A Theoretical and Laboratory Evaluation of Carbon Logging - Laboratory Evaluation

1971 ◽  
Vol 11 (02) ◽  
pp. 129-138 ◽  
Author(s):  
B.L. Lawson ◽  
C.F. Cook ◽  
J.D. Owen

Abstract Results we presented from a laboratory experimental evaluation of a carbon well-logging tool based on the detection of the 4.43-MeV gamma rays produced by the inelastic scattering of 14-MeV neutrons. The success of a carbon logging tool is dependent primarily upon the gamma-ray detection scheme used, which in this investigation is a two-crystal pair spectrometer. Using such a device in a simulated reservoir with and without casing and a cement annulus, semiquantitative detection of carbon was accomplished for a fluid-filled packed sand of 35-percent porosity. Analysis of the spectral results show that the log would be sensitive to lithology, saturation and porosity as well as carbon. With the resolution of this particular gamma-ray detector scheme, the presence of the casing using seen, but did not interfere with the carbon signal. Likewise the 1-in. annulus of concrete had no effect on the carbon detection. Comparison of our results with those previously published show that the oxygen and silicon interference encountered i, other proposed logging schemes is eliminated by the two-crystal pair spectrometer. As presently envisaged, between 5 to 10 minutes per pay zone to be evaluated is required to per pay zone to be evaluated is required to accumulate raw data. However, the growth potential offered by the new Ge(Li) gamma-ray counters may well remove this restriction. Introduction Theoretical results presented in Ref. 1 have indicated that liquid hydrocarbons should be detectable in noncarbonaceous reservoirs. Although the interference problem posed by energy degraded gamma rays from omnipresent oxygen is severe, it is not severe enough to prohibit detection of hydrocarbons by nuclear means. The theoretical data also showed thermal neutron effects caused by energy degradation of gamma rays from thermal capture in silicon, chlorine and iron could be eliminated by proper choice of a neutron source gamma detector gating scheme. Indeed, this has been demonstrated experimentally. The crux of the hydrocarbon detection problem lies with finding a gamma detector system with sufficient resolution to pick out 4.43-MeV gamma rays (carbon) from the background provided by oxygen. Previous investigations have shown that single NaI(T1) crystal detectors did not have sufficient energy resolution to accomplish the task. However, energy resolution is not the whole answer when it comes to extracting a monoenergetic signal from a continuum background. In addition to the interfering gamma rays produced through Compton collisions external to the detector system, there is an in-crystal Compton background in single-crystal spectrometry. The second source of interference arises because gamma rays entering the crystal at energies higher than the discrete energy of interest will produce Compton collisions within the crystal generating electrons that have precisely the same energy as that of the "desired signal". This second source of interference significantly reduces the carbon sensitivity of a single-crystal detector. Hence, elimination of the in-crystal background from oxygen produced gamma rays would go far in improving the in-situ carbon detection picture. In searching for an acceptable detector system, this point was kept foremost in mind. It was known a three-crystal pair spectrometer would virtually eliminate the in-crystal Compton background, but limitations imposed by borehole tool size ruled out its use. However, from studying the working principle of this device the concept of the principle of this device the concept of the two-crystal pair spectrometer emerged. A description of such a device was later found in Ref. 4 although no evidence has been found that such a device has been used to record spectra in a borehole or simulated borehole environment. This report presents experimental results obtained with such a presents experimental results obtained with such a two-crystal spectrometer in various simulated reservoir conditions. SPEJ P. 129

2016 ◽  
Vol 675-676 ◽  
pp. 772-775
Author(s):  
Nattasuda Yawai ◽  
Weerapong Chewpraditkul ◽  
Kriangkrai Wantong ◽  
Martin Nikl

The luminescence and gamma-ray detection properties of Gd2SiO5: Ce single crystal scintillator were investigated. The light yield (LY) and energy resolution were measured using R6231 photomultiplier. At 662 keV γ-rays, high LY of 10,300 photons /MeV and good energy resolution of 6.4 % were obtained. The intrinsic LY and light loss coefficient under excitation with 662 keV γ-rays were evaluated. The mass attenuation coefficient for 662 keV γ-rays was also measured by transmission method and compared with the theoretical value calculated by WinXCom program.


