Engineering topics

Yoshida, Takashi

Publications and source records attributed to Yoshida, Takashi.

16 records

DOE OSTI2021

Three-flavor collective neutrino conversions with multi-azimuthal-angle instability in an electron-capture supernova model

We investigate the multi-azimuthal angle (MAA) effect on collective neutrino oscillation by considering the three-dimensional neutrino momentum distribution in a realistic electron-capture supernova model with an 8.8 M ⊙ progenitor. We find that the MAA effect induces collective flavor conversions at epochs when it is completely suppressed under the axial-symmetric approximation. This novel activity is switched on/off by the growth of the MAA instability and imprints additional time evolution in the expected neutrino event rate. We validate our results by extending the linear stability analysis into the three-flavor scheme including mixing angles, and confirm that the onset of collective neutrino oscillation matches the steep growth of flavor instability. Furthermore, we discuss how the MAA effect alters neutrino detection at Super-Kamiokande and DUNE.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗

DOE OSTI2020

Neutrino halo effect on collective neutrino oscillation in iron core-collapse supernova model of a 9.6 M ⊙ star

We extend the multi-angle computational framework and investigate the time evolution of the neutrino halo on collective neutrino oscillation in the core collapse of an iron core progenitor. We find that in the case of the 9.6 M progenitor adopted in this work, there are windows of time when the effects of neutrino halo and collective neutrino oscillation are not simultaneously large. Inside the shock, the impact of the inward-scattered halo neutrino cannot in general be neglected compared to the outward-propagating neutrino flux. However, during early epochs, collective neutrino oscillation is effectively shut down by multi-angle matter suppression. During the intermediate epoch, collective neutrino oscillation is not suppressed, but its onset radius is beyond the still relatively small explosion shock front where the halo is prominent. We also find in the case of the 9.6 M progenitor the halo neutrinos induce a delay in the onset of collective neutrino oscillations. This causes novel flavor conversions which sharpen collective neutrino oscillation spectral features. We predict that the inclusion of neutrino halo effects makes neutrino signals that are more clearly distinct from thermal emission that when halo neutrinos are omitted.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2018

Minimum Information about an Uncultivated Virus Genome (MIUViG)

We present an extension of the Minimum Information about any (x) Sequence (MIxS) standard for reporting sequences of uncultivated virus genomes. Minimum Information about an Uncultivated Virus Genome (MIUViG) standards were developed within the Genomic Standards Consortium framework and include virus origin, genome quality, genome annotation, taxonomic classification, biogeographic distribution and in silico host prediction. Community-wide adoption of MIUViG standards, which complement the Minimum Information about a Single Amplified Genome (MISAG) and Metagenome-Assembled Genome (MIMAG) standards for uncultivated bacteria and archaea, will improve the reporting of uncultivated virus genomes in public databases. In turn, this should enable more robust comparative studies and a systematic exploration of the global virosphere.

59 BASIC BIOLOGICAL SCIENCES↗

DOE OSTI2017

Neutrino Emissions in All Flavors up to the Pre-bounce of Massive Stars and the Possibility of Their Detections

This paper is a sequel to our 2015 paper, Kato et al., which calculated the luminosities and spectra of electron-type anti-neutrinos ( ν-bar {sub e}) from the progenitors of core-collapse supernovae. Expecting that the capability to detect electron-type neutrinos (ν{sub e}) will increase dramatically with the emergence of liquid-argon detectors such as DUNE, we broaden the scope in this study to include all flavors of neutrinos emitted from the pre-bounce phase. We pick up three progenitor models of electron capture supernovae (ECSNe) and iron-core collapse supernovae (FeCCSNe). We find that the number luminosities reach ∼10{sup 57} s{sup –1} and ∼10{sup 53} s{sup –1 }at maximum for ν{sub e} and ν-bar {sub e}, respectively. We also estimate the numbers of detection events at terrestrial neutrino detectors including DUNE, taking flavor oscillations into account and assuming the distance to the progenitors to be 200 pc. It is demonstrated that ν-bar {sub e} from the ECSN progenitor will be undetected at almost all detectors, whereas we will be able to observe ≳15,900 ν{sub e} at DUNE for the inverted mass hierarchy. From the FeCCSN progenitors, the number of ν-bar {sub e} events will be largest for JUNO, 200–900 ν-bar {sub e}, depending on the mass hierarchy, whereas the number of ν{sub e} events at DUNE is ≳2100 for the inverted mass hierarchy. These results imply that the detection of ν-bar {sub e} is useful to distinguish progenitors of FeCCSNe from those of ECSNe, while ν{sub e} will provide us with detailed information on the collapse phase regardless of the type and mass of the progenitor.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2016

