A Simple Measurement of Turbulence in Cores of Galaxy Clusters
arXiv:astro-ph/0508249 · doi:10.1086/496972
Abstract
Using a simple model, we study the effects of turbulence on the motion of bubbles produced by AGN jet activities in the core of a galaxy cluster. We focus on the turbulence with scales larger then the size of the bubbles. We show that for a bubble pair with an age of ~10^8 yr, the projected angle between the two vectors from the cluster center to the two bubbles should be ~> 90 degree and the ratio of their projected distances from the cluster center should be ~< 2.5, if the velocity and scale of the turbulence are ~250 km s^-1 and ~20 kpc, respectively. The positions of the bubbles observed in the Perseus cluster suggest that the turbulent velocity is ~>100 km s^-1 for the cluster.
Accepted for publication in ApJL
References in corpus (5)
- Probing Turbulence in the Coma Galaxy Cluster
- Impact of stochastic gas motions on galaxy cluster abundance profiles
- A deep Chandra observation of the Centaurus cluster: bubbles, filaments and edges
- Strong Turbulence in the Cool Cores of Galaxy Clusters: Can Tsunamis Solve the Cooling Flow Problem?
- Simulating Astro-E2 Observations of Galaxy Clusters: the Case of Turbulent Cores Affected by Tsunamis
Cited by in corpus (7)
- Turbulence, magnetic fields and plasma physics in clusters of galaxies
- Simulating the interaction of jets with the intra-cluster medium
- Inefficient Driving of Bulk Turbulence by Active Galactic Nuclei in a Hydrodynamic Model of the Intracluster Medium
- Pressure-anisotropy-driven microturbulence and magnetic-field evolution in shearing, collisionless plasma
- The impact of numerical viscosity in SPH simulations of galaxy clusters
- The role of the artificial conductivity in SPH simulations of galaxy clusters: effects on the ICM properties
- Fast growth of magnetic fields in galaxy clusters: a self-accelerating dynamo