Nucleosynthesis in 2D core-collapse supernovae of 11.2 and 17.0 M<sub>⊙</sub>progenitors: implications for Mo and Ru production

Eichler, Marius; Nakamura, Ko; Takiwaki, Tomoya; Kuroda, T.; Kotake, Kei; Hempel, Matthias; Cabezón, Rubén M.; Liebendörfer, M.; Thielemann, Friedrich‐Karl

doi:10.1088/1361-6471/aa8891

Cited by 59 publications

(54 citation statements)

References 94 publications

(287 reference statements)

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“…But in standard CC SNe, the matter is mainly ejected by neutrinos, which reduce the number of neutrons by converting them into protons. In such conditions, current simulations indicate that standard CC SNe could at most produce trans-iron elements like Sr, Y, Zr, Mo, and Ru (first-peak elements), and perhaps in some cases elements up to Ag (e.g., Roberts et al 2010;Arcones & Montes 2011;Eichler et al 2018;Bliss et al 2018 and references therein). In order to produce heavier elements such as Eu, another ejection mechanism is necessary.…”

Section: C2 Core-collapse Supernovaementioning

confidence: 84%

Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way

Côté

Eichler

Arcones

et al. 2019

ApJ

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219

192

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Probing the origin of r-process elements in the universe represents a multi-disciplinary challenge. We review the observational evidence that probe the properties of r-process sites, and address them using galactic chemical evolution simulations, binary population synthesis models, and nucleosynthesis calculations. Our motivation is to define which astrophysical sites have significantly contributed to the total mass of r-process elements present in our Galaxy. We found discrepancies with the neutron star (NS-NS) merger scenario. Assuming they are the only site, the decreasing trend of [Eu/Fe] at [Fe/H] > −1 in the disk of the Milky Way cannot be reproduced while accounting for the delaytime distribution (DTD) of coalescence times (∝ t −1 ) derived from short gamma-ray bursts and population synthesis models. Steeper DTD functions (∝ t −1.5 ) or power laws combined with a strong burst of mergers before the onset of Type Ia supernovae can reproduce the [Eu/Fe] trend, but this scenario is inconsistent with the similar fraction of short gamma-ray bursts and Type Ia supernovae occurring in early-type galaxies, and reduces the probability of detecting GW170817 in an early-type galaxy. One solution is to assume an extra production site of Eu that would be active in the early universe, but would fade away with increasing metallicity. If this is correct, this extra site could be responsible for roughly 50 % of the Eu production in the early universe, before the onset of Type Ia supernovae. Rare classes of supernovae could be this additional r-process source, but hydrodynamic simulations still need to ensure the conditions for a robust r-process pattern.

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Section: C2 Core-collapse Supernovaementioning

confidence: 84%

Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way

Côté

Eichler

Arcones

et al. 2019

ApJ

Self Cite

219

192

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“…Arlandini et al 1999;Käppeler et al 2011;Prantzos et al 2020), might combine a number of different contributions. Especially the light trans-Fe elements like Sr, Y, Zr, seem to have also other origins aside from the typical r-process (Travaglio et al 2004;Fröhlich et al 2006;Farouqi et al 2009;Hansen et al 2012Hansen et al , 2014aEichler et al 2018;Akram et al 2020) which could possibly be attributed to regular core-collapse supernovae. When looking at the SAGA database (only for Milky Way stars) in this metallicity window, one recognizes that one finds Fe and Sr detections in 1277 of them, but Fe and Eu detections only in 498 stars (combined with a strong scatter in the Eu abundances).…”

Section: Introductionmentioning

confidence: 99%

Correlations of r-Process Elements in Very Metal-Poor Stars as Clues to their Nucleosynthesis Sites

