3D GRMHD collapsar simulations initialized with toroidal fields demonstrate that an accretion-disk dynamo generates poloidal fields and launches variable, wobbling jets with LGRB-comparable power.
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Primordial black holes captured by stars lead to either quiet consumption or explosive disruption via disk formation, producing transients and high-spin remnants with potentially observable event rates.
Neutrino-cooled collapsar disks in 3D GRMHD simulations lead to black hole equilibrium spins of a_eq ≈ 0.13, enabling 4-16x more powerful LGRB jets than non-radiative models.
GW190814 is proposed to originate from a collapsar-disk fragment merging with the central black hole, potentially preceded by SN2019npv ~60 days earlier, yielding H0 = 70.5 (+9.2, -6.4) km/s/Mpc.
Simulations show hierarchical subsolar-mass mergers in collapsar disks can retain eccentricity up to e~0.1 at merger as a potential observational signature.
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