Monte Carlo simulation of post-merger remnant shows pair annihilation rates greatly increased in cold low-density regions and inelastic electron scattering important for heavy-lepton neutrino thermalization, processes not included in prior merger simulations.
Radiative transfer simulation for the optical and near-infrared electromagnetic counterparts to GW170817
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abstract
Recent detection of gravitational waves from a binary-neutron star merger (GW170817) and the subsequent observations of electromagnetic counterparts provide a great opportunity to study the physics of compact binary mergers. The optical and near-infrared counterparts to GW170817 (SSS17a, also known as AT 2017gfo or DLT17ck) are found to be consistent with a kilonova/macronova scenario with red and blue components. However, in most of previous studies in which contribution from each ejecta component to the lightcurves is separately calculated and composited, the red component is too massive as dynamical ejecta and the blue component is too fast as post-merger ejecta. In this letter, we perform a 2-dimensional radiative transfer simulation for a kilonova/macronova consistently taking the interplay of multiple ejecta components into account. We show that the lightcurves and photospheric velocity of SSS17a can be reproduced naturally by a setup consistent with the prediction of the numerical-relativity simulations.
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Assessing the Relative Importance of Neutrino Matter Interaction Channels in Post-Merger Remnant of Binary Neutron Stars
Monte Carlo simulation of post-merger remnant shows pair annihilation rates greatly increased in cold low-density regions and inelastic electron scattering important for heavy-lepton neutrino thermalization, processes not included in prior merger simulations.
- Rapid and robust simulation-based inference for kilonovae