2020 ◽  
Author(s):  
Alexander Kozyrev ◽  
Maxim Litvak ◽  
Anton Sanin ◽  
Alexey Malakhov ◽  
Igor Mitrofanov ◽  
...  

<p>The Mercurian Gamma-ray and Neutron Spectrometer (MGNS) is a scientific instrument developed to study the elementary composition of the Mercury’s sub-surface by measurements of neutron and gamma-ray emission of the planet. MGNS measures neutron fluxes in a wide energy range from thermal energy up to 10 MeV and gamma-rays in the energy range of 300 keV up to 10 MeV with the energy resolution of 5% FWHM at 662 keV and of 2% at 8 MeV. The innovative crystal of CeBr3 is used for getting such a good energy resolution for a scintillation detector of gamma-rays.</p> <p>During the BC long cruise to Mercury, it is planned that the MGNS instrument will operate practically continuously to perform measurements of neutrons and gamma-ray fluxes for achieving two main goals of investigations.</p> <p>The first goal is monitoring of the local radiation background of the prompt spacecraft emission due to bombardment by energetic particles of Galactic Cosmic Rays. This data will be taken into account at the mapping phase of the mission on the orbit around Mercury. Detailed knowledge of the spacecraft background radiation during the cruise will help to derive the data for neutron and gamma-ray emission of the planet at the mapping stage of the mission because many elements, like Mg, Na, O and others, the abundance of which at the uppermost layer of the planet is studied, are also present in the material of the spacecraft. Indeed, the nuclear lines of Al, Mg and O are well-pronounced in the spectrum, which are also expected to be detectable in the gamma-ray spectrum of the Mercury emission.</p> <p>The second goal of MGNS cruise operations is the participation in the Inter Planetary Network (IPN) program for the localization of sources of Gamma-Ray Bursts in the sky. In fact, the localization accuracy by the interplanetary triangulation technique is inversely proportional to the distance between the spacecrafts that jointly detected a GRB. Before the launch of BepiColombo, the IPN network included a group of spacecrafts in the near-to-Earth orbit (e.g. Konus-Wind, Fermi-GBM, INTEGRAL, Insight-HXMT) and the Mars Odyssey spacecraft on the orbit around Mars. Now, MGNS provides another interplanetary location, potentially increasing the accuracy of GRBs localization. During the first 13 months of continuous operation, MGNS detected 24 GRB's. Pre-set value of time resolution for continuous measurements of profiles of GRBs is 20 seconds. Since of November 14, 2019, the BC Mission Operation Centre has allocated downlink resources to run MGNS continuously in a 1 sec time resolution for GRB measurements. The GRB detection rate, based on data with a time resolution of 1 sec is about 2-3 GRB's per month.</p> <p>Gamma-rays of solar flares are also detectable by MGNS. Solar flares are nonstationary and anisotropic processes and the ability to observe them from different directions in the Solar system is crucial for further understanding their developments and propagation, as it was demonstrated in the case of HEND instrument on board Mars Odyssey. The Sun cycle is presently around its minimum, and MGNS has not detected any solar events during its first 7 months of the cruise, but the flight to Mercury is long enough and many future flares are expected to be detected.</p> <p>The MGNS instrument will also perform special sessions of measurements during flybys of Earth, Venus and Mercury with the objective to measure neutron and gamma-ray albedo of the upper atmosphere of Earth and Venus and of the surface of Mercury. Another objective is to test the computational model of the local background of the spacecraft using the data measured at different orbital phases of flyby trajectories. The low altitude flybys (such as the 700 km flyby for Venus and three 200 km flybys for Mercury) would be the most useful for such tests being BC maximally shadowed for cosmic radiation by the actual planet. Neutron and gamma-ray measurements during Earth flybys enable investigation of interaction between solar wind and Earth environments as well as studies of spacecraft neutron and gamma-ray background upon its passage through the Earth's radiation belts.</p>


