Tohoku University · Physics and Astronomy
Professor Masaomi Tanaka's research lab specializes in theoretical astrophysics, focusing on the nucleosynthesis and radiative transfer processes in neutron star mergers. The lab investigates the formation and observational signatures of kilonovae, particularly the role of r-process elements and their atomic opacities in shaping electromagnetic counterparts to gravitational wave events like GW170817. Using advanced atomic structure calculations, the lab explores element-specific radiative properties to interpret multi-messenger observations. Their work bridges nuclear physics, atomic physics, and observational astrophysics to understand the origin of heavy elements in the universe.
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Abstract Recent detection of gravitational waves from a neutron star (NS) merger event GW170817 and identification of an electromagnetic counterpart provide a unique opportunity to study the physical processes in NS mergers. To derive properties of ejected material from the NS merger, we perform radiative transfer simulations of kilonova, optical and near-infrared emissions powered by radioactive decays of r-process nuclei synthesized in the merger. We find that the observed near-infrared emissi
ABSTRACT Coalescence of neutron stars (NSs) gives rise to kilonova, thermal emission powered by radioactive decays of freshly synthesized r-process nuclei. Although observational properties are largely affected by bound–bound opacities of r-process elements, available atomic data have been limited. In this paper, we study element-to-element variation of the opacities in the ejecta of NS mergers by performing systematic atomic structure calculations of r-process elements for the first time. We sh
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