We study slowly rotating black hole solutions in the Einstein-Bel-Robinson gravity (EBR) in four dimensions. At the leading order in the rotation parameter, the only modification with respect to the static case is the appearance of a nonvanishing $g_{t\varphi }$ component. We construct approximate solutions to these equations and study how physical properties of the solutions, such as the angular velocity, photon sphere, black hole shadow, and innermost stable circular orbit, are modified, working to leading order in the coupling constant and the rotation parameter. Finally, we study the superradiance of a massive scalar wave scattering off slowly rotating black holes. Using direct integration, we derive the superradiant conditions and compute the energy flux through the event horizon. We demonstrate how the flux will change as a function of the black hole rotation and frequency of the incident wave. Finally, we showed how black hole parameters, including the gravitational coupling of EBR, change during superradiance. We study the impact of the superradiant evolution on the black hole shadow and show that the shadow radius can either shrink or grow depending on the competition between the involved components during the evolution.

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• Alternative gravity theories
• Gravitation
• Classical black holes