The last decade has seen significant improvements in the identification and monitoring of active surface processes on Mars. Repeat observations have allowed the study of a wide range of features and processes. Many of these studies have concentrated on changes observed on the slopes of crater walls, particularly of gully (e.g., Dundas et al., 2015) and recurring slope lineae (RSL) features (e.g., McEwen et al., 2014). To date, none of these active features have been driven by endogenic processes, with environmental conditions instead the most likely explanation for change. Some of the most significant changes involving boulder movement have been identified at high latitudes on Mars, where a number of environmental processes are likely enhanced (Dundas et al., 2019). To date, such significant boulder movement has not been studied in detail at lower latitudes on Mars.On Earth, boulder size and fall frequency have been used as proxies for earthquake location (e.g., Keefer, 1984). On Mars, this correlation has been applied to studies of boulder populations in the graben of Cerberus Fossae (Brown & Roberts, 2019;Roberts et al., 2012), in addition to proposed evidence of recent, localized seismic activity in Valles Marineris, and Jezero Crater (Senthil Kumar et al., 2019;Sinha et al., 2020). However, these studies were restricted to images representing a single time period, and thus no active boulder transport was identified. Here we use repeat orbital images to study significant active boulder transport in an unnamed near-equatorial crater in Terra Sirenum (Figure 1). Dark flows on the crater walls are made mostly of meter-scale boulders, and through a rigorous co-registration procedure, we have identified several areas of active boulder transport, and discuss possible causes for the activity.