Self-organization in continuous systems is associated with dissipative processes. In particular, for magnetized plasmas, it is known as magnetic relaxation, where the magnetic energy is converted into heat and kinetic energy of flow through the process of magnetic reconnection. An example of such a system is the solar corona, where reconnection manifests as solar transients like flares and jets. Consequently, toward investigation of plasma relaxation in solar transients, we utilize a novel approach of data-constrained MHD simulation for an observed solar flare. The selected active region NOAA 12253 hosts a GOES M1.3 class flare. The investigation of extrapolated coronal magnetic field in conjunction with the spatiotemporal evolution of the flare reveals a hyperbolic flux tube (HFT), overlying the observed brightenings. MHD simulation is carried out with the EULAG-MHD numerical model to explore the corresponding reconnection dynamics. The overall simulation shows signatures of relaxation. For a detailed analysis, we consider three distinct subvolumes. We analyze the magnetic field line dynamics along with time evolution of physically relevant quantities like magnetic energy, current density, twist, and gradients in magnetic field. In the terminal state, none of the subvolumes is seen to reach a force-free state, thus remaining in nonequilibrium, suggesting the possibility of further relaxation. We conclude that the extent of relaxation depends on the efficacy and duration of reconnection, and hence on the energetics and time span of the flare.

连续系统中的自组织与耗散过程相关。特别是，对于磁化等离子体，它被称为磁弛豫，其中磁能通过磁重联过程转化为热能和流动动能。这种系统的一个例子是日冕，其中重新连接表现为耀斑和喷流等太阳瞬变。因此，为了研究太阳瞬变中的等离子体弛豫，我们采用了一种数据约束 MHD 模拟的新方法来观测太阳耀斑。选定的活跃区域 NOAA 12253 拥有 GOES M1.3 级耀斑。对推断的日冕磁场与耀斑时空演化的研究揭示了双曲通量管（HFT），覆盖了观测到的增亮区域。利用 EULAG-MHD 数值模型进行 MHD 模拟，探索相应的重联动力学。整体模拟显示出放松的特征。为了进行详细分析，我们考虑三个不同的子卷。我们分析磁场线动力学以及物理相关量（如磁场能量、电流密度、扭曲和梯度）的时间演化。在最终状态，没有一个子体积达到无力状态，因此保持非平衡，这表明进一步松弛的可能性。我们得出的结论是，放松的程度取决于重新连接的功效和持续时间，因此也取决于耀斑的能量和时间跨度。