Abundances of La138 and Ta180 Through ν-Nucleosynthesis in 20M ⊙ Type II Supernova Progenitor, Guided by Stellar Models for Seeds

Lahkar, Narendra; Kalita, Sanjeev; Duorah, H. L.; Duorah, K.

doi:10.1007/s12036-017-9428-y

Cited by 8 publications

(5 citation statements)

References 14 publications

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“…Since 180 Ta and 138 La are both produced after the first neutrino burst and before the phase transition induced explosion, the EoS would have little effect on their production. Additional and more detailed discussion about the interesting isotopes 138 La and 180 Ta can be found here (Arnould & Goriely 2003;Byelikov et al 2007;Austin et al 2011;Lahkar et al 2017;Sieverding et al 2018). 11 B is another rare 𝜈-process isotope that shows large production factors for both progenitors in Figure 13 and 14.…”

Section: 43mentioning

confidence: 99%

The Role of the Hadron-Quark Phase Transition in Core-Collapse Supernovae

Jakobus,

Mueller,

Heger

et al. 2022

Preprint

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The hadron-quark phase transition in quantum chromodyanmics has been suggested as an alternative explosion mechanism for core-collapse supernovae. We study the impact of three different hadron-quark equations of state (EoS) with first-order (DD2F, STOF-B145) and second-order (CMF) phase transitions on supernova dynamics by performing 97 simulations for solarand zero-metallicity progenitors in the range of 14-100 M . We find explosions only for two low-compactness models (14M and 16 M ) with the DD2F EoS, both with low explosion energies of ∼10 50 erg. These weak explosions are characterised by a neutrino signal with several mini-bursts in the explosion phase due to complex reverse shock dynamics, in addition to the typical second neutrino burst for phase-transition driven explosions. The nucleosynthesis shows significant overproduction of nuclei such as 90 Zr for the 14 M zero-metallicity model and 94 Zr for the 16 M solar-metallicity model, but the overproduction factors are not large enough to place constraints on the occurrence of such explosions. Several other low-compactness models using the DD2F EoS and two high-compactness models using the STOS EoS end up as failed explosions and emit a second neutrino burst. For the CMF EoS, the phase transition never leads to a second bounce and explosion. For all three EoS, inverted convection occurs deep in the core of the proto-compact star due to anomalous behaviour of thermodynamic derivatives in the mixed phase, which heats the core to entropies up to 4𝑘 B /baryon and may have a distinctive gravitational wave signature, also for a second-order phase transition.

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Section: 43mentioning

confidence: 99%

The Role of the Hadron-Quark Phase Transition in Core-Collapse Supernovae

Jakobus,

Mueller,

Heger

et al. 2022

Preprint

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“…Related references. 7 Li (Woosley et al 1990), (Yoshida et al 2004), (Yoshida et al 2005), (Yoshida et al 2006), (Yoshida et al 2008), (Suzuki & Kajino 2013), (Kusakabe et al 2019) 11 B (Woosley et al 1990), (Yoshida et al 2004), (Yoshida et al 2005), (Yoshida et al 2006), (Yoshida et al 2008), (Nakamura et al 2010), (Austin et al 2011), (Suzuki & Kajino 2013), (Kusakabe et al 2019) 19 F (Woosley et al 1990), (Sieverding et al 2018), (Olive & Vangioni 2019) 93 Nb (Hayakawa et al 2013) 98 Tc (Hayakawa et al 2018) 138 La (Woosley et al 1990), (Sieverding et al 2018), (Heger et al 2005), (Hayakawa et al 2008), (Byelikov et al 2007), (Rauscher et al 2013), (Kajino et al 2014), (Kheswa et al 2015) (Lahkar et al 2017) 180 Ta (Woosley et al 1990), (Heger et al 2005), (Hayakawa et al 2010), (Byelikov et al 2007), (Rauscher et al 2013), (Kajino et al 2014) (Lahkar et al 2017), (Ma...…”