Alpha-constrained QSE nucleosynthesis in high-entropy and fast-expanding material

We investigate the nucleosynthesis process in high-entropy (s/k{sub B}≳100) and very fast expanding (τ{sub exp}∼10{sup −3} s) materials. In such a material with the electron fraction near 0.5, an interesting nucleosynthesis process occurs. In this process, the abundance distribution of heavy nuclei of A>100 achieves quasi-statistical equilibrium (QSE) at high temperature and the abundances are frozen at the end of the nucleosynthesis. We explain this abundance distribution using the “alpha-constrained QSE” abundances formulated in this paper. We demonstrate that this nucleosynthesis would occur in neutrino-driven winds from massive proto-neutron stars in hypernovae, where A∼140 p-nuclei are synthesized.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2015

Nucleosynthesis in neutrino-driven winds in hypernovae

We investigate the nucleosynthesis in the neutrino-driven winds blown off from a 3 M{sub ⊙} massive proto-neutron star (mPNS) temporarily formed during the collapse of a 100 M{sub ⊙} star. Such mPNSs would be formed in hypernovae. We construct steady and spherically symmetric wind solutions. We set large neutrino luminosities of ∼10{sup 53} erg s{sup −1} and average energies of electron neutrinos and antineutrinos in the ranges of ϵ{sub ν{sub e}}=9−16 MeV and ϵ{sub ν-bar {sub e}}=11−18 MeV based on a recent numerical relativity simulation. The wind solutions indicate a temperature-decrease timescale much shorter than that of the winds from ordinary PNSs, and, depending on ϵ{sub ν}, the winds can be both neutron-rich and proton-rich. In the neutron-rich wind, the r-process occurs and the abundance distribution of a fiducial wind model of the mPNS gives an approximate agreement with the abundance pattern of metal-poor weak r star HD 122563, although the third-peak elements are produced only when the ν-bar {sub e} energy is much larger than the ν{sub e} energy. In the proton-rich wind, the strong νp-process occurs and A>100 nuclides are synthesized. The synthesized nuclei can be neutron-rich in some cases because the large neutrino luminosity of the mPNS supplies a sufficient amount of neutrons.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2015

Pre-supernova neutrino emissions from ONe cores in the progenitors of core-collapse supernovae: Are they distinguishable from those of Fe cores?

Aiming to distinguish two types of progenitors of core-collapse supernovae, i.e., one with a core composed mainly of oxygen and neon (abbreviated as ONe core) and the other with an iron core (or Fe core), we calculated the luminosities and spectra of neutrinos emitted from these cores prior to gravitational collapse, taking neutrino oscillation into account. We found that the total energies emitted as ν-bar {sub e} from the ONe core are ≲10{sup 46} erg, which is much smaller than ∼10{sup 47} erg for Fe cores. The average energy, on the other hand, is twice as large for the ONe core as those for the Fe cores. The neutrinos produced by the plasmon decays in the ONe core are more numerous than those from the electron–positron annihilation in both cores, but they have much lower average energies ≲1 MeV. Although it is difficult to detect the pre-supernova neutrinos from the ONe core even if it is located within 200 pc from Earth, we expect ∼9–43 and ∼7–61 events for Fe cores at KamLAND and Super-Kamiokande, respectively, depending on the progenitor mass and neutrino-mass hierarchy. These numbers might be increased by an order of magnitude if we envisage next-generation detectors such as JUNO. We will hence be able to distinguish the two types of progenitors by the detection or nondetection of the pre-supernova neutrinos if they are close enough (≲1 kpc).

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2015

The Ocean Sampling Day Consortium

In this study, Ocean Sampling Day was initiated by the EU-funded Micro B3 (Marine Microbial Biodiversity, Bioinformatics, Biotechnology) project to obtain a snapshot of the marine microbial biodiversity and function of the world’s oceans. It is a simultaneous global mega-sequencing campaign aiming to generate the largest standardized microbial data set in a single day. This will be achievable only through the coordinated efforts of an Ocean Sampling Day Consortium, supportive partnerships and networks between sites. This commentary outlines the establishment, function and aims of the Consortium and describes our vision for a sustainable study of marine microbial communities and their embedded functional traits.

