r-Java 2.0: the astrophysics

Kostka, M.; Koning, N.; Shand, Z.; Ouyed, R.; Jaikumar, P.

doi:10.48550/arxiv.1402.3824

Cited by 3 publications

(8 citation statements)

References 68 publications

(120 reference statements)

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“…To perform the calculations we have chosen the r-java2.0 code, developed by the Calgary University group. [43][44][45] This code solves the nuclear r-process network coupled to an astrophysical scenario. We have modified the inputs of the code to include the βdecay rates of Eq.…”

Section: Calculation Of Heavy Nuclei Abundancesmentioning

confidence: 99%

“…To characterize the neutrino wind, we have chosen the initial temperature as T 0 = 3 × 10 9 K, the density profile ρ = ρ 0 (1+t/(2τ )) 2 where the initial density is ρ 0 = 10 11 g/cm 3 and the expansion time-scale is τ = 0.1 s. The wind speed of expansion was set to Vexp = 7500 km/s and the initial wind radius fixed at R 0 = 390 km. 41,43,44,[46][47][48] b) a neutron-star merger (NSm);…”

Section: Calculation Of Heavy Nuclei Abundancesmentioning

confidence: 99%

“…This environment was characterized by an initial temperature T 0 = 3 × 10 9 K and the polytropic profile P = Kρ (n+1)/n where the polytropic index is fixed at n = 1.5 and K is constant. 44 The initial density and the internal pressure were set to ρ 0 = 10 11 g/cm 3 and P 0 = 0.005 MeV/fm 3 respectively. Finally, the expansion velocity was fixed at Vexp = 1.9×10 5 km/s and the initial radius of the ejecta at R 0 = 2 km.…”

Section: Calculation Of Heavy Nuclei Abundancesmentioning

confidence: 99%

“…For the neutron-star mergers we have considered two values for Ye, namely 0.1 and 0.3, and performed a combination of both computed abundances to obtain their final values, as done in. 44,51,52…”

Section: Calculation Of Heavy Nuclei Abundancesmentioning

confidence: 99%

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Limits on active-sterile neutrino mixing parameters using heavy nuclei abundances

Saez

Fushimi

Mosquera

et al. 2021

Int. J. Mod. Phys. E

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The production of heavy-mass elements due to the rapid neutron-capture mechanism ([Formula: see text]-process) is associated with astrophysical scenarios, such as supernovae and neutron-star mergers. In the [Formula: see text]-process the capture of neutrons is followed by [Formula: see text]-decays until nuclear stability is reached. A key element in the chain of nuclear weak-decays leading to the production of isotopes may be the change of the parameters controlling the neutrino sector, due to the mixing of active and sterile species. In this work, we have addressed this question and calculated [Formula: see text]-decay rates for the nuclei involved in the [Formula: see text]-process chains as a function of the neutrino mixing parameters. These rates are then used in the calculation of the abundance of the heavy elements produced in core-collapse supernova and in neutron-star mergers, starting from different initial mass-fraction distributions. The analysis shows that the core-collapse supernova environment contributes with approximately [Formula: see text] of the total heavy nuclei abundance while the neutron-star merger contributes with about [Formula: see text] of it. Using available experimental data we have performed a statistical analysis to set limits on the active-sterile neutrino mixing angle and found a best-fit value [Formula: see text], a value comparable with those found in other studies reported in the literature.

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Section: Calculation Of Heavy Nuclei Abundancesmentioning

confidence: 99%

Section: Calculation Of Heavy Nuclei Abundancesmentioning

confidence: 99%

Section: Calculation Of Heavy Nuclei Abundancesmentioning

confidence: 99%

Section: Calculation Of Heavy Nuclei Abundancesmentioning

confidence: 99%

See 2 more Smart Citations

Limits on active-sterile neutrino mixing parameters using heavy nuclei abundances