2011 ◽  
Vol 199-200 ◽  
pp. 1796-1803 ◽  
Author(s):  
Chalerm Wanarak ◽  
Weerapong Chewpraditkul ◽  
Akapong Phunpueok ◽  
Jakrapong Kaewkhao

The luminescence and gamma-ray detection properties of the new cerium-doped rare-earth scintillator lutetium-yttrium oxyorthosilicate ( Lu1.95Y0.05SiO5:Ce, LYSO:Ce) were investigated and compared to those of cerium-doped yttrium oxyorthosilicate ( Y2SiO5:Ce, YSO:Ce) crystal. The light yield and energy resolution were measured using photomultiplier tube (PMT) readout. The non-proportionality of the light yield and energy resolution versus γ-ray energy were measured and the intrinsic resolution of the crystals was calculated. In spite of significant progress in light yield and luminescence properties, the energy resolution of LYSO:Ce appears to still suffer from an excess variance in the number of scintillation photons. The mass attenuation coefficient of LYSO:Ce and YSO:Ce for 662 keV gamma rays was also measured by transmission method and compared with the theoretical values calculated by WinXCom program.


1971 ◽  
Vol 41 ◽  
pp. 14-36 ◽  
Author(s):  
Carl E. Fichtel

The detecting systems used in high energy astrophysics are generally more similar to particle detectors than to optical devices. The basic design of the gamma ray instrument depends on whether the energy range is below about 10 MeV and therefore in the region where the Compton effect predominates in the absorption of the gamma-rays, or above that energy where electron-positron pair production is most important. The most usual approach to the detector system in the lower of the two energy intervals is to use a scintillation counter in the center of the detector system to absorb the photons and permit a measure of their energy, and to surround it by another detector which is employed as an active anticoincidence shield to discriminate against charged particles. In the gamma-ray interval above about 10 MeV, the very low flux of gamma rays and the high particle background has directed the development of high energy gamma-ray telescopes towards complicated techniques and large detector arrays. As a result, several investigators have now turned to the spark chamber as the heart of a detector system. Generally, it is surrounded by an anticoincidence system and is triggered by a counter telescope.


1994 ◽  
Vol 353 ◽  
Author(s):  
Ryutaro Fujisawa ◽  
Shigeo Tsujikawa

AbstractThe photoelectrochemical behaviours of a TiO2 single crystal and TiO2 coating were studied, for the purposes of cathodic protection of stainless steels and Cu via the TiO2 coating combined with glass scintillators under gamma ray irradiation. It was confirmed that a TiO2 coating could protect 304 stainless steel cathodically from crevice corrosion under illumination. A logarithmic relationship between the photopotential of single crystal TiO2(rutile) and light intensity was found, moreover, the photopotential was found to be least noble when wavelength equals 375 nm. Under illumination by gamma rays combined with the glass scintillators, the electrode potential of single crystal TiO2 was found to shift in the less noble direction by about 200 mV. Therefore, the technique of cathodic protection by TiO2 coating is considered to be applicable to protect the packaging metal from corrosion for a long time.


2011 ◽  
Vol 199-200 ◽  
pp. 1789-1795 ◽  
Author(s):  
Akapong Phunpueok ◽  
Weerapong Chewpraditkul ◽  
Pichet Limsuwan ◽  
Chalerm Wanarak

The luminescence and gamma-ray detection properties of cerium-doped scintillators, namely, Lu0.3Y0.7AlO3:Ce (Lu0.3Y0.7AP:Ce), Lu0.7Y0.3AlO3:Ce (Lu0.7Y0.3AP:Ce ), and YAlO3:Ce (YAP:Ce) were investigated. UV excitation and emission spectra of studied crystals were compared. The light yield and energy resolution were measured using photomultiplier tube (PMT) readout. The light yield non-proportionality and energy resolution versus gamma-ray energy were measured and the intrinsic resolution of the crystals was determined after correcting the measured energy resolution for PMT statistics. For 662 keV gamma rays (137Cs source), YAP: Ce showed the highest light yield of 28,500 ph/MeV and the best energy resolution of 4.4 % , while its photofraction is worst.


2017 ◽  
Vol 866 ◽  
pp. 329-332
Author(s):  
Akapong Phunpueok ◽  
Voranuch Thongpool ◽  
Weerapong Chewpraditkul

Nowadays, single crystal scintillators play an key role in the scientific researches, high-energy physics and modern medical imaging. In this research, we studied the scintillation response of polished yttrium oxyorthosilicate with Ce-doped (Y2SiO5:Ce, YSO(Ce)) crystals grown by the Czochralski method. The nominal Ce3+ ion is about 0.5% for tested crystals. Energy resolution and photon yield of the scintillator are read out by the photomultiplier tube (XP5200B PMT) under excitation with gamma-rays. The polished YSO:Ce samples (5x5x1 mm3 and 5x5x3 mm3) was tested at room temperature. The 1 mm thick sample shows the better energy resolution than the 3 mm thick crystal. The light yield dependences on the height of crystal were evaluated under excitation with 662 keV gamma ray energy and the intrinsic light yield and loss parameter were also determined.


2020 ◽  
Author(s):  
Alexander Kozyrev ◽  
Maxim Litvak ◽  
Alexey Malakhov ◽  
Igor Mitrofanov ◽  
Maxim Mokrousov ◽  
...  

<p>The Mercurian Gamma-ray and Neutron Spectrometer (MGNS) is a scientific instrument developed to study the elementary composition of the Mercury’s sub-surface by measurements of neutron and gamma-rays emission of the planet. MGNS measures neutron fluxes in a wide energy range from thermal energy up to 10 MeV and gamma-rays in the energy range of 300 keV up to 10 MeV with the energy resolution of 5% FWHM at 662 keV and of 2% at 8 MeV. The innovative crystal of CeBr<sub>3</sub> is used for getting such a good energy resolution for a scintillation detector of gamma-rays.</p><p>During the BepiColombo long cruise to Mercury, it is planned that the MGNS instrument will operate practically continuously to perform measurements of neutrons and gamma-rays fluxes for achieving two main goals of investigations: monitoring of the local radiation background of the prompt spacecraft emission due to bombardment by energetic particles of Galactic Cosmic Rays and the participation in the Inter Planetary Network (IPN) program for the localization of sources of Gamma-Ray Bursts in the sky.</p><p>The MGNS instrument will also perform special sessions of measurements during flybys of Earth, Venus and Mercury with the objective to measure neutron and gamma-rays albedo of the upper atmosphere of Earth and Venus and of the surface of Mercury. Another objective is to test the computational model of the local background of the spacecraft using the data measured at different orbital phases of flyby trajectories. The low altitude flybys (such as the 700 km flyby for Venus and three 200 km flybys for Mercury) would be the most useful for such tests being BC maximally shadowed for cosmic radiation by the actual planet. Neutron and gamma-rays measurements during Earth flybys enable investigation of interaction between solar wind and Earth environments as well as studies of spacecraft neutron and gamma-rays background upon its passage through the Earth's radiation belts.</p>


2011 ◽  
Vol 284-286 ◽  
pp. 2008-2013
Author(s):  
Akapong Phunpueok ◽  
Weerapong Chewpraditkul ◽  
Pichet Limsuwan ◽  
Bing Kun Yu ◽  
Chalerm Wanarak

The scintillation response of Lu0.7Y0.3AP:Ce and Bi4Ge3O12 scintillation crystals have been compared using photomultiplier tube readout for photon energies ranging from 22.1 to 1274.5 keV. Lu0.7Y0.3AP:Ce showed a light yield non-proportionality of about 20% upon lowering energy from 1,274.5 to 22.1 keV, which is better than that of about 39% obtained for Bi4Ge3O12. Lu0.7Y0.3AP:Ce showed the light yield of 13,400 ph/MeV and energy resolution of about 8 % for 662 keV gamma rays from a 137Cs source. The photofraction of Bi4Ge3O12 is better than that of Lu0.7Y0.3AP:Ce. The intrinsic resolution of the crystals versus energy of gamma rays has been determined after correcting the measured energy resolution for photomultiplier tube statistics.