54 ENVIRONMENTAL SCIENCES↗

DOE OSTI2014

Stellar yields of rotating first stars. I. Yields of weak supernovae and abundances of carbon-enhanced hyper-metal-poor stars

We perform a stellar evolution simulation of first stars and calculate stellar yields from the first supernovae. The initial masses are taken from 12 to 140 M {sub ☉} to cover the whole range of core-collapse supernova progenitors, and stellar rotation is included, which results in efficient internal mixing. A weak explosion is assumed in supernova yield calculations, thus only outer distributed matter, which is not affected by the explosive nucleosynthesis, is ejected in the models. We show that the initial mass and the rotation affect the explosion yield. All the weak explosion models have abundances of [C/O] larger than unity. Stellar yields from massive progenitors of >40-60 M {sub ☉} show enhancement of Mg and Si. Rotating models yield abundant Na and Al, and Ca is synthesized in nonrotating heavy massive models of >80 M {sub ☉}. We fit the stellar yields to the three most iron-deficient stars and constrain the initial parameters of the mother progenitor stars. The abundance pattern in SMSS 0313–6708 is well explained by 50-80 M {sub ☉} nonrotating models, rotating 30-40 M {sub ☉} models well fit the abundance of HE 0107-5240, and both nonrotating and rotating 15-40 M {sub ☉} models explain HE 1327-2326. The presented analysis will be applicable to other carbon-enhanced hyper-metal-poor stars observed in the future. The abundance analyses will give valuable information about the characteristics of the first stars.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2014

Process metallurgy simulation for metal drawing process optimization by using two-scale finite element method

We developed two-scale FE analysis procedure based on the crystallographic homogenization method by considering the hierarchical structure of poly-crystal aluminium alloy metal. It can be characterized as the combination of two-scale structure, such as the microscopic polycrystal structure and the macroscopic elastic plastic continuum. Micro polycrystal structure can be modeled as a three dimensional representative volume element (RVE). RVE is featured as by 3×3×3 eight-nodes solid finite elements, which has 216 crystal orientations. This FE analysis code can predict the deformation, strain and stress evolutions in the wire drawing processes in the macro- scales, and further the crystal texture and hardening evolutions in the micro-scale. In this study, we analyzed the texture evolution in the wire drawing processes by our two-scale FE analysis code under conditions of various drawing angles of dice. We evaluates the texture evolution in the surface and center regions of the wire cross section, and to clarify the effects of processing conditions on the texture evolution.

75 CONDENSED MATTER PHYSICS, SUPERCONDUCTIVITY AND↗

DOE OSTI2014

Stellar yields of rotating first stars

First stars, also called population III stars, are born in the earliest universe without any heavy elements. These stars are the first nuclear reactor in the universe and affect their circumstances emitting synthesized materials. Not only the stellar evolution, but also their chemical yields have many distinctive characteristics. We have modeled evolution of population III stars including effect of stellar rotation. Internal mixing induced by rotation naturally results in primary nitrogen production. Evolution of rotating massive stars is followed until the core collapse phase. The new Pop III yield model will consistently explain the observed abundances of metal-poor systems.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2014

Evolution and explosion of the most massive asymptotic giant branch star

The most massive asymptotic giant branch (AGB) stars can form a critical mass of ONe core at its center. The collapse of such a critical ONe core may end up as an Electron Capture Supernova (ECSN). We have accomplished a progenitor calculation for ECSN for the first time in more than two decades and have updated a pre-explosion structure for this model. Some details for ONe core formation and important mechanisms for the core contraction are shown. We discuss how the envelope mass loss affects the predicted existence of ECSN, and what physics is needed to model for a plausible structure of ECSN progenitor.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2014

Ultra high-energy neutrinos via heavy-meson synchrotron emission in strong magnetic fields

