Simultaneous existence of the ocsillations, counterstreaming flows and mass injections in solar quiescent prominences

TL;DR

This study uses high-resolution solar observations to analyze the coexistence of oscillations, counterstreaming flows, and mass injections in quiescent prominences, revealing their dynamic interactions and characteristics.

Contribution

It provides detailed observational evidence of multiple dynamic phenomena co-occurring in solar prominences, enhancing understanding of their complex behavior.

Findings

Identified a 83-minute longitudinal oscillation in prominence plasma.

Observed counterstreaming flows with velocities from 4 to 11 km/s.

Detected intermittent mass injections with velocities from 3 to 30 km/s.

Abstract

Solar prominences are very spectacular structures embedded in the tenuous and hot solar corona. The counterstreaming flows, a common feature in solar quiescent prominences, have been discovered for more than twenty years. However, the mechanism driving the counterstreaming flows is still elusive. To unveil the nature of this phenomenon, we analyzed the data of a quiescent prominence observed by the New Vacuum Solar Telescope (NVST), the Interface Region Imaging Spectrograph (IRIS), and the Solar Dynamical Observatory (SDO). It is found that there is a distinct longitudinal oscillation of prominence plasma along the higher part of the prominence spine in H$\alpha$ observations. The oscillation period is approximately 83 minutes and the amplitude is about 32 Mm. The counterstreaming flows are dominant in the middle part of the prominence spine. The velocities of the counterstreaming flows range from about 4 km s$^{-1}$ to 11 km s$^{-1}$. Moreover, the intermittent mass flows with the upward plumes from the top of the bubbles and tornado-like barbs are observed to be injected into the lower part of the prominence spine from the lower atmosphere. The velocities of these injected mass flows range from about 3 km s$^{-1}$ to 30 km s$^{-1}$. Some injected mass flows exhibit redshifted Doppler signals, while others exhibit blueshifted signals. Based on these high resolution observations, it is found that different parts of the prominence spine exhibit the different dynamic characteristics. These results further advance the understanding of the ubiquitous counterstreaming flows in solar quiescent prominences.