Nanoflare Heating: Field-Aligned Modeling and Observations of Coronal XBPs and ARs

Nanoflares are considered prime candidates for heating the non-flaring solar corona. However, direct detection of individual nanoflares with current-generation instruments remains challenging. Understanding the frequency and energy distribution of nanoflares is critical to assessing their contribution to coronal heating. In this study, we employ a field-aligned hydrodynamic model to simulate the emission from non-flaring X-ray Bright Points (XBPs) and Active Regions (ARs). The lengths and magnetic field strengths of the coronal loops are derived from magnetic field extrapolations based on photospheric magnetograms obtained by SDO/HMI. Each loop is assumed to be heated by randomly occurring nanoflares, whose frequency and magnitude depend on the loop length and magnetic field strength. The simulation results are then compared with observations to constrain the properties of nanoflares. We will present the outcomes of these studies and discuss the extent to which these models can reproduce the observed X-ray emission from coronal structures.