We explore the generation and possibility for the detection of heavy-meson synchrotron emission due to the acceleration of ultra-relativistic protons (and possibly nuclei) in the presence of strong magnetic fields (H ≳ 10{sup 15} G) in transient astrophysical environments such as magnetar flares. We show that, in addition to the well-known pion synchrotron emission, heavy vector mesons like ρ, D{sub S} , J/Ψ, and Y could be generated. For high enough energies and magnetic field strengths, such heavy vector mesons can be formed with high intensity (∼10{sup 3} times the photon intensity) through strong couplings to the ultra-relativistic nucleons. We examine in particular the synchrotron emission and subsequent cooling and decay of the heavy ρ{sup 0} and Y(1S) mesons, e.g., via p → p' + Y(1S), Y(1S) → τ{sup +} + τ{sup –}, τ{sup −}→μ{sup −}+ ν-bar {sub μ}+ν{sub τ} and e{sup −}+ ν-bar {sub e}+ν{sub τ}. We evaluate the spectra of escaping ν {sub e}, ν{sub μ}, and ν{sub τ} due to the decay of short-lived τ mesons. We deduce the possible event rate in a terrestrial TeV neutrino detector. We estimate that neutrinos produced from the heavy vector-meson synchrotron radiation from a strong magnetar soft gamma repeater burst will only be detectable with the current generation of detectors if the source is very nearby (<30 pc). Nevertheless, if ever detected, the existence of heavy meson synchrotron emission might be identifiable by the unique signature of energetic tau neutrinos emanating from the source.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2013

Cysteine 295 indirectly affects Ni coordination of carbon monoxide dehydrogenase-II C-cluster

Highlights: •CODH-II harbors a unique [Ni-Fe-S] cluster. •We substituted the ligand residues of Cys{sup 295} and His{sup 261}. •Dramatic decreases in Ni content upon substitutions were observed. •All substitutions did not affect Fe-S clusters assembly. •CO oxidation activity was decreased by the substitutions. -- Abstract: A unique [Ni–Fe–S] cluster (C-cluster) constitutes the active center of Ni-containing carbon monoxide dehydrogenases (CODHs). His{sup 261}, which coordinates one of the Fe atoms with Cys{sup 295}, is suggested to be the only residue required for Ni coordination in the C-cluster. To evaluate the role of Cys{sup 295}, we constructed CODH-II variants. Ala substitution for the Cys{sup 295} substitution resulted in the decrease of Ni content and didn’t result in major change of Fe content. In addition, the substitution had no effect on the ability to assemble a full complement of [Fe–S] clusters. This strongly suggests Cys{sup 295} indirectly and His{sup 261} together affect Ni-coordination in the C-cluster.

60 APPLIED LIFE SCIENCES↗

DOE OSTI2013

EVOLUTION OF PROGENITORS FOR ELECTRON CAPTURE SUPERNOVAE

We provide progenitor models for electron capture supernovae (ECSNe) with detailed evolutionary calculation. We include minor electron capture nuclei using a large nuclear reaction network with updated reaction rates. For electron capture, the Coulomb correction of rates is treated and the contribution from neutron-rich isotopes is taken into account in each nuclear statistical equilibrium (NSE) composition. We calculate the evolution of the most massive super asymptotic giant branch stars and show that these stars undergo off-center carbon burning and form ONe cores at the center. These cores become heavier up to the critical mass of 1.367 M{sub Sun} and keep contracting even after the initiation of O+Ne deflagration. Inclusion of minor electron capture nuclei causes convective URCA cooling during the contraction phase, but the effect on the progenitor evolution is small. On the other hand, electron capture by neutron-rich isotopes in the NSE region has a more significant effect. We discuss the uniqueness of the critical core mass for ECSNe and the effect of wind mass loss on the plausibility of our models for ECSN progenitors.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗

DOE OSTI2011

EVOLUTION OF FLUORINE IN THE GALAXY WITH THE {nu}-PROCESS

We calculate the evolution of fluorine in the solar neighborhood with the {nu}-process of core-collapse supernovae, the results of which are in good agreement with the observations of field stars. The {nu}-process operating in supernovae causes the [F/O] ratio to plateau at [O/H] {approx}< - 1.2, followed by a rapid increase toward [O/H] {approx} - 0.5 from the contribution of asymptotic giant branch stars. The plateau value of [F/O] depends on the neutrino luminosity released by core-collapse supernovae and may be constrained by using future observations of field stars at low metallicities. For globular clusters, the handful of [F/O] measurements suggest that the relative contribution from low-mass supernovae is smaller in these systems than in the field.

79 ASTRONOMY AND ASTROPHYSICS↗