Fig. 1: Hills mass and superradiant spin-down due to scalars and vectors.
Gray: region in the plane of the SMBH mass MBH and spin a, where the SMBH mass exceeds the Hills mass for a Sun-like star. In this region, no observable TDEs occur for such type of stars. The spin dependence of the Hills mass is taken from ref. 4. Boundaries of the red and blue regions: maximal BH spins allowed by thin-disk spin-up and superradiant spin-down due to scalars (a) and vectors (b), for two selected ULB masses μ = 5 × 10−19 eV (red) and μ = 10−19 eV (blue). Star: maximal Hills mass allowed by an ULB with mass μ = 10−19 eV.
