Solar flare observations with Chandrayaan-2 Solar X-ray Monitor

Solar flares ranging from small microflares to large X-class flares are believed to be the result of sudden release of magnetic energy in the atmosphere of the Sun. Measuring the distribution of various flare parameters over a wide range of flare intensities provide a good opportunity to investigate the scale invariance of the underlying physical processes. Solar X-ray Monitor (XSM) on board Chandrayaan-2 has been observing the Sun for more than three years, providing soft X-ray spectral measurements and has detected a many flares from sub-A class to X-class. XSM data provides a great opportunity for statistical studies of the solar flare parameters. For this purpose, we developed an automated flare-detection algorithm to identify the different flaring episodes from the XSM light curves that provide the start and end times of the flares in addition to the peak time. As the XSM observations often have gaps due to the Sun being out of its field of view, the algorithm is designed taking these gaps into consideration. The algorithm is applied on the XSM observations during its primary observing seasons to generate a flare database which is planned to be regularly updated and made available on the XSM website along with additional information of the flares from other sources. Here we present the details of the flare detection techniques and the results. We also discuss the preliminary flare parameter distributions and their future potential.