite, as well as the long-term storage required to support and mantain the...
We hereby present the computational requirements of the infrastructure needed by the Monitoring System (MON) of the Cherenkov Telescope Array (CTA) in two different scenarios: the performance tests and the on-site deployment. The CTA will be composed of hundreds of telescopes working together to attempt to unveil some fundamental physics of the high-energy Universe. Along with the scientific...
The solar corona shows inexplicably high temperatures, up to million degrees, when compared with the cold lower photosphere. The conversion of magnetic energy into thermal one through the magnetic reconnection has been chased for the last decades as the mechanism to explain this phenomenon. The reason why such mechanism remains elusive is because reconnection events are singularly too small...
The solar corona consists of plasma confined by, and interacting with, the coronal magnetic field. The magnetic processes are highly dynamic and non linear, and their description requires time-dependent magnetohydrodynamic modelling on high performance computing systems.
Large-scale energy release in the corona may involve MHD instabilities such as the kink instability in a single twisted...
Pulsar Wind Nebulae (PWNe) constitute a magnificent lab to investigate high-energy astrophysics in its many facets, from non-thermal emission, to particle acceleration, from relativistic fluid dynamics to anti-matter creation. The group in Arcetri has always been one of the leading team in the study of PWNe, and through the years has developed a vast and advanced suits of numerical tools for...
In numerical experiments of the propagation of relativistic jets produced e.g. by Supermassive Black Holes (SMBH) the covariant equation of state determines a relationship between density, pressure and temperature. While the former is proportional to the Lorentz factor and the second is invariant, one is left with different possibilities concerning temperature. The usual choice adopted in...
Core-collapse supernova remnants (SNRs) exhibit intricate morphologies and a highly non-uniform distribution of stellar debris. In the case of young remnants (less than 5000 years old), their characteristics offer insights into the inner processes of the supernova (SN) engine, including nucleosynthetic yields and large-scale asymmetries originating from the early stages of the explosion....
Magnetic fields manifest themselves almost everywhere in the Universe. Their effects are visible through different kinds of electromagnetic radiation and in the spectra of cosmic rays. In our talk, we focus on the magnetic field in supernova remnants. We show how high-performance computing allows us to investigate the evolution of magnetic field in the remnants of different types of supernova...
