2024/05/22 by Beyhan Karakas, Karakas, Beyhan, Rahime Matur +3 · 1 citation
Physics and Astronomy · #FOS: Physical sciences #Gamma-ray bursts and supernovae #General Relativity and Quantum Cosmology (gr-qc) #High Energy Astrophysical Phenomena (astro-ph.HE) #Pulsars and Gravitational Waves Research
paper · doi:10.48550/arxiv.2405.13687
openalex publication_date 2024/05/22 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/01
We investigate the effect of spin on equal and unequal mass binary neutron star mergers using finite-temperature, composition-dependent Steiner-Fischer-Hempel equation of state with parameter set ``o'' (SFHo), via 3+1 general relativistic hydrodynamics simulations which take into account neutrino emission and absorption. Equal mass, irrotational cases that have a mass of M1,2 =1.27M\odot, result in a long-lived neutron star, while 1.52 and 2.05M\odot cases lead to a prompt collapse to a black hole. For all cases, we analyse the effect of initial spin on dynamics, on the structure of the final remnant, its spin evolution, the amount and composition of the ejected matter, gravitational waves, neutrino energies and luminosities, and disc masses. We show that in equal mass binary neutron star mergers, the ejected mass could reach ∼0.06M\odot for highly aligned-spins (χ=0.67). The black hole which results from such a highly spinning, high-mass binary neutron star merger reaches a dimensionless spin of 0.92; this is the highest spin reached in binary neutron star mergers, to date.