Linear analysis of the gravitational beam-plasma instability
arXiv:2203.16990 · doi:10.1140/epjc/s10052-023-11647-z
Abstract
We investigate the well-known phenomenon of the beam-plasma instability in the gravitational sector, when a fast population of particles interacts with the massive scalar mode of an Horndeski theory of gravity, resulting into the linear growth of the latter amplitude. Following the approach used in the standard electromagnetic case, we start from the dielectric representation of the gravitational plasma, as introduced in a previous analysis of the Landau damping for the scalar Horndeski mode. Then, we set up the modified Vlasov-Einstein equation, using at first a Dirac delta function to describe the fast beam distribution. This way, we provide an analytical expression for the dispersion relation and we demonstrate the existence of non-zero growth rate for the linear evolution of the Horndeski scalar mode. A numerical investigation is then performed with a trapezoidal beam distribution function, which confirms the analytical results and allows to demonstrate how the growth rate decreases as the beam spread increases.
Revised version, two sections added + minor changes
References in corpus (11)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Gravitational Waves and Gamma-rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A
- Covariant Galileon
- Dark Energy after GW170817: dead ends and the road ahead
- Strong constraints on cosmological gravity from GW170817 and GRB 170817A
- Evidence for dark matter in the inner Milky Way
- Dark matter spikes in the vicinity of Kerr black holes
- New Graviton Mass Bound from Binary Pulsars
- Landau damping for gravitational waves in parity-violating theories
- Contributions to the linear and non-linear theory of the beam-plasma interaction
- Stability Conditions for the Horndeski Scalar Field Gravity Model