Section: Elementmentioning

confidence: 99%

Comprehensive Analyses of the Neutrino-Process in the Core-collapsing Supernova

Ko,

Jang,

Cheoun

et al. 2022

Preprint

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We investigate the effects of the neutrino flavor change by the neutrino self-interaction, the shock effect and the matter effect on the neutrino-process of the core-collapsing supernova (CCSN). For the hydrodynamics, we compare the results of a simple thermal bomb and a specified hydrodynamic model for SN1987A. As a pre-supernova model, we take an updated model adjusted to explain the SN1987A employing recent development of the (n, γ) reaction rates calculated for nuclei near the stability line (A ∼ 100). As for the neutrino luminosity, we adopt two different models: equivalent neutrino luminosity and non-equivalent luminosity models. The latter is taken from the synthetic analysis of the CCSN simulation data which compared quantitatively the results obtained by various neutrino transport models. Relevant neutrino-induced reaction rates are calculated by a shell model for light nuclei and a quasi-particle random phase approximation model for heavy nuclei. For each model, we present and discuss abundances of the light nuclei ( 7 Li, 7 Be, 11 B and 11 C) and heavy nuclei ( 92 Nb, 98 Tc, 138 La and 180 Ta). The light nuclei are known to be sensitive to the Mikheyev-Smirnov-Wolfenstein region around O-Ne-Mg region. Through the detailed analysis of the numerical abundances, we find that neutrino self-interaction becomes a key ingredient in addition to the MSW effect for understanding the neutrino-process and the relevant nuclear abundances. However, the whole results are shown to depend on the adopted neutrino luminosity scheme. Detailed analyses of the nuclear abundances for the two possible neutrino mass hierarchies are also performed with the data from the meteorite analyses. The normal mass hierarchy is shown to be more compatible with the meteoritic data.

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“…The neutrino interactions include charged-(CC) and neutral-current (NC) reactions. Although the neutrino interactions with nuclei are usually negligible, the ν process can contribute entirely or to a significant portion of the production of a handful of rare isotopes including 7 Li, 11 B, 15 N, 19 F, 92 Nb, 98 Tc, 138 La and 180 Ta, as well as two radioisotopes 22 Na and 26 Al (Woosley et al 1990;Heger et al 2005;Byelikov et al 2007;Yoshida et al 2004Yoshida et al , 2005Yoshida et al , 2006aByelikov et al 2007;Yoshida et al 2008;Hayakawa et al 2008Hayakawa et al , 2010Nakamura et al 2010;Austin et al 2011;Cheoun et al 2012;Suzuki and Kajino 2013;Rauscher et al 2013;Hayakawa et al 2013;Lahkar et al 2017;Sieverding et al 2018;Hayakawa et al 2018;Olive and Vangioni 2019;Malatji et al 2019;Kusakabe et al 2019;Li and Li 2022;.…”

Section: ν-Process Nucleosynthesis and Neutrinosmentioning

confidence: 99%

“…The heavy ν-process isotopes are mainly created though CC reactions. For example, stellar evolution studies Heger et al (2005) found that the rare odd-odd nuclides 138 La and 180 Ta are mainly created by the CC reactions 138 Ba(ν e , e − ) 138 La and 180 Hf(ν e , e − ) 180 Ta, thus 138 La and 180 Ta could serve as a constraint for ν e spectra and luminosities (Hayakawa et al 2008;Byelikov et al 2007;Rauscher et al 2013;Kheswa et al 2015;Lahkar et al 2017). Additionally, the main neutrino reactions to produce 92 Nb are the charged-current 92 Zr(ν e , e − ) 92 Nb and the neutral-current 93 Nb(ν(ν ′ ),ν ′ (ν)n) 92 Nb reactions, and similarly the main reactions producing 98 Tc are 98 Mo(ν e , e − ) 98 Tc and 99 Ru(ν(ν ′ ),ν ′ (ν)p) 98 Tc (Hayakawa et al 2013(Hayakawa et al , 2018Cheoun et al 2012).…”

Section: ν-Process Nucleosynthesis and Neutrinosmentioning

confidence: 99%

Neutrinos and Heavy Element Nucleosynthesis

Wang

Surman

2022

Handbook of Nuclear Physics

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This chapter discusses three nucleosynthesis processes involved in producing heavy nuclei beyond the iron group that are influenced or shaped by neutrino interactions: the ν process, the ν p process and the r process. These processes are all related to explosive events involving compact objects, such as core-collapse supernovae and binary neutron star mergers, where an abundant amount of neutrinos are emitted. The interactions of the neutrinos with nucleons and nuclei through both charged-current and neutral-current reactions play a crucial role in the nucleosynthesis processes. During the propagation of neutrinos inside the nucleosynthesis sites, neutrinos may undergo flavor oscillations that can also potentially affect the nucleosynthesis yields. Here we provide a general overview of the possible effects of neutrinos and neutrino flavor conversions on these three heavy-element nucleosynthesis processes. Heavy element nucleosynthesisThe seminal work of Burbidge et al. (1957) identified three main nucleosynthesis processes responsible for the synthesis of elements heavier than iron: the slow (s) and rapid (r) neutron capture processes and the proton-rich (p) process. Since this time, our understanding has evolved and new nucleosynthesis processes have been discovered, (

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Abundances of La138 and Ta180 Through ν-Nucleosynthesis in 20M ⊙ Type II Supernova Progenitor, Guided by Stellar Models for Seeds

Cited by 8 publications

References 14 publications

The Role of the Hadron-Quark Phase Transition in Core-Collapse Supernovae

The Role of the Hadron-Quark Phase Transition in Core-Collapse Supernovae

Comprehensive Analyses of the Neutrino-Process in the Core-collapsing Supernova

Neutrinos and Heavy Element Nucleosynthesis

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