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Transport and Mixing of R-process Elements in Neutron Star Binary Merger Blast Waves by Montes, Gabriela; Ramirez-Ruiz, Enrico; Naiman, Jill; Shen, Sijing; Lee, William H. is a scholarly article available to read on EtoBox.

What is Transport and Mixing of R-process Elements in Neutron Star Binary Merger Blast Waves about?

The r-process nuclei are robustly synthesized in the material ejected during a neutron star binary merger (NSBM), as tidal torques transport angular momentum and energy through the outer Lagrange point in the form of a vast tidal tail. If NSBM are indeed solely responsible for the solar system r- process abundances, a galaxy like our own would require to host a few NSBM per million years, with each event ejecting, on average, about 5x10^{-2} M_sun of r-process material. Because the ejecta velocities in the tidal tail are significantly larger than in ordinary supernovae, NSBM deposit a comparable amount of energy into the interstellar medium (ISM). In contrast to extensive efforts studying spherical models for supernova remnant evolution, calculations quantifying the impact of NSBM ejecta in the ISM have been lacking. To better understand their evolution in a cosmological context, we perform a suite of three-dimensional hydrodynamic simulations with optically-thin radiative cooling of isolated NSBM ejecta expanding in environments with conditions adopted from Milky Way-like galaxy simulations. Although the remnant morphology is highly complex at early times, the subsequent radiative

Author

Montes, Gabriela; Ramirez-Ruiz, Enrico; Naiman, Jill; Shen, Sijing; Lee, William H.

Published

2016

Language

EN