{'fraction_non_alphanumeric': 0.019402985074626865, 'fraction_numerical': 0.008208955223880597, 'mean_word_length': 4.96, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 0, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
Global evaluation of coronal heating due to magnetic reconnection based on solar dynamics observatory observations

The energy flux released into the corona is estimated from magnetic reconnection events in all spatial scales, covering down to nanoflares. The reconnection model used is based on a quasi-3D configuration that approximates the braiding of magnetic field lines which is produced by photospheric motions and includes both resistive and collisionless reconnection, depending on the event size [Martinell, J.J. Rad. Effects Defec. Solids 2010, 165, 114]. This model is applied to all length scales involved in the energy release adding all them up. In order to obtain the size distribution, the observations of the Solar Dynamics Observatory (SDO) are used for two wavelengths in the far UV, together with the corresponding magnetograms and look for correlations brightness-magnetic field. Since the resolution limit of the SDO is just above the nanoflare scales, the spectral index of the energy distribution is determined and it is used to extrapolate down to nanoflare scales. An upper limit of the energy flux is obtained following two different methods, as well as an estimate for the aspect ratio of the current sheets. The energy flux estimates are in the range of which is of the order needed to maintain the hot corona.