A Recipe to Probe Alternative Theories of Gravitation via N-body Numerical Simulations. I. Spiral Galaxies
arXiv:1204.5366 · doi:10.1088/0004-637X/750/1/29
Abstract
A way to probe alternative theories of gravitation is to study if they could account for the structures of the universe. We then modified the well-known Gadget-2 code to probe alternative theories of gravitation through galactic dynamics. As an application, we simulate the evolution of spiral galaxies to probe alternative theories of gravitation whose weak field limits have a Yukawa-like gravitational potential. These simulations show that galactic dynamics can be used to constrain the parameters associated with alternative theories of gravitation. It is worth stressing that the recipe given in the present study can be applied to any other alternative theory of gravitation in which the superposition principle is valid.
arXiv comment34 pages, 18 figures
References in corpus (17)
- Measurements of Omega and Lambda from 42 High-Redshift Supernovae
- A Universal Density Profile from Hierarchical Clustering
- The Structure of Cold Dark Matter Halos
- The cosmological simulation code GADGET-2
- Modeling feedback from stars and black holes in galaxy mergers
- Forming Realistic Late-Type Spirals in a LCDM Universe: The Eris Simulation
- The central slope of dark matter cores in dwarf galaxies: Simulations vs. THINGS
- Tidal tails in CDM cosmologies
- On the origin of rR_1 ring structures in barred galaxies
- Star formation in isolated AMIGA galaxies: dynamical influence of bars
- Galaxy Dynamics Predictions in the Nonsymmetric Gravitational Theory
- Galaxy Dynamics Predictions in the Nonsymmetric Gravitational Theory
- Model for Gravitational Interaction between Dark Matter and Baryons
- A solution for galactic disks with Yukawian gravitational potential
- Potential-density pairs for axisymmetric galaxies: the influence of scalar fields
- Probing Yukawian gravitational potential by numerical simulations. I. Changing N-body codes
- Probing Yukawian Gravitational Potential by Numerical Simulations. II. Elliptical Galaxies