WEAK INTERACTION RATES OF sd-SHELL NUCLEI IN STELLAR ENVIRONMENTS CALCULATED IN THE PROTON–NEUTRON QUASIPARTICLE RANDOM-PHASE APPROXIMATION

Nabi, Jameel‐Un; Klapdor‐Kleingrothaus, H. V.

doi:10.1006/adnd.1998.0801

Cited by 108 publications

(70 citation statements)

References 87 publications

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“…Similar physics include for example the choice of electron capture rates for iron-peak elements [15]. But we have also included the capture rate for isotopes not presented in [15] but shown in [16]. The nuclear network for hydrodynamics is also similar, where we use a 7-isotope network, compared to their 5-isotope network.…”

Section: Resultsmentioning

confidence: 99%

“…We use the Helmholtz equation of states, which contains contributions from ideal electron gas of arbitrarily relativistic and degenerate levels, blackbody photon gas, ions with Coulomb interactions and positron-electron annihilation pairs [4]. To describe the nuclear reactions, we use a 7-isotope network coupled with the simulations, including 4 He, 12 C, 16 O, 20 Ne, 24 Mg, 28 Si and 56 Ni [5]. We use the turbulent deflagration model [6] with delayed detonation transition [7].…”

Section: Methodsmentioning

confidence: 99%

“…The nuclear reaction rates are taken from [13] and [14]. Weak interaction rates of iron-peaked elements are obtained from [15], whereas other isotopes are obtained from [16]. We perform a parameter survey to study the influences of model parameters based on a benchmark model, which satisfies three criteria: 1.…”

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confidence: 99%

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Nucleosynthesis of Iron-Peak Elements in Type-Ia Supernovae

Leung¹,

Nomoto²

2017

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

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The observed features of typical Type Ia supernovae are well-modeled as the explosions of carbonoxygen white dwarfs both near Chandrasekhar mass and sub-Chandrasekhar mass. However, observations in the last decade have shown that Type Ia supernovae exhibit a wide diversity, which implies models for wider range of parameters are necessary. Based on the hydrodynamics code we developed, we carry out a parameter study of Chandrasekhar mass models for Type Ia supernovae. We conduct a series of two-dimensional hydrodynamics simulations of the explosion phase using the turbulent flame model with the deflagration-detonation-transition (DDT). To reconstruct the nucleosynthesis history, we use the particle tracer scheme. We examine the role of model parameters by examining their influences on the final product of nucleosynthesis. The parameters include the initial density, metallicity, initial flame structure, detonation criteria and so on. We show that the observed chemical evolution of galaxies can help constrain these model parameters. KEYWORDS:Type Ia supernovae, hydrodynamics, nucleosynthesis MethodWe carry out two-dimensional hydrodynamics simulations [1] by solving the Euler equations in cylindrical coordinates. The spatial and temporal discretization are calculated by the fifth-order weighted essentially non-oscillatory (WENO) scheme [2] and the five-step third-order non-strong stability preserving Runge-Kutta scheme [3]. We use the Helmholtz equation of states, which contains contributions from ideal electron gas of arbitrarily relativistic and degenerate levels, blackbody photon gas, ions with Coulomb interactions and positron-electron annihilation pairs [4]. To describe the nuclear reactions, we use a 7-isotope network coupled with the simulations, including 4 He, 12 C, 16 O, 20 Ne, 24 Mg, 28 Si and 56 Ni [5]. We use the turbulent deflagration model [6] with delayed detonation transition [7]. The flame and detonation are described by the level-set scheme [8]. The laminar flame and detonation speed are taken from [9] and calculated using the scheme in [10]. The energy production by the explosion follows the three-step scheme as in [11], which includes carbon burning, nuclear quasi-statistical equilibrium (NQSE) burning and NSE burning. In NSE burning, electron capture is included.To calculate the detailed nucleosynthesis, we use the torch nuclear reaction subroutine which consists of 495 isotopes from 1 H to 91 Tc [12]. The nuclear reaction rates are taken from [13] and [14]. Weak interaction rates of iron-peaked elements are obtained from [15], whereas other isotopes are obtained from [16]. We perform a parameter survey to study the influences of model parameters based on a benchmark model, which satisfies three criteria: 1. Healthy 56 Ni production about 0.6 solar mass; 2. Consistency of the 55 Mn to the galactic chemical evolution; 3. Agreement of 58 Ni with the solar abundance.

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Section: Resultsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

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Nucleosynthesis of Iron-Peak Elements in Type-Ia Supernovae

Leung¹,

Nomoto²

2017

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

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“…For the detailed model formalism, we refer to Ref. [16]. The Hamiltonian of the pn-QRPA model is given by…”

Section: Model Description and Formalismmentioning

confidence: 99%

Gamma ray heating rates due to chromium isotopes in stellar core during late stages of high mass stars (>10M_⊙)

Nabi

Fayaz

2017

EPJ Web Conf.

