Tidal disruption events around spherically symmetric compact boson stars Matheus C. Teodoro Institute of Physics, University of Oldenburg, 26111 Oldenburg, Germany E-mail: matheus.do.carmo.teodoro@uol.de Lucas G. Collodel Theoretical Astrophysics, University of T¨ ubingen, 72076 T¨ ubingen, Germany E-mail: lucas.gardai-collodel@uni-tuebingen.de Jutta Kunz Institute of Physics, University of Oldenburg, 26111 Oldenburg, Germany E-mail: jutta.kunz@uni-oldenburg.de Abstract. We report simulations regarding tidal disruption clouds orbiting spherically symmetric compact boson stars in two different regimes, performed in 2D. First we consider clouds in three different bound orbits close to the boson star and analyze the mechanisms of debris formation for these. We infer from the simulations that the lifetimes of these hot-spots are longer for circularly orbiting clouds than for clouds on eccentric orbits. Next we compare the evolution of more extended and less dense clouds on circular orbits around a boson star and a Schwarzschild black hole. As an outcome of the simulations we observe the formation of a ring-like structure around the boson star endowed with a spiralling shock structure and a constant thermal bremsstrahlung total luminosity. This final configuration contrasts strongly with the black hole scenario where the gas is totally captured behind the event horizon. 1. Introduction Among the most powerful events in the universe, accretion onto compact objects has been driving the attention of the scientific community for decades, not only due to its fascinating complexity which arises from the combination of gravity and fluid dynamics, but also due to its importance for observational astrophysics, recently realized in the observation of the accretion disc and the shadow of the compact object at the center of M87 [1], for which general relativistic magnetohydrodynamics simulations were crucial in the data processing and analysis. Regarding accretion, many other scenarios different from accretion discs have relevance. Proposed in 1975 [2] as an accretion mechanism onto arXiv:2003.05220v2 [astro-ph.HE] 26 May 2020