The PLUTO code for adaptive mesh computations in astrophysical fluid dynamics
A Mignone, C Zanni, P Tzeferacos… - The Astrophysical …, 2011 - iopscience.iop.org
We present a description of the adaptive mesh refinement (AMR) implementation of the
PLUTO code for solving the equations of classical and special relativistic …
PLUTO code for solving the equations of classical and special relativistic …
MPI-AMRVAC for solar and astrophysics
O Porth, C Xia, T Hendrix, SP Moschou… - The Astrophysical …, 2014 - iopscience.iop.org
In this paper, we present an update to the open source MPI-AMRVAC simulation toolkit
where we focus on solar and non-relativistic astrophysical magnetofluid dynamics. We …
where we focus on solar and non-relativistic astrophysical magnetofluid dynamics. We …
Beyond second-order convergence in simulations of magnetized binary neutron stars with realistic microphysics
We investigate the impact of using high-order numerical methods to study the merger of
magnetized neutron stars with finite-temperature microphysics and neutrino cooling in full …
magnetized neutron stars with finite-temperature microphysics and neutrino cooling in full …
Gravitational waveforms from binary neutron star mergers with high-order weighted-essentially-nonoscillatory schemes in numerical relativity
S Bernuzzi, T Dietrich - Physical Review D, 2016 - APS
The theoretical modeling of gravitational waveforms from binary neutron star mergers
requires precise numerical relativity simulations. Assessing convergence of the numerical …
requires precise numerical relativity simulations. Assessing convergence of the numerical …
Three-dimensional solar wind modeling from the Sun to Earth by a SIP-CESE MHD model with a six-component grid
X Feng, L Yang, C Xiang, ST Wu, Y Zhou… - The Astrophysical …, 2010 - iopscience.iop.org
The objective of this paper is to explore the application of a six-component overset grid to
solar wind simulation with a three-dimensional (3D) Solar-InterPlanetary Conservation …
solar wind simulation with a three-dimensional (3D) Solar-InterPlanetary Conservation …
GRHydro: a new open-source general-relativistic magnetohydrodynamics code for the Einstein toolkit
We present the new general-relativistic magnetohydrodynamics (GRMHD) capabilities of the
Einstein toolkit, an open-source community-driven numerical relativity and computational …
Einstein toolkit, an open-source community-driven numerical relativity and computational …
The fully developed remnant of a neutrino-driven supernova-Evolution of ejecta structure and asymmetries in SNR Cassiopeia A
S Orlando, A Wongwathanarat, HT Janka… - Astronomy & …, 2021 - aanda.org
Context. The remnants of core-collapse supernovae (SNe) are probes of the physical
processes associated with their parent SNe. Aims. Here we aim to explore to which extent …
processes associated with their parent SNe. Aims. Here we aim to explore to which extent …
THC: a new high-order finite-difference high-resolution shock-capturing code for special-relativistic hydrodynamics
D Radice, L Rezzolla - Astronomy & Astrophysics, 2012 - aanda.org
We present THC: a new high-order flux-vector-splitting code for Newtonian and special-
relativistic hydrodynamics designed for direct numerical simulations of turbulent flows. Our …
relativistic hydrodynamics designed for direct numerical simulations of turbulent flows. Our …
High-order conservative reconstruction schemes for finite volume methods in cylindrical and spherical coordinates
A Mignone - Journal of Computational Physics, 2014 - Elsevier
High-order reconstruction schemes for the solution of hyperbolic conservation laws in
orthogonal curvilinear coordinates are revised in the finite volume approach. The …
orthogonal curvilinear coordinates are revised in the finite volume approach. The …
On the amplification of magnetic fields in cosmic filaments and galaxy clusters
The amplification of primordial magnetic fields via a small-scale turbulent dynamo during
structure formation might be able to explain the observed magnetic fields in galaxy clusters …
structure formation might be able to explain the observed magnetic fields in galaxy clusters …