Circumstellar disks of planetesimals known as debris disks are an integral component of planetary systems. They are analogous to the Solar System’s Kuiper and asteroid belts, with observable structures that indicate the presence, properties and dynamical history of planets that interact with the disk. Beta Pictoris hosts one of the most well-studied debris disks, yet despite the wealth of observations, the nature of a prominent clump of dust and gas in the disk remains uncertain. Such a brightness asymmetry is rarely witnessed in debris disks, and could be a sign of past or ongoing interactions involving planets. We recently studied multi-epoch mid-infrared images of the debris disk of Beta Pictoris, which together constrain any projected motion of the dust clump. The results suggest that the dust clump is likely stationary, which disfavours the scenario in which it originated from planetesimals in resonance with a perturbing planet. Although the observations do not firmly rule out this model, they set constraints on the properties required of any perturbing planets. Several scenarios are possible in which the dust clump is expected to be stationary, such as a giant impact involving a planet-sized body. Upcoming observations with JWST are expected to provide further constraints on the dust clump’s morphology and motion as well as the presence of any planets, which would further constrain or even rule out theories on the dynamical scenario in the system.