Solar transition region supersonic downflows (SDs) are downward falling mass flux toward the sunspots. This unique phenomenon commonly exists above most sunspots. In IRIS spectra, SDs are often observed as strongly redshifted secondary emission peaks with a speed of around 100 km/s, and last for at least several hours. Until now, how these long-lived SDs form, and what mechanisms are responsible for their substantial and stable mass supply still remain unclear since their discovery in the 1980s.

Recently, Dr. Li Leping from the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC) and his co-authors shed new light on these unresolved questions. They proposed that the SDs originate from the cooling and condensation of hot coronal plasma in magnetic dips facilitated by magnetic reconnection.

This new study was published in The Astronomy & Astrophysics on March 15.

Employing joint observations from a ground-based Chinese solar telescope, namely, the New Vacuum Solar Telescope (NVST), and several satellites including SDO, STEREO, and IRIS, the researchers investigated a series of transition region SDs in NOAA AR 12740 and their associated coronal activities. "We clearly track the formation of a quasi-steady SD event for the first time," said Dr. Chen Hechao from Peking University, the first author of the study.

Dual-perspective extreme ultraviolet (EUV) images (see Figures 1 and 2) reveal that these SDs originate from the cooling and condensation of coronal plasma in dips along a large-scale closed loop system that connects the sunspot and a remote region. In the dips, repeated coronal rain forms and continuously flows along these loops towards the sunspot, resulting a TR SD event. "This dual-perspective joint observations from multiple telescopes provide us a very valuable opportunity to directly track the coronal origin of these SDs," said Prof. Tian Hui from Peking University, one corresponding author of the study.

Based on imaging observations and magnetic field extrapolations, the authors proposed a reconnection-facilitated coronal condensation scenario for SD formation (see Figure 2b). In this scenario, the dips form slowly via reconnection between two sets of loops with opposite polarities. The coronal plasma in the dips then quickly cools and condenses via thermal instability. In this process, condensed materials accumulate as a transient prominence in the dips and thus form a mass reservoir available to feed a long-lasting rain flow.

"As the rain persistently drains into the sunspot along different trajectories in funnel-like structures, i.e., sunspot plumes, the funnel effect of this geometry further reshapes the clumpy rain at the coronal height into a more elongated and stream-like one when reaching the lower atmosphere," said Dr. Chen. “This leads to the quasi-steady SDs".

"This work shows a new extended application of our previous reconnection-facilitated coronal condensation scenario that was initially proposed for coronal rain formation", said Dr. Li, the other corresponding author of the study.

The drainage of coronal rain and its resultant SDs last for more than 2 hours (Figures1b and 1d), indicating a substantial mass supply by the coronal condensation. In the dip, the total mass of condensation and condensation rate were calculated. They are indeed large enough to sustain this long-lived SD event. "SDs thus play an important role in the chromosphere-corona mass cycle of the sunspot atmosphere," said Dr. Li.

Figure 1: Sunspot SDs detected during the IRIS Raster scan and their associated coronal rain events. (Credit: Chen Hechao)

Figure 2: A possible scenario for the formation of reconnection-facilitated coronal condensation and its induced quasi-steady SDs from the observations, schematic diagram, and PFSS model. (Credit: Chen Hechao)

The paper can be accessed at https://www.aanda.org/articles/aa/abs/2022/03/aa42093-21/aa42093-21.html