Energy levels of excited in the decay of the isomeric pair and

1968 ◽  
Vol 46 (21) ◽  
pp. 2375-2397 ◽  
Author(s):  
S. Monaro ◽  
J. Barrette ◽  
A. Boutard
Keyword(s):  
Gamma Rays ◽  
Energy Levels ◽  
Correlation Coefficients ◽  
Coincidence Circuit ◽  
Isomeric Pair ◽  
Γ Ray

The γ-ray spectra accompanying the decay of 96gTc (4.3 d) and 96mTc (52 m), produced in the reactions 96Mo (p, n) 96Tc and 97Mo (p, 2n) 96Tc, have been studied with lithium-drifted Ge detectors.Gamma rays (relative intensities are in parentheses) of 314.2 ± 0.2 (2.4), 316.3 ± 0.2 (1.5), 434.8 ± 0.4 (0.8), 460.2 ± 0.4 (0.48), 568.9 ± 0.4 (.95), 778.2 ± 0.2 (100), 812.5 ± 0.2 (83), 849.8 ± 0.2 (98), 1091.3 ± 0.4(0.9), 1126.8 ± 0.3 (15.3), 1200.0 ± 0.4 (0.41), and 1497.7 ± 0.5 keV (0.081), plus several other very weak lines, have been observed in the decay of 96Tc (4.3 d). Several transitions never previously reported were found in the decay of 96mTc (52 m). All but four of these transitions could fit already known excited levels in 96Mo at 778.2, 1497.9, 1628.0, 1869.6, and 1978.3 keV, whereas the placing of the remaining 616.1-, 966.6-, 1096.6-, and 1816.2-keV gamma rays required the existence of a new level in 96Mo at 2594.5 keV.In view of the results obtained from the study of the decay of the 96Tc isomeric pair, it was considered very desirable to reinvestigate the decay of 96Nb to levels in 96Mo. The 96Nb source was produced in the reaction 96Zr (p, n) 96Nb. Ge(Li) detectors were again employed and gamma–gamma directional correlation measurements were performed with two NaI(Tl) crystals, a fast coincidence circuit, and a multiparameter analyzer to record the data.The experimental directional correlation coefficients of the 1200.1–778.2, 1200.1–460.1, 778.2–460.1, 1091.4–778.2, 1091.4–568.7, and 778.2–568.7 keV cascades are[Formula: see text]respectively.These values seem to be compatible with spin assignments of 4+, 3+, and 5+ for the 1869.6-, 1978.3-, and 2438.4-keV levels in 96Mo respectively.

Energy levels of excited in the decay of the 94Tcm,g isomeric pair

1969 ◽  
Vol 47 (9) ◽  
pp. 995-1003 ◽  
Author(s):  
J. Barrette ◽  
A. Boutard ◽  
S. Monaro
Keyword(s):  
Solid State ◽  
Excited States ◽  
Gamma Rays ◽  
Level Scheme ◽  
Coulomb Excitation ◽  
Energy Levels ◽  
Isomeric Pair ◽  
Solid State Detectors ◽  
Γ Ray ◽  
Type Detector

The γ-ray spectra resulting from the decay of the 94Tcm,g isomeric pair to the excited states of 94Mo have been investigated using Ge(Li) solid state detectors. Gamma rays (relative intensities are in parentheses) of 871.05(100); 993.19(2.35); 1196.4(0.80); 1522.1 (4.80); 1868.68(6.10); 2393.2(0.50); 2529.8(0.33); 2740.1(3.74); 3129.1(1.47); 3512.5(0.06); 3793.1(0.05); 3892.7(0.016); plus several other weak lines have been observed in the decay of 94Tcm(52 min). Gamma rays (relative intensities are in parentheses) of 449.2(3.3); 532.1(2.35); 702.67(99.7); 742.3(1.21); 849.74(95.8); 871.05(100); 961.10(7.6); 1509.3(0.68); 1592.1(2.25); 1765.6(0.29) have been detected in the decay of 94Tcg(5 h). To investigate this latter activity a hollow coaxial Ge(Li) spectrometer was also used as a well-type detector in order to obtain sum spectra of coincident gamma rays. The overall results obtained from this study allows construction of a level scheme of 94Mo which compares fairly well with previous investigations and removes some inconsistencies shown in Coulomb excitation measurements.

scholarly journals What do Gamma Rays tell us about the ISM?: New Insight from the Compton Observatory

1996 ◽  
Vol 169 ◽  
pp. 437-446 ◽  
Author(s):  
Hans Bloemen
Keyword(s):  
Interstellar Medium ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Line Emission ◽  
Cosmic Ray ◽  
Gamma Ray Astronomy ◽  
Early Results ◽  
The Galaxy ◽  
Γ Ray ◽  
Insight Into

Gamma-ray astronomy has become a rich field of research and matured significantly since the launch of NASA's Compton Gamma Ray Observatory in April 1991. Studies of the diffuse γ-ray emission of the Galaxy can now be performed in far more detail and extended into the MeV regime, including both continuum and line emission. These studies provide unique insight into various aspects of the interstellar medium, in particular of the cosmic-ray component. This paper gives a brief review on the diffuse Galactic γ-ray emission and summarizes early results and prospects from the Compton Observatory.

scholarly journals The Flare of 1989 September 9, 09:09 UT: Does Coronal Loop Collision Initiate Efficient Gamma-Ray Emission?

