2004/03/16 by Madappa Prakash, Sasa Ratkovic, Sa a Ratkovi +1
Mathematics · Physics and Astronomy · #Astrobiology #Astronomy #Astrophysics #Binary number #Gamma-ray bursts and supernovae #Mathematics #Physics #Pulsars and Gravitational Waves Research #Stars #Stellar, planetary, and galactic studies #astro-ph #gr-qc #nucl-th
paper · pdf · doi:10.1088/0954-3899/30/8/108
published as J.Phys. G30 (2004) S1279-S1282 · Contribution to QM04 proceedings. Submitted to Journal of Physics G
arxiv created 2004/03/16 · openalex publication_date 2004/07/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract. The mergers of black hole-neutron star binaries are calcuated using a pseudo-general relativistic potential that incorporates O(v 2 /c 2) 3 post-Newtonian corrections. Both normal matter neutron stars and self-bound strange quark matter stars are considered as black hole partners. As long as the neutron stars are not too massive relative to the black hole mass, orbital decay terminates in stable mass transfer rather than an actual merger. For a normal neutron star, mass transfer results in a widening of the orbit but the stable transfer ends before the minimum neutron star mass is reached. For a strange star, mass transfer does not result in an appreciable enlargement of the orbital separation, and the stable transfer continues until the strange star essentially disappears. These differences might be observable through their respective gravitational wave signatures. Mergers of binary stars: The ultimate heavy-ion experience 2 The closest analog of a high-energy heavy-ion collision in nature is the gravitational wave-induced merger of two compact objects involving at least one neutron star or strange quark matter star in a binary system. However, since such a collision would involve more than 10 57 particles, it is vastly more energetic and would represent the