Dynamics of Streamers and Pseudostreamers and Implications for the Solar Wind

TL;DR

This study uses a 2.5D magnetohydrodynamic model to analyze the dynamic interactions of streamers and pseudostreamers, revealing continuous plasma release into the heliosphere and implications for solar wind variability.

Contribution

It extends previous models by including self-consistent thermodynamics to simulate the dynamic evolution of streamers and pseudostreamers with plasma release mechanisms.

Findings

Continuous interaction between closed and open flux in streamers and pseudostreamers.

Breathing cycle in helmet streamers causes plasmoid release and density fluctuations.

Pseudostreamers exhibit back-and-forth motion driving interchange reconnection.

Abstract

The origin of the Sun's slow wind and its inherent variability remain unknown, but there is increasing evidence that interactions between closed and open magnetic flux in the corona play a major role. This paper studies the dynamic evolution of streamers and pseudostreamers with a particular focus on the release of plasma from the closed to the open field region. We employ a global 2.5D magnetohydrodynamic model that extends from the solar chromosphere to 30 solar radii, and that extends previous interchange magnetic reconnection modelling by including self-consistent thermodynamics. We find that at both the helmet streamer and pseudostreamer there is a continual dynamic interaction between closed and open flux even in the absence of explicit driving. At the helmet streamer, the dynamics take the form of a ''breathing'' cycle in which the closed flux contracts and expands, and plasmoids are released along the heliospheric current sheet. The pseudostreamer exhibits a back-and-forth motion, driving interchange reconnection alternately on its opposite flanks. The resulting release of hot, dense plasma leads to density fluctuations in the open field that are significantly larger above the helmet streamer due to the persistence of the plasmoids there. Our model demonstrates that plasma is continually being released into the heliosphere from both streamers and pseudostreamers. We discuss the implications of our simulation results for observations of the corona and inner heliosphere.