Neutrinos and Their Impact on Core-Collapse Supernova Nucleosynthesis

Martı́nez-Pinedo, G.; Fischer, Tobias; Langanke, K.; Lohs, A.; Sieverding, André; Wu, Meng-Ru

doi:10.1007/978-3-319-20794-0_78-1

Cited by 9 publications

(10 citation statements)

References 113 publications

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“…For the two remaining energy levels of a three-qubit Hamiltonian block (recall that two eigenvalues were added arbitrarily to supplement the sixdimensional block), we obtained the eigenstates exactly by exploiting the symmetry of the reduced Hamiltonian block and then constructed quantum circuits generating them which we implemented on quantum hardware to obtain the experimental energy eigenvalues. As it is easily seen from the three-qubit reduced block Hamiltonian in (10), the eigenvalue 2µ is degenerate and the corresponding eigenvectors are 1…”

Section: A Qlanczos Algorithmmentioning

confidence: 99%

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Collective Neutrino Oscillations on a Quantum Computer

Yeter-Aydeniz¹,

Bangar²,

Siopsis³

et al. 2021

Preprint

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We calculate the energy levels of a system of neutrinos undergoing collective oscillations as functions of an effective coupling strength and radial distance from the neutrino source using the quantum Lanczos (QLanczos) algorithm implemented on IBM Q quantum computer hardware. Our calculations are based on the many-body neutrino interaction Hamiltonian introduced in Ref. [1]. We show that the system Hamiltonian can be separated into smaller blocks, which can be represented using fewer qubits than those needed to represent the entire system as one unit, thus reducing the noise in the implementation on quantum hardware. We also calculate transition probabilities of collective neutrino oscillations using a Trotterization method which is simplified before subsequent implementation on hardware. These calculations demonstrate that energy eigenvalues of a collective neutrino system and collective neutrino oscillations can both be computed on quantum hardware with certain simplification to within good agreement with exact results. a *

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Section: A Qlanczos Algorithmmentioning

confidence: 99%

“…For example, in a core-collapse supernova event the energy released is of order ∼ 10 59 MeV and 99% of this energy is carried away by neutrinos and antineutrinos. This large amount of of energy corresponds to ∼ 10 58 neutrinos [10]. Studying interactions between this many neutrinos using classical computers is a daunting task.…”

Section: Introductionmentioning

confidence: 99%

Collective Neutrino Oscillations on a Quantum Computer

Yeter-Aydeniz¹,

Bangar²,

Siopsis³

et al. 2021

Preprint

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“…The 2D subroutine accounting for weak magnetism using 32-grid-point Gauss quadratures for each dimension has been shown to be efficient and stable in symmetric CCSN simulations [33]. 5 The 4D subroutine, on the other hand, could be inefficient. Using less grid points or Monte Carlo points may provide ways to trade-off accuracy for computational efficiency for both subroutines.…”

Section: Subroutines and Tables For Neutrino Absorption On Nucleonsmentioning

confidence: 99%

“…Most of the gravitational binding energy of the neutron star is released in the form of neutrinos that in the neutrino-driven mechanism are responsible for the ejection of the stellar mantle [1]. Consequently, neutrino processes in hot and dense nuclear medium play crucial roles in many aspects of core-collapse supernovae (CC-SNe), in particular for the explosion mechanism and the nucleosynthesis of heavy elements [2][3][4][5]. The successful explosion of core-collapse supernovae by the neutrinodriven mechanism in three-dimensional simulations has demonstrated the high relevance of neutrino physics as well as the necessity of an accurate description of neutrino transport in hot and dense protoneutron star (PNS) [6].…”

Section: Introductionmentioning

confidence: 99%

Charged-Current Muonic Reactions in Core-Collapse Supernovae

Guo,

Martínez-Pinedo,

Lohs

et al. 2020

Preprint

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The steady advance in core-collapse supernova simulations requires a more precise description of neutrino processes in hot and dense matter. In this work, we study the rates of charged-current (CC) weak processes with (anti)muons in supernova matter. At the relativistic mean field level, we derive results for the rates of CC neutrino-nucleon reactions, taking into account full kinematics, weak magnetism and pseudoscalar terms, and q 2 -dependent nucleon form factors in the hadronic current. In addition to muonic semileptonic processes we also consider purely leptonic processes. In particular, we show that inverse muon decay can dominate the opacities for low energy νµ and νe at densities 10 13 g cm −3 .

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“…Neutrino interaction with nucleons in proto-neutron star (PNS) (Burrows et al 2006) plays a crucial role in many aspects of core-collapse supernovae (CCSNe), such as the explosion mechanism (Burrows 2013;Janka et al 2007;Janka 2012) as well as the synthesis of heavy elements in neutrino-driven winds (Arcones & Thielemann 2013;Martínez-Pinedo et al 2016) and the long-term neutron star cooling (Yakovlev et al 2001;Yakovlev & Pethick 2004). Three-dimentional (3D) simulations with detailed neutrino transport have shown that explosions are very sensitive to neutrino opacities even at the level of 10%-20% (Melson et al 2015;Burrows et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Chiral Effective Field Theory Description of Neutrino Nucleon–Nucleon Bremsstrahlung in Supernova Matter

Guo

Martı́nez-Pinedo

2019

ApJ

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We revisit the rates of neutrino pair emission and absorption from nucleon-nucleon Bremsstrahlung in supernova matter using the T -matrix formalism in the long wavelength limit. Based on chiral effective field theory (χEFT) two-body potentials, we solve the Bethe-Goldstone equation accounting for the in-medium T -matrix including non-diagonal contributions. Our calculations consider nucleons with arbitrary degree of degeneracy and hence account for final state Pauli blocking. We compare our results with one pion exchange (OPE) rates, commonly used in supernova simulations, and calculations using an effective on-shell diagonal T -matrix from measured phase shifts. We also estimate that multiscattering processes and RPA correlations introduce small corrections on top of the in-medium T -matrix results at subsaturation densities.

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Neutrinos and Their Impact on Core-Collapse Supernova Nucleosynthesis

Cited by 9 publications

References 113 publications

Collective Neutrino Oscillations on a Quantum Computer

Collective Neutrino Oscillations on a Quantum Computer

Charged-Current Muonic Reactions in Core-Collapse Supernovae

Chiral Effective Field Theory Description of Neutrino Nucleon–Nucleon Bremsstrahlung in Supernova Matter

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