Generation of quasi-periodic waves and flows in the solar atmosphere by oscillatory reconnection

TL;DR

This paper demonstrates that oscillatory reconnection in the solar atmosphere can generate quasi-periodic, high-speed outflows and jets, providing a physical explanation for observed solar phenomena.

Contribution

The study introduces 2.5D nonlinear simulations showing oscillatory reconnection as a mechanism for solar outflows, expanding understanding of solar jet dynamics.

Findings

Oscillatory reconnection produces quasi-periodic vertical outflows.

Outflow speeds range from 20 to 60 km/s, matching observations.

Periodicities vary from 1.75 to 3.5 minutes depending on magnetic strength.

Abstract

We investigate the long-term evolution of an initially buoyant magnetic flux tube emerging into a gravitationally-stratified coronal hole environment and report on the resulting oscillations and outflows. We perform 2.5D nonlinear numerical simulations, generalizing the models of McLaughlin et al. (2009) and Murray et al. (2009). We find that the physical mechanism of oscillatory reconnection naturally generates quasi-periodic vertical outflows, with a transverse/swaying aspect. The vertical outflows consist of both a periodic aspect and evidence of a positively-directed flow. The speed of the vertical outflow (20-60 km/s) is comparable to those reported in the observational literature. We also perform a parametric study varying the magnetic strength of the buoyant flux tube and find a range of associated periodicities: 1.75-3.5 min. Thus, the mechanism of oscillatory reconnection may provide a physical explanation to some of the high-speed, quasi-periodic, transverse outflows/jets recently reported by a multitude of authors and instruments.