Vertical flows and structures excited by magnetic activity in the Galactic center region

TL;DR

This study uses MHD simulations to reveal complex vertical, azimuthal, and radial flows driven by magnetic activity in the galactic center, explaining observed high velocity dispersions.

Contribution

It provides new insights into the magnetic loop-driven flow structures and their role in galactic center dynamics, based on detailed simulation analysis.

Findings

Fast downflows of ~100 km/s along magnetic loops

Flow directions are altered by magnetic loop geometry

Vertical, azimuthal, and radial motions are excited

Abstract

The vertical flow structure in the galactic center region remains poorly understood. We analyzed the MHD simulation data by Suzuki et al. (2015) for better understanding. As a result, we found the fast downflows with a speed of ~100 km/s near the foot-points of magnetic loops. These downflows are flowing along a magnetic field line and accelerated by the gravity. The direction of the fast flows is changed by the magnetic loop geometry, as it moves. As a result, not only vertical motions but also azimuthal and radial motions are excited. This feature could be relevant to the observed high velocity dispersion in the position-velocity diagram.