Prominence instability and CMEs triggered by massive coronal rain in the solar atmosphere

¹ IGAM, Institute of Physics, University of Graz, Universitätsplatz 5, 8010 Graz, Austria
² Ilia State University, Kakutsa Cholokashvili Ave 3/5, 0162 Tbilisi, Georgia
e-mail: zurab.vashalomidze.1@iliauni.edu.ge
³ E.Kharadze Georgian National Astrophysical Observatory, Mount Kanobili, Abastumani, Georgia
⁴ Astronomical Institute, Slovak Academy of Sciences, PO Box 18, 05960 Tatranská Lomnica, Slovak Republic

Received: 24 December 2020
Accepted: 28 September 2021

Abstract

Context. The triggering process for prominence instability and consequent coronal mass ejections (CMEs) is not fully understood. Prominences are maintained by the Lorentz force against the gravity; therefore, reduction of the prominence mass due to the coronal rain may cause the change of the force balance and hence destabilisation of the structures.

Aims. We aim to study the observational evidence of the influence of coronal rain on the stability of prominence and subsequent eruption of CMEs.

Methods. We used the simultaneous observations from the Atmospheric Imaging Assembly (AIA) of Solar Dynamics Observatory (SDO) and Sun Earth Connection Coronal and Heliospheric Investigation (SECHHI) of Solar Terrestrial Relations Observatory (STEREO) spacecrafts from different angles to follow the dynamics of prominence and to study the role of coronal rain in their destabilisation.

Results. Three different prominences observed during the years 2011–2012 were analysed using observations acquired by SDO and STEREO. In all three cases, massive coronal rain from the prominence body led to the destabilisation of prominence and subsequently to the eruption of CMEs. The upward rising of prominences consisted of the slow and fast rise phases. The coronal rain triggered the initial slow rise of prominences, which led to the final instability (the fast rise phase) after 18–28 h in all cases. The estimated mass flux carried by coronal rain blobs showed that the prominences became unstable after 40% of mass loss.

Conclusions. We suggest that the initial slow rise phase was triggered by the mass loss of prominence due to massive coronal rain, while the fast rise phase (the consequent instability of prominences) was caused by the torus instability and/or magnetic reconnection with the overlying coronal field. Therefore, the coronal rain triggered the instability of prominences and consequent CMEs. If this is the case, then the coronal rain can be used to predict the CMEs and hence to improve the space weather predictions.