Observations of Solar Coronal Rain in Null Point Topologies

TL;DR

This study reports the widespread occurrence of coronal rain near null point topologies in the Sun's corona, observed through multiple wavelengths, suggesting commonality and potential mechanisms like thermal nonequilibrium or reconnection.

Contribution

It provides new observational evidence of coronal rain in null point topologies near coronal hole boundaries, highlighting its ubiquity and potential formation mechanisms.

Findings

Coronal rain observed near null points and separatrices.

Coronal rain formation is frequent and detectable in these regions.

Possible mechanisms include thermal nonequilibrium and interchange reconnection.

Abstract

Coronal rain is the well-known phenomenon in which hot plasma high in the Sun's corona undergoes rapid cooling (from > 10^6 K to < 10^4 K), condenses, and falls to the surface. Coronal rain appears frequently in active region coronal loops and is very common in post-flare loops. This Letter presents discovery observations, which show that coronal rain is ubiquitous in the embedded bipole very near a coronal hole boundary. Our observed structures formed when the photospheric decay of active region leading sunspots resulted in a large parasitic polarity embedded in a background unipolar region. We observe coronal rain to appear within the legs of closed loops well under the fan surface, as well as preferentially near separatrices of the resulting coronal topology: the spine lines, null point, and fan surface. We analyze 3 events using SDO Atmospheric Imaging Assembly (AIA) observations in the 304, 171, and 211 {/AA} channels, as well as SDO Helioseismic and Magnetic Imager (HMI) magnetograms. The frequency of rain formation and the ease with which it is observed strongly suggests that this phenomenon is generally present in null-point topologies of this size scale. We argue that these rain events could be explained by the classic process of thermal nonequilibrium or via interchange reconnection at the null; it is also possible that both mechanisms are present. Further studies with higher spatial resolution data and MHD simulations will be required to determine the exact mechanism(s).