Nucleosynthesis, neutrino bursts and γ-rays from coalescing neutron stars

Eichler, David; Livio, Mario; Piran, Tsvi; Schramm, David N.

doi:10.1038/340126a0

Cited by 2,063 publications

(2,007 citation statements)

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“…However, weak reactions at high temperatures and densities are expected to change the relative amount of neutrons and protons, as a results of an asymmetric behavior of electron neutrinos and antineutrinos. In particular, Lν e > L νe (Eichler et al 1989, Ruffert et al 1997, Rosswog & Liebendörfer 2003 and the formation of an excess ofν e deep inside the hot remnant (Foucart et al 2015) increase the proton and electron abundances. To take these effects into account, we distinguish between different regimes (also summarized in Figure 2) to initialize Y e :…”

Section: Neutrino Propertiesmentioning

confidence: 99%

“…In the case of a sufficiently close event, we expect to observe gravitational waves from terrestrial detectors; electromagnetic radiation, ranging from gamma-and X-rays related with short gamma-ray bursts, to infrared emission associated with a kilonova (Metzger et al 2010) (also called macronova, Kulkarni (2005)); and possibly neutrinos. Moreover, neutron star mergers play a critical role in the chemical evolution of the universe as they are most likely production site of half of the heavy elements via the rapid neutron capture process (r-process, Lattimer et al 1977, Eichler et al 1989, Bauswein et al 2014. Indeed, the very neutron-rich isotopes that are formed and ejected in these events power the kilonova light curve as they decay to stability.…”

Section: Introductionmentioning

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%

Section: Introductionmentioning

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 detection of a kilonova signature in the late afterglow of two sGRB has recently corroborated this picture and the conjecture that NS mergers are the progenitors of sGRBs [4]. Moreover, ν-ν annihilation above the merger remnant is considered a possible central engine for the production of such relativistic jets [5].…”

Section: Introductionmentioning

confidence: 72%

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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“…Core-collapse SNe [5] and neutron star binary mergers are considered as possible sites [6][7][8]. The first produces small amounts of material at a high event rate while the latter produces large amounts in rare events.…”

Section: Introductionmentioning

confidence: 99%

Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

Hotokezaka¹,

Piran²,

Paul³

2017

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

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Measurements of the radioactive 244 Pu abundances can break the degeneracy between high-rate/lowyield and low-rate/high-yield scenarios for the production of heavy r-process elements. The first corresponds to production by core collapse supernovae (cc-SNe) while the latter corresponds to production by e.g. neutron star binary mergers. The estimated 244 Pu abundance in the current interstellar medium inferred from deep-sea measurements is significantly lower than that corresponding Early Solar System abundances. We estimate the expected median value of the 244 Pu abundances and fluctuations around this value in both models [1]. We show that while the current and Early Solar System abundances are explained within the low-rate/high-yield scenario, they are incompatible with the high-rate/low-yield (cc-SNe) model. The inferred event rate remarkably agrees with neutron star binary merger rates estimated from Galactic neutron star binaries and from short gamma-ray bursts. The ejected mass of r-process elements per event agrees with both theoretical and observational macronova estimates.

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Nucleosynthesis, neutrino bursts and γ-rays from coalescing neutron stars

Cited by 2,063 publications

References 14 publications

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

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

Neutrinos in the Aftermath of Neutron Star Mergers

Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

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Nucleosynthesis, neutrino bursts and γ-rays from coalescing neutron stars

Cited by 2,063 publications

References 14 publications

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

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

Neutrinos in the Aftermath of Neutron Star Mergers

Short-Lived 244Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

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Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis