Theoretical Treatment of the Asymptotic Behavior of Fission Product Decay Heat toward Very Short Cooling-Time.

Yoshida, Tadashi; Tachibana, Takeshi

doi:10.3327/jnst.37.491

Cited by 5 publications

(7 citation statements)

References 16 publications

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“…for k = EC, PC and 2001)), ODA (blue, Oda et al (1994)), FFN (green, Fuller et al (1985)), TACHI tables (yellow, Tachibana & Yamada (1995); Yoshida & Tachibana (2000); Tachibana (2000); Koura et al (2003); Koura (2004); Koura et al (2005)) as well as by the approximate formula (yellow, eq. ( 22)).…”

Section: Nuclear Weak Interactionsmentioning

confidence: 99%

“…Figure 4. Nuclear charts indicating in different colors the nuclear species with the reaction rates for EC (left) and β − decay (right) given in the LMSH (black, Langanke et al (2003)), LMP (red, Langanke et al (2001)), ODA (blue,Oda et al (1994)), FFN (green,Fuller et al (1985)), TACHI tables (yellow,Tachibana & Yamada (1995);Yoshida & Tachibana (2000);Tachibana (2000);Koura et al (2003);Koura (2004);Koura et al (2005)) as well as by the approximate formula (yellow, eq. (22)).…”

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confidence: 99%

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

Kato

Nagakura

Furusawa

et al. 2017

ApJ

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This paper is a sequel to our 2015 paper, Kato et al., which calculated the luminosities and spectra of electron-type anti-neutrinos ( e n ) from the progenitors of core-collapse supernovae. Expecting that the capability to detect electron-type neutrinos ( e n ) 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 57 s -1 and ∼10 53 s -1 at maximum for e n and e n , 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 e n from the ECSN progenitor will be undetected at almost all detectors, whereas we will be able to observe 15,900 e n at DUNE for the inverted mass hierarchy. From the FeCCSN progenitors, the number of e n events will be largest for JUNO, 200-900 e n , depending on the mass hierarchy, whereas the number of e n events at DUNE is 2100  for the inverted mass hierarchy. These results imply that the detection of e n is useful to distinguish progenitors of FeCCSNe from those of ECSNe, while e n will provide us with detailed information on the collapse phase regardless of the type and mass of the progenitor.

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Section: Nuclear Weak Interactionsmentioning

confidence: 99%

mentioning

confidence: 99%

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

Kato

Nagakura

Furusawa

et al. 2017

ApJ

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“…The applicability of this theory in this field is seen, for example, in Ref. 14). We find that this theory gives a good agreement for the calculation of not only the -decay half-lives but also the E and E values on average in the wide nuclear region.…”

Section: Application Of the Gross Theory Of Beta Decaymentioning

confidence: 53%

“…More detailed information on the model of this theory, especially on its application to the decay heat calculation, has been presented in our previous papers. 8,13,14) The total -decay constant is obtained as…”

Section: Application Of the Gross Theory Of Beta Decaymentioning

confidence: 99%

Reconsideration of the Theoretical Supplementation of Decay Data in Fission Product Decay Heat Summation Calculations (II)

Hagura¹,

Tachibana²,

Yoshida³

2010

J. Nucl. Sci. Technol.

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In our previous paper, the theoretical overcorrection in JENDL FP Decay Data File 2000 for the decay heat summation calculation was suggested. In order to eliminate this, we redefined the criteria of applying the theoretical values to average energy release per decay, that is, E and E values. Furthermore, the results of the TAGS (total absorption gamma ray spectrometer) measurements up to the newest ones are adopted into the decay heat calculations. As a result, we obtained a reasonable agreement between the calculation and the sample irradiation experiments, not only for 239 Pu but for 233;235;238 U and 241 Pu. The present revision of the FP decay data file will provide us with a reasonable starting point for the future revision of the decay data file by introducing the results from the TAGS effort now in progress. In addition, the effects of the so-called pandemonium problem are clearly demonstrated and this also affects the conventional decay schemes, especially for the short-lived FP nuclides having large -decay Qvalues.

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“…We have been developing several theoretical models to apply them to nuclear decay data. Gross theory [13][14][15] is one of our powerful approaches. This model gives a reasonable agreement with experimental data in half-lives, delayed neutron branching ratios, and average β and γ emission energies in a wide range of nuclei.…”

Section: Theoretical Model Applicationsmentioning

confidence: 99%

Toward next JENDL Fission Yield Data and Decay Data

Minato

2020

EPJ Web Conf.

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Theoretical Treatment of the Asymptotic Behavior of Fission Product Decay Heat toward Very Short Cooling-Time.

Cited by 5 publications

References 16 publications

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

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

Reconsideration of the Theoretical Supplementation of Decay Data in Fission Product Decay Heat Summation Calculations (II)

Toward next JENDL Fission Yield Data and Decay Data

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