EvoL: The new Padova T-SPH parallel code for cosmological simulations - I. Basic code: gravity and hydrodynamics

Abstract

We present EvoL, the new release of the Padova N-body code for cosmological simulations of galaxy formation and evolution. In this paper, the basic Tree + SPH code is presented and analysed, together with an overview on the software architectures. EvoL is a flexible parallel Fortran95 code, specifically designed for simulations of cosmological structure formation on cluster, galactic and sub-galactic scales. EvoL is a fully Lagrangian self-adaptive code, based on the classical Oct-tree and on the Smoothed Particle Hydrodynamics algorithm. It includes special features such as adaptive softening lengths with correcting extra-terms, and modern formulations of SPH and artificial viscosity. It is designed to be run in parallel on multiple CPUs to optimize the performance and save computational time. We describe the code in detail, and present the results of a number of standard hydrodynamical tests.

33 pages, 49 figures, accepted on A&A

References in corpus (6)

• SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
• Modelling discontinuities and Kelvin-Helmholtz instabilities in SPH
• Astrophysical Smooth Particle Hydrodynamics
• MAGMA: a 3D, Lagrangian magnetohydrodynamics code for merger applications
• VINE -- A numerical code for simulating astrophysical systems using particles I: Description of the physics and the numerical methods
• Simulating the formation and evolution of galaxies: Multi-phase description of the interstellar medium, star formation, and energy feedback

Cited by in corpus (23)

• Implementation of feedback in SPH: towards concordance of methods
• Dusty gas with SPH - I. Algorithm and test suite
• Dynamics of stars around spiral arms in an N-body/SPH simulated barred-spiral galaxy
• A Comparison of Cosmological Codes: Properties of Thermal Gas and Shock Waves in Large Scale Structures
• SEREN - A new SPH code for star and planet formation simulations
• The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR
• Tree-based solvers for adaptive mesh refinement code FLASH - I: gravity and optical depths
• Gas and Stellar Motions and Observational Signatures of Co-Rotating Spiral Arms
• Hydrodynamic simulations with the Godunov SPH
• A fast recursive coordinate bisection tree for neighbour search and gravity
• Numerical Simulations of Bubble-Induced Star Formation in Dwarf Irregular Galaxies with a Novel Stellar Feedback Scheme
• On dust entrainment in photoevaporative winds
• Formation and Evolution of Early-Type Galaxies. III Star formation history as a function of mass and over-density
• Towards a self-consistent numerical model of late-type galaxies: Calibrating the effects of sub-grid physics on galactic models
• Hydrodynamic capabilities of an SPH code incorporating an artificial conductivity term with a gravity-based signal velocity
• The entropy core in galaxy clusters: numerical and physical effects in cosmological grid simulations
• ROBO: a Model and a Code for the Study of the Interstellar Medium
• A comparison of SPH artificial viscosities and their impact on the Keplerian disk
• Theory of Stellar Population Synthesis with an application to N-Body simulations
• GalMod: a Galactic synthesis population model
• The Robustness of Cosmological Hydrodynamic Simulation Predictions to Changes in Numerics and Cooling Physics
• The parallelism between galaxy clusters and early-type galaxies: III. The Mass-Radius Relationship
• Modelling galaxy spectra in presence of interstellar dust-III. From nearby galaxies to the distant Universe