Studying Postmerger Outflows from Magnetized Neutrino-cooled Accretion Disks

Nouri, Fatemeh Hossein; Janiuk, Agnieszka; Przerwa, Małgorzata

doi:10.48550/arxiv.2212.05628

Cited by 1 publication

(1 citation statement)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…There is a long history of treating post-merger outflows (Ruffert et al 1997;Popham et al 1999;Kohri et al 2005) with various levels of approximation for angular momentum transport and neutrino physics, and the literature has recently exploded (Siegel & Metzger 2017Hossein Nouri et al 2018;Christie et al 2019;Fernandez et al 2019;De & Siegel 2021;Murguia-Berthier et al 2021;Fahlman & Fernandez 2022;Just et al 2022;Nouri et al 2022). An exciting recent development is the self-consistent evolution of a binary NS merger from inspiral through the remnant phase, seconds after merger (Hayashi et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Nucleosynthesis in Outflows from Black Hole–Neutron Star Merger Disks with Full GR(ν)RMHD

Curtis

Miller

Fröhlich

et al. 2023

ApJL

View full text Add to dashboard Cite

Along with binary neutron star mergers, the inspiral and merger of a black hole and a neutron star is a predicted site of r-process nucleosynthesis and associated kilonovae. For the right mass ratio, very large amounts of neutron-rich material (relative to the dynamical ejecta) may become unbound from the post-merger accretion disk. We simulate a suite of four post-merger disks with three-dimensional general-relativistic magnetohydrodynamics with time-dependent Monte Carlo neutrino transport. We find that within 104 GM BH/c 3 (∼200–500 ms), the outflows from these disks are very close to the threshold conditions for robust r-process nucleosynthesis. For these conditions, the detailed properties of the outflow determine whether a full r-process can or cannot occur, implying that a wide range of observable phenomena is possible. We show that on average the disk outflow lanthanide fraction is suppressed relative to the solar isotopic pattern. In combination with the dynamical ejecta, these outflows imply a kilonova with both blue and red components.

show abstract