Statistics of blob properties in two types of coronal streamers

TL;DR

This study statistically compares the properties of coronal streamer blobs in active region streamers and quiet equatorial streamers, revealing differences in occurrence rates, velocities, and accelerations based on streamer type.

Contribution

It provides the first comprehensive statistical analysis of blob properties in two distinct streamer types using a full year's SOHO/LASCO/C2 data.

Findings

Blobs in active region streamers occur twice as often as in quiet streamers.

Active region streamer blobs have higher initial velocities and accelerations.

Coronal activity influences the dynamics and structure of solar wind originating from streamers.

Abstract

Previous studies have shown that a streamer blob might originate in the lower corona and thus be affected by activity in that region. While the base of one streamer might differ from that of another, it can be cataloged into two distinct types: active region streamers (ARSs) that have active regions at their base, and quiet equatorial streamers (QESs) that do not have an active region underneath.The difference between the blob properties in ARSs and those in QESs remains unknown. By analyzing the whole-year observations from SOHO/LASCO/C2 in 2018, we carried out a statistical analysis of the properties of propagating blobs in ARSs and QESs. We found that the properties of streamer blobs are very different from one blob to another. The occurrence rate of blobs in ARSs is about twice as high as that in QESs. On average, the ARS blobs have significantly higher initial velocities and slightly higher accelerations, but slightly lower heights of first appearance than the QES blobs. There is a weak positive correlation between the initial velocities and heights of first appearance in the two groups of streamer blobs. The correlation between the accelerations and heights of first appearance in ARS blobs is negative, while that in QES blobs is positive. Our results provide statistical evidence that a higher degree of activity at the coronal base of a streamer can cause more dynamic blobs higher up, and that it affects the structures of the solar wind originating in the region.