scholarly journals Sampling the fermi distribution for {beta}-decay energy input to EGS4

1992 ◽  
Author(s):  
W.R. Nelson ◽  
J. Liu
Keyword(s):  
Beta Decay ◽  
Energy Input ◽  
Decay Energy ◽  
Fermi Distribution

scholarly journals Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

2020 ◽  
Vol 641 ◽  
pp. L10
Author(s):  
Takashi J. Moriya ◽  
Pablo Marchant ◽  
Sergei I. Blinnikov
Keyword(s):  
Light Curve ◽  
Energy Input ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Core Collapse ◽  
Decay Energy ◽  
Slow Cooling ◽  
Gamma Ray Burst ◽  
The Core ◽  
Optical Light Curve

We show that the luminous supernovae associated with ultra-long gamma-ray bursts can be related to the slow cooling from the explosions of hydrogen-free progenitors that are extended by pulsational pair-instability. We have recently shown that some rapidly-rotating hydrogen-free gamma-ray burst progenitors that experience pulsational pair-instability can keep an extended structure caused by pulsational pair-instability until the core collapse. These types of progenitors have large radii exceeding 10 R⊙ and they sometimes reach beyond 1000 R⊙ at the time of the core collapse. They are, therefore, promising progenitors of ultra-long gamma-ray bursts. Here, we perform light-curve modeling of the explosions of one extended hydrogen-free progenitor with a radius of 1962 R⊙. The progenitor mass is 50 M⊙ and 5 M⊙ exists in the extended envelope. We use the one-dimensional radiation hydrodynamics code STELLA in which the explosions are initiated artificially by setting given explosion energy and 56Ni mass. Thanks to the large progenitor radius, the ejecta experience slow cooling after the shock breakout and they become rapidly evolving (≲10 days), luminous (≳1043 erg s−1) supernovae in the optical even without energy input from the 56Ni nuclear decay when the explosion energy is more than 1052 erg. The 56Ni decay energy input can affect the light curves after the optical light-curve peak and make the light-curve decay slowly when the 56Ni mass is around 1 M⊙. They also have a fast photospheric velocity above 10 000 km s−1 and a hot photospheric temperature above 10 000 K at around the peak luminosity. We find that the rapid rise and luminous peak found in the optical light curve of SN 2011kl, which is associated with the ultra-long gamma-ray burst GRB 111209A, can be explained as the cooling phase of the extended progenitor. The subsequent slow light-curve decline can be related to the 56Ni decay energy input. The ultra-long gamma-ray burst progenitors we proposed recently can explain both the ultra-long gamma-ray burst duration and the accompanying supernova properties. When the gamma-ray burst jet is off-axis or choked, the luminous supernovae could be observed as fast blue optical transients without accompanying gamma-ray bursts.

Beta-decay energy and atomic mass of148Tb

1995 ◽  
Vol 352 (1) ◽  
pp. 1-2 ◽  
Author(s):  
H. Keller ◽  
R. Kirchner ◽  
B. Rubio ◽  
J. L. Tain ◽  
Th. D�rfler ◽  
...  
Keyword(s):  
Beta Decay ◽  
Atomic Mass ◽  
Decay Energy

Beta Decay Energy of Tritium

1959 ◽  
Vol 115 (2) ◽  
pp. 450-453 ◽  
Author(s):  
Fred T. Porter
Keyword(s):  
Beta Decay ◽  
Decay Energy

Beta decay of 187W

1970 ◽  
Vol 48 (9) ◽  
pp. 1040-1054 ◽  
Author(s):  
A. W. Herman ◽  
E. A. Heighway ◽  
J. D. MacArthur
Keyword(s):  
Excited State ◽  
Beta Decay ◽  
Decay Scheme ◽  
Decay Energy ◽  
Beta Transition ◽  
Point Energy ◽  
Absolute Intensities ◽  
Gamma Coincidence ◽  
First Excited State ◽  
Coincidence Measurements

Coincidence studies have established in the decay scheme of,187W the existence of transitions of energy 7, 36, 77, 455, 589, and 639 keV with intensities of 3.0 ± 0.5%, 0.50 ± 0.06%, 0.31 ± 0.07%, 0.05 ± 0.02%, 0.14 ± 0.04%, and 0.05 ± 0.02% respectively as well as yielding the absolute intensities of the well-known transitions in 187Re. In addition the beta–gamma coincidence measurements have shown that (1) a first-forbidden unique transition feeds the first-excited state of 187Re, (2) there is at most a very weak beta transition to the level at 512 keV, (3) there is no inner beta group of about 300 keV end-point energy and intensity 8% as indicated by several earlier investigations, and (4) the decay energy of 187W to 187Re is 1311 ± 2 keV. The relevance of these observations to the structure of 187Re is discussed.

scholarly journals New Formula for Negative Beta Decay Energy in the range

2020 ◽  
Vol 29 (4) ◽  
pp. 53-65
Author(s):  
Aws Qasim ◽  
Firas Al-jomaily
Keyword(s):  
Beta Decay ◽  
Decay Energy ◽  
New Formula

Beta-decay strength measurement, total beta-decay energy determination, and dcay-scheme completeness testing by total absorption γ-ray spectroscopy

2004 ◽  
Vol 67 (10) ◽  
pp. 1876-1883 ◽  
Author(s):  
I. N. Izosimov ◽  
A. A. Kazimov ◽  
V. G. Kalinnikov ◽  
A. A. Solnyshkin ◽  
J. Suhonen
Keyword(s):  
Beta Decay ◽  
Total Absorption ◽  
Decay Energy ◽  
Strength Measurement ◽  
Γ Ray ◽  
Energy Determination ◽  
Total Beta

Beta-decay energy measurements using total gamma-absorption spectroscopy

1993 ◽  
Vol 344 (4) ◽  
pp. 425-429 ◽  
Author(s):  
G. D. Alkhazov ◽  
L. H. Batist ◽  
A. A. Bykov ◽  
F. V. Moroz ◽  
S. Yu. Orlov ◽  
...  
Keyword(s):  
Beta Decay ◽  
Absorption Spectroscopy ◽  
Decay Energy ◽  
Gamma Absorption

Beta-decay energy and nuclear mass of100Nb

1983 ◽  
Vol 313 (3) ◽  
pp. 251-252 ◽  
Author(s):  
U. Keyser ◽  
F. M�nnich ◽  
B. Pahlmann ◽  
B. Pfeiffer ◽  
H. Weikard
Keyword(s):  
Beta Decay ◽  
Decay Energy ◽  
Nuclear Mass
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