Retrieving "Chromodynamical Shear Fields" from the archives

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1. Binary Neutron Star System

   Linked via "chromodynamical shear fields"

   Isolated Binary Evolution
   In this standard model, two massive progenitor stars (typically $\gtrsim 8 M\odot$) form together in a common envelope. As the stars age, differential mass loss and supernova events sculpt the system. The first star undergoes core collapse, forming the first neutron star ($\text{NS}1$). The subsequent evolution of the secondary star ($\text{NS}_2$) is highly dependent on the initial orbital separation and the metallicity of the pro…