- 1LIRA Observatoire de Paris, Meudon, France (brigitte.schmieder@obspm.fr)
- 2Nanjing University, Nanjing, China (jinhan.Guo@kuleuven.be)
- 3ROCS, University of Oslo, Oslo, Norway (reetikajoshi.ntl@gmail.com)
- 4Institute of Theoretical Astrophysics, University of Oslo, Oslo, Norway (reetika.joshi@astro.uio.no)
- 5Astronomical Institute Czech Academy of Sciences, Ondrejov, Czech Republic ( jaroslav.dudik@asu.cas.cz)
- 6CmPA, KU Leuven, Leuven, Belgium (stefaan.poedts@kuleuven.be)
- 7University of Lublin, Lublin, Poland
In standard 2D eruption models, the eruption of a magnetic flux rope is associated with magnetic reconnection occurring beneath it. However, in a 3D context, additional reconnection possibilities arise, particularly involving interactions between the flux rope and the overlying arcades. This process results in the drifting of the legs of the erupting flux rope.
We show examples of such magnetic reconnections between erupting filaments interacting with coronal arcades, called ar-rf (arcade + rope – rope + flare loop), using AIA/SDO and IRIS data.
To understand the physical processes behind observations, we perform data-inspired MHD numerical simulations, which reproduce such magnetic reconnection between flux rope and overlying magnetic fields. Our model clearly exhibits the slippage of flux-rope field lines and the remote heating and flare ribbons due to such external reconnection.
How to cite: Schmieder, B., Guo, J., Joshi, R., Dudik, J., and Poedts, S.: 3D Magnetic reconnection in solar eruptions: observations and MHD numerical simulations, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-1796, https://doi.org/10.5194/egusphere-egu25-1796, 2025.
