MHD Modelling of magnetic reconnection heating and jets in the solar corona
Abstract
Magnetic reconnection is seen as the lead mechanism to explain the persistent and bursty heating of the solar corona that keeps its thermal structure. Lately the observations and modelling of magnetic reconnection outflows, i.e. nanojets, has empowered our capabilities to scrutinise this mechanisms, however more needs to be understood on the relation between the energetic and kinematic events. The aim of this paper is to study in details the properties of the heating events (nanoflare) and the kinematic counterparts (nanojets) in order to augment detection capabilities of magnetic reconnection events. We use MHD simulations of the interaction of two magnetic flux tubes where magnetic reconnection occurs and such reconnection outflows are generated. We vary key parameters, such as the critical current and the size of the domain to study the heating and slingshot mechanisms. We find that the properties of the nanojets can give away much information on the magnetic reconnection that generated it, while it is difficult to directly link the amount of heating and the jet speeds. We also find that such reconnection model can explain a wide range of heating events. Magnetic reconnection still is invariably linked to both heating and outflows and our simulations show the complex interplay between these two byproducts of the magnetic reconnection and how their properties can be studied in observations.
Related
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- Magnetic Reconnection Heating of Thin Accretion Disks around Kerr Black Holes
- Understanding how Coronal Heating and Magnetic Field Scaling Affect Global Properties of the Low and Middle Corona
- Current Sheets and Magnetic Reconnection statistics by Solar Orbiter at few to tens of Ion Inertial Lengths II: Conditions for Reconnection, and Current Sheet Planarity
- Magnetic Reconnection Governs the Entire Lifecycle of Solar Eruptive Magnetic Flux Rope
BibTeX
@misc{pagano2026modelling,
title = {{MHD Modelling of magnetic reconnection heating and jets in the solar corona}},
author = {P. Pagano and C. Argiroffi and F. Reale and A. Petralia and G. Cozzo and P. Testa},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.10205},
eprint = {2609.10205},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.10205},
}
RIS
TY - UNPB
TI - MHD Modelling of magnetic reconnection heating and jets in the solar corona
AU - P. Pagano
AU - C. Argiroffi
AU - F. Reale
AU - A. Petralia
AU - G. Cozzo
AU - P. Testa
PY - 2026
DA - 2026/09/09
PB - arXiv
DO - 10.48550/arxiv.2609.10205
UR - https://arxiv.org/abs/2609.10205
AB - Magnetic reconnection is seen as the lead mechanism to explain the persistent and bursty heating of the solar corona that keeps its thermal structure. Lately the observations and modelling of magnetic reconnection outflows, i.e. nanojets, has empowered our capabilities to scrutinise this mechanisms, however more needs to be understood on the relation between the energetic and kinematic events. The aim of this paper is to study in details the properties of the heating events (nanoflare) and the kinematic counterparts (nanojets) in order to augment detection capabilities of magnetic reconnection events. We use MHD simulations of the interaction of two magnetic flux tubes where magnetic reconnection occurs and such reconnection outflows are generated. We vary key parameters, such as the critical current and the size of the domain to study the heating and slingshot mechanisms. We find that the properties of the nanojets can give away much information on the magnetic reconnection that generated it, while it is difficult to directly link the amount of heating and the jet speeds. We also find that such reconnection model can explain a wide range of heating events. Magnetic reconnection still is invariably linked to both heating and outflows and our simulations show the complex interplay between these two byproducts of the magnetic reconnection and how their properties can be studied in observations.
ER -