1994 ◽  
Vol 142 ◽  
pp. 707-711
Author(s):  
H. Aurass ◽  
A. Hofmann ◽  
E. Rieger
Keyword(s):  
Current Sheet ◽  
Gamma Rays ◽  
Coronal Loop ◽  
Gamma Ray ◽  
High Energy ◽  
X Rays ◽  
Subject Headings ◽  
Γ Ray ◽  
Gamma Ray Emission ◽  
Magnetogram Data

AbstractVector magnetogram data and Hα pictures together with data published by Chupp et al. lead us to conjecture that in the presented case a contact between the rising two-ribbon flare current sheet and a coronal loop connecting two nearby plage regions initiates efficient high-energy γ-ray emission.Subject headings: Sun: corona — Sun: flares — Sun: X-rays, gamma rays

Gamma rays and high-energy neutrons in the atmosphere

1968 ◽  
Vol 46 (10) ◽  
pp. S1030-S1033 ◽  
Author(s):  
M. V. K. Apparao ◽  
R. R. Daniel ◽  
George Joseph ◽  
G. S. Gokhale ◽  
P. J. Lavakare ◽  
...  
Keyword(s):  
Gamma Rays ◽  
Counting Rate ◽  
Plastic Scintillator ◽  
Pulse Height ◽  
Growth Curves ◽  
High Energy ◽  
Cutoff Rigidity ◽  
Energy Formula ◽  
Γ Rays ◽  
Γ Ray

In continuation of our earlier experiments studying the emission of solar neutrons, we have now developed detector systems which respond to γ rays of energy 1–5 MeV and neutrons of energy [Formula: see text]. The two detectors are almost identical. Each consists of a CsI (Na) crystal (B) of diameter 3.8 cm, completely enclosed in a tapered cylinder of plastic scintillator (A) operated in anticoincidence; the crystals have thicknesses of 2.4 and 1.2 cm respectively. A balloon carrying these detectors was flown on March 16, 1967 over Hyderabad, India (vertical cutoff rigidity 16.9 GV) and floated at a ceiling altitude of 6.0 mb for 1 hour. In addition to γ-ray and neutron events (AB), events A and AB were also continuously monitored throughout the flight. Pulses corresponding to 1–5 MeV in the 2.4-cm crystal (γ rays) and 6–40 MeV in the 1.2-cm crystal (high-energy neutrons) were analyzed by a 64-channel pulse-height analyzer. On the basis of the pulse-height distributions and γ-ray efficiencies in the two crystals, we attribute events of 1–5 MeV energy from the thicker crystal to γ rays and those > 10 MeV in energy from the thinner one to stars produced by high-energy neutrons [Formula: see text] in the crystal. Atmospheric growth curves for γ rays and neutrons have been obtained; these growth curves as well as those for events A and AB show the normal features of the Pfotzer maximum, steady decreases up to the ceiling altitude, and a constant counting rate at ceiling. The atmospheric counting rates at ceiling altitude give for γ rays of energy 1–5 MeV a flux of ~1 photon per cm2 s and for neutrons of energy [Formula: see text] a flux of ~0.1 neutron per cm2 s. No evidence for a solar component in either channel was found.

Using a clinical linac to determine the energies of gamma-ray transitions and half-lives of barium nuclei

2020 ◽  
Vol 35 (10) ◽  
pp. 2050062
Author(s):  
Abdullah Engin Çalık ◽  
Kaan Manisa ◽  
Ahmet Biçer ◽  
Mehmet Erdoğan ◽  
Mürsel Şen ◽  
...  
Keyword(s):  
Gamma Rays ◽  
Linear Accelerator ◽  
Nuclear Physics ◽  
Hpge Detector ◽  
Gamma Ray ◽  
Energy Levels ◽  
Photonuclear Reactions ◽  
High Purity Germanium ◽  
Physics Experiment ◽  
First Time

Photonuclear reactions have great importance in understanding the structure of the nuclei. These reactions, performed using the gamma rays obtained by way of bremsstrahlung, are a standard nuclear physics experiment. In this study, a non-enriched barium sample was activated for the first time by using a clinical linear accelerator (cLINACs). The spectrum of barium radioisotopes was obtained by using a gamma spectrometry with a high purity germanium (HPGe) detector. The obtained spectroscopic data were analyzed and energy levels and half-life values together with their uncertainties were obtained. Some energy levels and half-lives of [Formula: see text]Ba were determined with more precision than those of literature values.