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Abstract. Gamma ray heating rates are thought to play a crucial role during the pre-supernova stage of high mass stars. Gamma ray heating rates, due to β ± -decay and electron (positron) capture on chromium isotopes, are calculated using proton-neutron quasiparticle random phase approximation theory. The electron capture significantly affects the lepton fraction (Y e ) and accelerates the core contraction. The gamma rays emitted as a result of weak processes heat the core and tend to hinder the cooling and contraction due to electron capture and neutrino emission. The emitted gamma rays tend to produce enormous entropy and set the convection to play its role at this stage. The gamma heating rates, on 50-60 Cr, are calculated for the density range 10 ˂ ρ (g.cm -3 ) ˂ 10 11 and temperature range 10 7 ˂ T (K) ˂ 3.0×10 10 .

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“…While the energy loss rate as well as the decrease of the electron fraction because of weak processes were extensively studied in the past (Fuller et al 1980(Fuller et al , 1982aOda et al 1994;Aufderheide et al 1994a,b;Caurier et al 1999;Langanke & Martínez-Pinedo 2000;Nabi & Klapdor-Kleingrothaus 1999;Seitenzahl et al 2009;Juodagalvis et al 2010, and references therein), relatively little is known about the combined energy spectrum of these neutrinos (Langanke et al 2001;Odrzywolek 2009). Typically, the spectrum is integrated in advance and the results are tabulated.…”

Section: Weak Nuclear Processesmentioning

confidence: 99%

Probing thermonuclear supernova explosions with neutrinos

Odrzywołek¹,

Plewa²

2011

A&A

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Aims. We present neutrino light curves and energy spectra for two representative type Ia supernova explosion models: a pure deflagration and a delayed detonation. Methods. We calculate the neutrino flux from β processes using nuclear statistical equilibrium abundances convoluted with approximate neutrino spectra of the individual nuclei and the thermal neutrino spectrum (pair+plasma). Results. Although the two considered thermonuclear supernova explosion scenarios are expected to produce almost identical electromagnetic output, their neutrino signatures appear vastly different, which allows an unambiguous identification of the explosion mechanism: a pure deflagration produces a single peak in the neutrino light curve, while the addition of the second maximum characterizes a delayed-detonation. We identified the following main contributors to the neutrino signal: (1) weak electron neutrino emission from electron captures (in particular on the protons 55 Co and 56 Ni) and numerous β-active nuclei produced by the thermonuclear flame and/or detonation front, (2) electron antineutrinos from positron captures on neutrons, and (3) the thermal emission from pair annihilation. We estimate that a pure deflagration supernova explosion at a distance of 1 kpc would trigger about 14 events in the future 50 kt liquid scintillator detector and some 19 events in a 0.5 Mt water Cherenkov-type detector. Conclusions. While in contrast to core-collapse supernovae neutrinos carry only a very small fraction of the energy produced in the thermonuclear supernova explosion, the SN Ia neutrino signal provides information that allows us to unambiguously distinguish between different possible explosion scenarios. These studies will become feasible with the next generation of proposed neutrino observatories.

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WEAK INTERACTION RATES OF sd-SHELL NUCLEI IN STELLAR ENVIRONMENTS CALCULATED IN THE PROTON–NEUTRON QUASIPARTICLE RANDOM-PHASE APPROXIMATION

Cited by 108 publications

References 87 publications

Nucleosynthesis of Iron-Peak Elements in Type-Ia Supernovae

Nucleosynthesis of Iron-Peak Elements in Type-Ia Supernovae

Gamma ray heating rates due to chromium isotopes in stellar core during late stages of high mass stars (>10M_⊙)

Probing thermonuclear supernova explosions with neutrinos

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WEAK INTERACTION RATES OF sd-SHELL NUCLEI IN STELLAR ENVIRONMENTS CALCULATED IN THE PROTON–NEUTRON QUASIPARTICLE RANDOM-PHASE APPROXIMATION

Cited by 108 publications

References 87 publications

Nucleosynthesis of Iron-Peak Elements in Type-Ia Supernovae

Nucleosynthesis of Iron-Peak Elements in Type-Ia Supernovae

Gamma ray heating rates due to chromium isotopes in stellar core during late stages of high mass stars (>10M⊙)

Probing thermonuclear supernova explosions with neutrinos

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Gamma ray heating rates due to chromium isotopes in stellar core during late stages of high mass stars (>10M_⊙)