Farouqi,

Thielemann,

Rosswog

et al. 2021

Preprint

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Aims. Various nucleosynthesis studies have pointed out that the r-process elements in very metal-poor (VMP) halo stars might have different origins. By means of familiar concepts from statistics (correlations, cluster analysis, rank tests of elemental abundances), we look for causally correlated elemental abundance patterns and attempt to link them to astrophysical events. Some of these events produce the r-process elements jointly with iron, while others do not have any significant iron contribution. We try to (a) characterize these different types of events by their abundance patterns and (b) identify them among the existing set of suggested r-process sites. Methods. The Pearson and Spearman correlation coefficients are used in order to investigate the relationship between iron and the r-process elements (X) in VMP halo stars. We gradually track the evolution of those coefficients in terms of the element-enrichment with respect to Fe [X/Fe] and the metallicity [Fe/H]. This approach, aided by cluster analysis to find different structures of abundance patterns and rank tests to identify whether several events contributed to the observed pattern is new and provides deeper insights into the abundances of VMP stars. Results. In the early stage of our Galaxy, at least three r-process nucleosynthesis sites have been active. The first two produce and eject iron and the majority of the lighter r-process elements. We assign them to two different types of core-collapse events, not identical to regular core-collapse supernovae (CCSNe), which produce only light trans-Fe elements. The third category is characterized by a strong r-process and responsible for the major fraction of the heavy main r-process elements without a significant co-production of Fe. It does not appear to be connected to CCSNe, in fact the Fe found in the related r-process enriched stars must come from previously occurring CCSNe. The existence of actinide boost stars indicates a further division among strong r-process sites. We assign these two strong r-process sites to neutron star mergers without fast black hole formation and to events where the ejecta are dominated by black hole accretion disk outflows. Indications from the lowest-metallicity stars hint at a connection to massive single stars (collapsars) forming black holes in the early Galaxy.

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“…The authors have found out that proton-rich winds may be predominant contributors to the solar abundance of 98 Ru, significant contributions to those of 96 Ru (≲40%) and 92 Mo (≲27%), and relatively minor contributions to that of 94 Mo (≲14%). The production of 92 Mo and 94 Mo is observed in slightly neutron-rich conditions in 11 and 17 M  simulations, 96,98 Ru can only be produced efficiently via the νpprocess and heavily depends on the presence of very proton-rich material in the ejecta (Eichler et al, 2018). SNIa have been suggested as a site for the production of pnuclides for the abundance ratios 92 Mo/ 94 Mo (Travaglio et al, 2015, Nishimura et al, 2018.…”

Section: Mo and Ru Nucleosynthesismentioning

confidence: 96%

Molybdenum and Ruthenium in the Galaxy

Gorbaneva

2018

OAP

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We present a brief overview of the molybdenum and ruthenium present-day nucleosynthesis calculations and abundance determinations in stars belonging to different substructures (populations) in the Galaxy. The following sources of Mo, Ru production were considered: the Asymptotic Giant Branch (AGB) stars of different masses (main s-process), massive stars (weak s-process), neutrino-induced winds from the core-collapse supernova CCSNe (weak r-process), merging of neutron stars (main rprocess). Many production sites of the p-nuclei have been proposed: the Type II and Ia supernovae (at the presupernova phase, during and after the supernova explosion), the rp-process in neutrino-driven winds, the high-entropy wind (HEW), the νp-process; inside in a supercritical accretion disk (SSAD), in the He-accreting CO white dwarfs of sub-Chandrasekhar mass, and in the carbon deflagration model for Type Ia. We also emphasize on some additional processes such as the i-process in rapidly accreting white dwarfs (RAWDs), the lighter element primary process LEPP as well as another formation channel, namely the charged-particle process (r-process). The contribution to the solar abundance of neutron capture elements and the Galactic Chemical Evolution (GCE) models for n-capture elements were considered. The Mo and Ru observations in metal-poor stars, Ba stars, globular clusters, meteoritic matter (presolar grains) as well as our new Mo and Ru determinations in Galactic disc are presented. Having analysed our date in the near solar metallicities we found out that there are different sources contributing to the Mo and Ru abundances, and that the main s-process contribution to the Mo and Ru abundances is lower than to the predominant s-element (Y, Zr and Ba) solar abundances. By comparing the behavior of Mo and Ru in the wide range of [Fe/H] with GCE models one can see that the theoretical description of the galactic behavior of Mo not depicts sufficient and we are faced with the underproduction of molybdenum in the sources and in processes that used at the GCE creation. Additional sources may be the p-process (SN Ia and/or SN II), νp-process (massive stars) or several more exotic processes.

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Nucleosynthesis in 2D core-collapse supernovae of 11.2 and 17.0 M_⊙progenitors: implications for Mo and Ru production

Cited by 59 publications

References 94 publications

Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way

Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way

Correlations of r-Process Elements in Very Metal-Poor Stars as Clues to their Nucleosynthesis Sites

Molybdenum and Ruthenium in the Galaxy

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Nucleosynthesis in 2D core-collapse supernovae of 11.2 and 17.0 M⊙progenitors: implications for Mo and Ru production

Cited by 59 publications

References 94 publications

Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way

Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way

Correlations of r-Process Elements in Very Metal-Poor Stars as Clues to their Nucleosynthesis Sites

Molybdenum and Ruthenium in the Galaxy

Contact Info

Product

Resources

About

Nucleosynthesis in 2D core-collapse supernovae of 11.2 and 17.0 M_⊙progenitors: implications for Mo and Ru production