Neutrino-Driven Winds in the Aftermath of a Neutron Star Merger: Nucleosynthesis and Electromagnetic Transients

Martin, Dirk; Perego, Albino; Arcones, Almudena; Thielemann, Friedrich‐Karl; Korobkin, Oleg; Rosswog, Stephan

doi:10.1088/0004-637x/813/1/2

Cited by 250 publications

(277 citation statements)

References 98 publications

(173 reference statements)

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“…We map the outcome of a general relativistic binary merger simulation ‡ into the FISH+ASL code (Käppeli et al 2011, Perego et al 2016. The latter has been extensively employed to study the evolution of binary merger remnants and their neutrino emission (Perego et al 2014, Martin et al 2015. For the mapping, we choose a time step corresponding to ∼ 15 ms after the first touch t m .…”

Section: Neutrino Propertiesmentioning

confidence: 99%

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The role of weak interactions in dynamic ejecta from binary neutron star mergers

Martin

Perego

Kastaun

et al. 2018

Class. Quantum Grav.

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Abstract. Weak reactions are critical for the neutron richness of the matter dynamically ejected after the merger of two neutron stars. The neutron richness, defined by the electron fraction (Y e ), determines which heavy elements are produced by the r-process and thus directly impacts the kilonova light curve. In this work, we have performed a systematic and detailed post-processing study of the impact of weak reactions on the distribution of the electron fraction and of the entropy on the dynamic ejecta obtained from an equal mass neutron star binary merger simulated in full general relativity and with microscopic equation of state. Previous investigations indicated that shocks increase Y e , however our results show that shocks can also decrease Y e , depending on their thermodynamical conditions. Moreover, we have found that neutrino absorption are key and need to be considered in future simulations. We also demonstrated that the angular dependence of the neutrino luminosity and the spatial distribution of the ejecta can lead to significant difference in the electron fraction distribution. In addition to the detailed study of the Y e evolution and its dependences, we have performed nucleosynthesis calculations. They clearly point to the necessity of improving the neutrino treatment in current simulations to be able to predict the contribution of neutron star mergers to the chemical history of the universe and to reliable calculate their kilonova light curves.

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Section: Neutrino Propertiesmentioning

confidence: 99%

“…In order to determine the composition of the fluid along the trajectories, we employ a complete nuclear reaction network (Winteler et al 2012, Korobkin et al 2012, Martin et al 2015. It includes over 5800 nuclei between the valley of stability and the neutron drip line, comprising isotopes from H to Rg.…”

Section: Nuclear Networkmentioning

confidence: 99%

The role of weak interactions in dynamic ejecta from binary neutron star mergers

Martin

Perego

Kastaun

et al. 2018

Class. Quantum Grav.

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“…The dominant absorption of ν e inside the wind increases the electron fraction and the matter entropy. [10]) and wind (coloured, [9]) ejecta. For the wind ejecta, we distinguish between different final times.…”

Section: Neutrino-driven Wind: Nucleosynthesis and Electromagnetic Trmentioning

confidence: 99%

“…We analyzed the properties of the tracer particles ejected in the simulation [9]. The electron fraction covered a broad range of values, ranging from 0.2 to 0.4.…”

Section: Neutrino-driven Wind: Nucleosynthesis and Electromagnetic Trmentioning

confidence: 99%

Neutrinos in the Aftermath of Neutron Star Mergers

Perego¹,

Arcones²,

Martin³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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We performed three dimensional hydrodynamics simulations of the aftermath of a binary neutron star merger under the influence of neutrinos and in presence of a long-lived massive neutron star. Neutrino absorption inside the remnant triggers a ν-driven wind, inside which a significant amount of matter is ejected over several dynamical time scales. The increased electron fraction produces weak r-process nucleosynthesis in the ejecta, which powers an electromagnetic transient earlier and bluer than the one expected from full r-process nucleosynthesis. The presence of a massive neutron star in the centre increases significantly the rate at which neutrino pairs can deposit energy in the funnel above the remnant.

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“…The final stages of neutron-star demise can be the origin [31,32] of some of the recently observed [33] fast radio bursts (FRBs), as well as x-ray and γ-ray transients. A kilonova-type [34][35][36][37][38][39][40][41] afterglow can accompany the decompressing nuclear matter ejecta, but unlike COMs, these events are not associated with a significant release of neutrinos or gravitational radiation. Therefore, future observations of gravitational waves and kilonovae will be able to distinguish between r-process scenarios.…”

mentioning

confidence: 99%