Scaling relations between numerical simulations and physical systems they represent
arXiv:1111.6865 · doi:10.1111/j.1365-2966.2012.20489.x
Abstract
The dynamical equations describing the evolution of a physical system generally have a freedom in the choice of units, where different choices correspond to different physical systems that are described by the same equations. Since there are three basic physical units, of mass, length and time, there are up to three free parameters in such a rescaling of the units, . In Newtonian hydrodynamics, e.g., there are indeed usually three free parameters, . If, however, the dynamical equations contain a universal dimensional constant, such as the speed of light in vacuum or the gravitational constant , then the requirement that its value remains the same imposes a constraint on the rescaling, which reduces its number of free parameters by one, to . This is the case, for example, in magneto-hydrodynamics (MHD) or special relativistic hydrodynamics, where appears in the dynamical equations and forces the length and time units to scale by the same factor, or in Newtonian gravity where the gravitational constant appears in the equations. More generally, when there are independent (in terms of their units) universal dimensional constants, then the number of free parameters is . When both gravity and relativity are included, there is only one free parameter (, as both and appear in the equations so that ), and the units of mass, length and time must all scale by the same factor. The explicit rescalings for different types of systems are discussed and summarized here. Such rescalings of the units also hold for discrete particles, e.g. in N-body or particle in cell simulations. They are very useful when numerically investigating a large parameter space or when attempting to fit particular experimental results, by significantly reducing the required number of simulations.
6 pages, 2 tables, accepted to MNRAS (expanded discussion of the general context in the introduction)
References in corpus (6)
- Particle acceleration in relativistic collisionless shocks: Fermi process at last?
- The Dynamics and Afterglow Radiation of Gamma-Ray Bursts. I. Constant Density Medium
- Gamma-ray burst afterglow broadband fitting based directly on hydrodynamics simulations
- Deceleration of arbitrarily magnetized GRB ejecta: the complete evolution
- Simulations of GRB Jets in a Stratified External Medium: Dynamics, Afterglow Lightcurves, Jet Breaks and Radio Calorimetry
- Gamma-Ray Burst Dynamics and Afterglow Radiation from Adaptive Mesh Refinement, Special Relativistic Hydrodynamic Simulations
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