Saez

Fushimi

Mosquera

et al. 2021

Int. J. Mod. Phys. E

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“…We generate our r-process simulation data using an extension of the r-Java 2.0 code [12,13] that now includes a graphical-user interface (GUI) module for sensitivity runs. This first-of-its-kind code, "SiRop", allows users to run the r-process simulation and output sensitivity metrics in a single Java-based application in order to represent and analyze changes in the abundance curves.…”

Section: Simulation Parametersmentioning

confidence: 99%

Critical assessment of nuclear sensitivity metrics for the r-process

Shand¹,

Ouyed²,

Koning³

et al. 2017

Preprint

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Any simulation of the r-process is affected by uncertainties in our present knowledge of nuclear physics quantities and astrophysical conditions. It is common to quantify the impact of these uncertainties through a global sensitivity metric, which is then used to identify specific nuclides that would be most worthwhile to measure experimentally. Using descriptive statistics, we assess a set of metrics used in previous sensitivity studies, as well as a new logarithmic measure. For certain neutron-rich nuclides lying near the r-process path for the typical hot-wind scenario, we find opposing conclusions on their relative sensitivity implied by different metrics, although they all generally agree which ones are the most sensitive nuclei. The underlying reason is that sensitivity metrics which simply sum over variations in the r-process distribution depend on the scaling used in the baseline, which often varies between simulations. We show that normalization of the abundances causes changes in the reported sensitivity factors and recommend reporting a minimized F statistic in addition to a scale estimation for rough calibration to be used when comparing tables of sensitivity factors from different studies.

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A quark nova in the wake of a core-collapse supernova: a unifying model for long duration gamma-ray bursts and fast radio bursts

Ouyed

Leahy

Koning

2020

Res. Astron. Astrophys.

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By appealing to a Quark-Nova (QN; the explosive transition of a neutron star to a quark star) in the wake of a core-collapse Supernova explosion of a massive star, we develop a unified model for long duration Gamma-ray Bursts (LGRBs) and Fast Radio Bursts (FRBs). The time delay (years to decades) between the SN and the QN and, the fragmented nature (i.e. millions of chunks) of the relativistic QN ejecta are key to yielding a robust LGRB engine. In our model, a LGRB light-curve exhibits the interaction of the fragmented QN ejecta with a turbulent (i.e. filamentary and magnetically saturated) SN ejecta which is shaped by its interaction with an underlying pulsar wind nebula (PWN). The afterglow is due to the interaction of the QN chunks, exiting the SN ejecta, with the surrounding medium. Our model can fit BAT/XRT prompt and afterglow light-curves, simultaneously with their spectra, thus yielding the observed properties of LGRBs (e.g. the Band function and the X-ray flares). We find that the peak luminosity-peak photon energy relationship (i.e. the Yonetoku law), and the isotropic energy-peak photon energy relationship (i.e. the Amati law) are not fundamental but phenomenological. FRBs in our model result from coherent synchrotron emission (CSE) when the QN chunks interact with non-turbulent weakly magnetized PWN-SN ejecta, where conditions are prone to the Weibel instability. Magnetic field amplification induced by the Weibel instability in the shocked chunk frame sets the bunching length for electrons and pairs to radiate coherently. The resulting emission frequency, luminosity, duration and dispersion measure (DM) in our model are consistent with FRB data. We find a natural unification of high-energy burst phenomena from FRBs to LGRBs including X-ray Flashes (XRFs) and X-ray rich GRBs (XRR-GRBs) as well as Super-Luminous SNe (SLSNe). We find a possible connection between Ultra-High Energy Cosmic Rays and FRBs and propose that a QN following a binary neutron star merger can yield a short GRB (SGRB) with fits to BAT/XRT light-curves.

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r-Java 2.0: the astrophysics

Cited by 3 publications

References 68 publications

Limits on active-sterile neutrino mixing parameters using heavy nuclei abundances

Limits on active-sterile neutrino mixing parameters using heavy nuclei abundances

Critical assessment of nuclear sensitivity metrics for the r-process

A quark nova in the wake of a core-collapse supernova: a unifying model for long duration gamma-ray bursts and fast radio bursts

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