| Abstract : | Solar coronal plumes are long-lasting, elongated, ray-like structures predominantly visible inside the solar coronal hole. Although they have been studied for an extended period, the physics of their formation and evolution still need to be fully comprehended. It has been speculated that magnetic reconnection plays a crucial role in their formation and sustenance. In this study, we examine the evolution of a single plume from its formation to disappearance over six days. To achieve this, we conduct observations using data recorded by AIA and HMI on board the Solar Dynamics Observatory (SDO). Our observations suggest that the plume formation is a gradual process, beginning with plume haze, jet, and jetlet events. A dominant polarity magnetic field emerges at the plume's base, becoming the primary source of the plume's brightness. We found a correlation between the intensity light curve and the evolution of the magnetic field at the base of the plume. The plume exists as long as the magnetic field at the base exists. Brightness modulation of the plume also appears to be closely related to the changes in the dominant magnetic field.
Furthermore, we discover that the plume's temperature is not homogeneous. Instead, there is a temperature structure within the plume, reflected in the nature of outflows observed in different wavelength filters corresponding to different temperatures and directly verified by the Differential Emission Measure (DEM)-weighted temperature maps. Brightness modulation also closely follows the magnetic field modulation, suggesting a strong relationship between the two. The temperature structures within the plume indicate the presence of high-temperature kernels, which may contribute to the plume's long-lasting nature. |
