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We present a systematic study of magnetised neutron star head on collisions.We investigate the resulting magnetic field geometries as the two neutron starsmerge. Furthermore, we analyze the luminosity produced in these collisions andmonitor the evolution of the magnetic fields from the time of merger until thesubsequent production of a black hole. At the time of black hole formation theluminosity peaks and rings-down following the decay of the electromagneticfields. A comparison is presented for three different cases, one where theinitial magnetic field in both neutron stars is aligned, one where they areanti-aligned and also one case where they initially have unequal magnetic fieldstrength. We identify regions and set limits so that pair creation and magneticreconnection would occur in this scenario, and further discuss limits anddifferences in the radiated energy. This study should be regarded as a toymodel of the case where the remnant, of a binary neutron star merger, undergoesa prompt collapse to a black hole with a negligible surrounding disk. We notethat the generated electromagnetic pulses resembles the fast radio burstsphenomenology. We consider implications on the high mass mergers leading to afast prompt collapse to a black hole and the expected flux to be observed at adistance similar to the binary neutron star gravitational wave detectionGW190425.

A Toy Model for the Electromagnetic Output of Neutron-star Merger Prompt Collapse to a Black Hole: Magnetized Neutron-star Collisions