scholarly journals Gamma Rays from Cosmic Rays

1981 ◽  
Vol 94 ◽  
pp. 309-319 ◽  
Author(s):  
A. W. Wolfendale
Keyword(s):  
Cosmic Rays ◽  
Gamma Rays ◽  
Molecular Clouds ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Cosmic Ray Interactions ◽  
The Galaxy ◽  
Γ Rays ◽  
Γ Ray

It is shown that there is evidence favouring molecular clouds being sources of γ-rays, the fluxes being consistent with expectation for ambient cosmic rays interacting with the gas in the clouds for the clouds considered. An estimate is made of the fraction of the apparently diffuse γ-ray flux which comes from cosmic ray interactions in the I.S.M. as distinct from unresolved discrete sources. Finally, an examination is made of the possibility of gradients of cosmic ray intensity in the Galaxy.

scholarly journals Gamma rays from violent interstellar events

1989 ◽  
Vol 120 ◽  
pp. 494-499
Author(s):  
J.B.G.M. Bloemen
Keyword(s):  
Gamma Rays ◽  
High Velocity ◽  
Galactic Disk ◽  
Cosmic Ray ◽  
Point Sources ◽  
Prominent Feature ◽  
Hii Region ◽  
Ray Density ◽  
Γ Ray ◽  
High Velocity Clouds

SummaryAs an illustration of what the next generation of γ-ray telescopes may show us, an up-to-date COS-B ‘finding chart’ of potential γ-ray point sources and unexplained extended γ-ray features is presented. The latter, in particular, may be related to energetic phenomena in the interstellar medium, capable of enhancing the local cosmic-ray density. As an example, a prominent feature, extending over at least 10° — 15° almost perpendicular to the Galactic disk, is discussed in some detail, linking it to the giant HII region S54 and Complex C of high-velocity clouds.

The 12 C(γ, 3α) reaction energy levels of 8 Be and 12 C

1955 ◽  
Vol 228 (1174) ◽  
pp. 376-396 ◽  
Keyword(s):  
Ground State ◽  
Energy Levels ◽  
Electric Quadrupole ◽  
Angular Distributions ◽  
Reaction Energy ◽  
Reaction Proceeds ◽  
Γ Ray ◽  
Relationship Of ◽  
The Relationship ◽  
Α Particles

The mechanism of the 12 C(γ, 3α) reaction, for γ-ray energies, E γ , up to about 40 MeV, has been determined from a study of over 2500 stars in nuclear emulsions. The study includes investigation of the angular distributions and correlations of the α-particles. The reaction is initiated mainly by electric-dipole and electric-quadrupole γ-ray interaction, the former being unexpectedly strong when E γ < 20 MeV. For E γ < 25 MeV the reaction proceeds mainly by transitions to the ground-state of 8 Be (spin J = 0), and to 2⋅95 ± 0⋅10 MeV ( J = 2) and 4⋅0 ± 0⋅1 MeV ( J = 2 or 4) levels of 8 Be. Transitions to levels near 6, 10 and 15 MeV (all J = 0, 2 or 4) become predominant when 25 MeV ≤ E γ <26 MeV. For E γ ≥ 26 MeV, most transitions lead to 16⋅8 ± 0⋅2 MeV ( J = 2) and 17⋅6 ± 0⋅2 MeV ( J = 2, possibly 0) levels, and possibly to a further 16⋅4 ± 0⋅2 MeV ( J = 0 or 2) level, levels which have not been detected in other reactions. The reaction mechanism is interpreted in terms of competing modes of decay of a compound nucleus, demonstrating the strong influence of the isotopic spins ( T ) of the levels of 12 C and 8 Be involved. For example, the 2 + levels of 12 C involved when 16 MeV ≤ E γ <20 MeV are (unexpectedly) found to have T = 1, and the 16⋅8 and 17⋅6 MeV levels of 8 Be are also found to have T = 1. The relationship of the 12 C (γ, 3α) reaction to other 12 C photodisintegration reactions (including some new reactions established during the present experiments) is discussed.

Energy levels ofCm249from measurements of thermal neutron capture gamma rays

1982 ◽  
Vol 25 (5) ◽  
pp. 2232-2254 ◽  
Author(s):  
R. W. Hoff ◽  
W. F. Davidson ◽  
D. D. Warner ◽  
H. G. Börner ◽  
T. von Egidy
Keyword(s):  
Thermal Neutron ◽  
Gamma Rays ◽  
Neutron Capture ◽  
Energy Levels ◽  
Thermal Neutron Capture

Gamma Rays from theHg199(n, γ)Hg200Reaction and Energy Levels inHg200

1967 ◽  
Vol 164 (4) ◽  
pp. 1548-1558 ◽  
Author(s):  
O. W. B. Schult ◽  
W. R. Kane ◽  
M. A. J. Mariscotti ◽  
J. M. Simic
Keyword(s):  
Gamma Rays ◽  
Energy Levels
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