# On the observations of rapid forced reconnection in the solar corona

**Authors:** A.K. Srivastava, Sudheer K. Mishra, P. Jel\'inek, Tanmoy Samanta, Hui, Tian, Vaibhav Pant, P. Kayshap, D. Banerjee, J.G. Doyle, B.N. Dwivedi

arXiv: 1901.07971 · 2020-01-08

## TL;DR

This paper presents observational and numerical evidence that external forcing by a moving prominence can induce rapid magnetic reconnection in the solar corona, leading to localized heating and high reconnection rates.

## Contribution

It introduces a novel physical scenario of forced reconnection driven by external plasma inflows, supported by multiwavelength observations and parametric numerical modeling.

## Key findings

- Forced reconnection occurs rapidly at high rates in the solar corona.
- External plasma inflows can initiate reconnection without significant diffusion.
- Reconnection rates increase with external forcing even at lower resistivity.

## Abstract

Using multiwavelength imaging observations from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) on 03 May 2012, we present a novel physical scenario for the formation of a temporary X-point in the solar corona, where plasma dynamics is forced externally by a moving prominence. Natural diffusion was not predominant, however, a prominence driven inflow occurred firstly, forming a thin current sheet and thereafter enabling a forced magnetic reconnection at a considerably high rate. Observations in relation to the numerical model reveal that forced reconnection may rapidly and efficiently occur at higher rates in the solar corona. This physical process may also heat the corona locally even without establishing a significant and self-consistent diffusion region. Using a parametric numerical study, we demonstrate that the implementation of the external driver increases the rate of the reconnection even when the resistivity required for creating normal diffusion region decreases at the X-point. We conjecture that the appropriate external forcing can bring the oppositely directed field lines into the temporarily created diffusion region firstly via the plasma inflows as seen in the observations. The reconnection and related plasma outflows may occur thereafter at considerably larger rates.

## Full text

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## Figures

7 figures with captions in the complete paper: https://tomesphere.com/paper/1901.07971/full.md

## References

53 references — full list in the complete paper: https://tomesphere.com/paper/1901.07971/full.md

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Source: https://tomesphere.com/paper/1901.07971