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ORIGINAL RESEARCH article

Front. Astron. Space Sci.
Sec. Stellar and Solar Physics
Volume 11 - 2024 | doi: 10.3389/fspas.2024.1369362
This article is part of the Research Topic Advances On The Initiation And Evolution Of CMEs Involving Remote And In-situ Observations Within 0.5 AU, Theory, Modeling, And Simulations View all 3 articles

Triggering Mechanism of an Eruptive Filament Located in a Weak Active Region

Provisionally accepted
Peng Zou Peng Zou 1*Chaowei Jiang Chaowei Jiang 1Xinkai Bian Xinkai Bian 1Juntao Wang Juntao Wang 1,2
  • 1 Harbin Institute of Technology, Shenzhen, Shenzhen, China
  • 2 Lingnan Normal University, Zhanjiang, Guangdong, China

The final, formatted version of the article will be published soon.

    The triggering mechanism for those filament located in weak magnetic field typically leans toward magnetohydrodynamics instabilities due to the weak magnetic strength inherent in filament structures.However, there still remains a subset of eruption events associated with significant flares. Therefore, we seek to understand the role that reconnection plays in the eruption of filaments with weak magnetic field. In this context, we present a case study of an eruptive filament located in relatively weaker magnetic environment. This filament remains stable until the expansion of the heated bright arcades underneath. This expansion initially activates the filament, prompting its upward movement and leading to a gentle reconnection slightly to the south of them. The ensuing reconnection continues to propel the filament upward with uniform acceleration. These upward motions cause the drainage of filament mass, likely activating the torus instability of the filament. This torus instability then triggers the final eruption of the filament, successfully generating a coronal mass ejection (CME) and leaving behind a double-ribbon flare. Based on this scenario, we conclude that the torus instability serves as the primary triggering mechanism of this eruption, while pre-eruption reconnection plays a role in pushing the filament upward to meet the instability condition.

    Keywords: Sun: coronal mass ejections (CMEs), Sun: filaments, prominences, Sun: magnetic fields, Magnetic Reconenction, Magnetic reconstruction

    Received: 12 Jan 2024; Accepted: 24 Jul 2024.

    Copyright: © 2024 Zou, Jiang, Bian and Wang. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) or licensor are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.

    * Correspondence: Peng Zou, Harbin Institute of Technology, Shenzhen, Shenzhen, China

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