1985 ◽  
Vol 25 (04) ◽  
pp. 515-520 ◽  
Author(s):  
D. Ellis ◽  
C. Flaum ◽  
E. Marienbach ◽  
C. Roulet ◽  
B. Seeman

Abstract A second-generation density logging tool has beendeveloped that uses a gamma-ray source and two NaIscintillator detectors for borehole measurement of electrondensity, pe, and a quantity Fpe that is related to thelithology of the formation. An active stabilization system controls the gains of the two detectors, which permits selective gamma-ray detection. Spectral analysis isperformed in the near detector (two energy windows) and performed in the near detector (two energy windows) and in the detector farther away from the source (three energy windows). This paper describes the results of laboratory measurements undertaken to define the basic tool response. The tool is shown to provide reliable measurements offormation density and lithology under a variety ofenvironmental conditions. Introduction In the second-generation density logging tool, as in otherlogging devices, the principle exploited for the density measurement is that the interaction of medium-energygamma rays (662 keV) with rock formations is primarilya result of Compton scattering with electrons. Thus, theattenuation of gamma rays can be related to the electrondensity (pe) in the scattering material, defined by Zpe = 2<–>Pb,................................(1)A where less than Z/A greater than is the average value ofthe ratio of the atomic number to the atomic weight of thescattering formation. For most rocks, less than Z/A greaterthan is on the order of 0.5, while for hydrogen it is veryclose to 1.0. Therefore, with a knowledge of the lithology and formation fluid constituents, this measured parameter canbe related to the bulk density, pb, of the formation. The traditional transform between measured density values (PLOG)and the electron density is pLOG = 1.0704pe–0.1883........................(2) This ensures that the log-measured density values ofwater-filled calcite agree with the actual bulk density despite the fact that the electron density of water is 11%greater than its bulk density. As the gamma rays emitted from the source are successively scattered, their energy is reduced and they become increasingly subject to photoelectric absorption. This additional attenuation caused by photoelectric absorption is also used to measure the absorption characteristics of the formation, which are determined primarily by its lithology. This measurement is called the primarily by its lithology. This measurement is called the photoelectric factor because it is related to the photoelectric photoelectric factor because it is related to the photoelectric cross section and is referred to as pe in the literature and onlog headings. The theoretical considerations and interpretationof this measurement can be found in Refs. 2 and 3. Our paper describes, in general, the borehole logging devicethat has been designed to meet these goals. The measurements made to define the tool response are presented, as well as the performance of the tool under laboratory and field conditions. performance of the tool under laboratory and field conditions. Description of the Hardware The basic components of the measurement system are a1.5-Ci radioactive source of (137)Cs and two NaIcrystal/photo multiplier assemblies. The two gamma-raydetectors are necessary for mudcake compensation, which is discussed in the section on Environmental Effects. Awindow made of beryllium allows low-energy gamma raysfrom the formation to pass through the skid-shieldingmaterial and pressure housing for use in the lithology measurement. To make the lithology measurement and to improve the response of the density measurement, a spectral analysis of the detected gamma rays is made. Measurements are made in three distinct energy regions at the farther detector(LS) from the source and two at the nearer (SS). To make these spectral measurements, a system of active gain stabilization has been incorporated. This is achieved, bythe use of two weak (137)Cs reference sources, one foreach detector. These provide references for the two feed-backloops. Fig. 1 shows the approximate location of the windows used in the energy analysis. Estimates of the density ofthe formation are obtained from the LS window labeledLs and the SS window labeled Ss1. The lower-energy edgeof these two windows was determined as a compromise between the needs for both high counting rate and aminimization of photoelectric absorption perturbations. The inference of the formation lithology comes from acomparison of the LS window labeled LITH and the Lswindow. The long-spacing detector's density estimate isrefined further by using the LITH window to compensatefor any residual photoelectric absorption in the primary window (Ls). primary window (Ls).SPEJ P. 515


Sign in / Sign up

Export Citation Format

Share Document