Monte-Carlo simulation of pinhole collimator of a small field of view gamma camera for small animal imaging

Needs in scintimammography applications,especially for small animal cardiac imaging,lead to develop a small field of view,high spatial resolution gamma camera with a pinhole collimator.However the ideal pinhole collimator must keep a compromise between spatial resolution and sensitivity.In order to design a pinhole collimator with an optimized sensitivity and spatial resolution,the spatial resolution and the geometric sensitivity response as a function of the source to collimator distance has been obtained by means of Monte-Carlo simulation for a small field of view gamma camera with a pinhole collimator of various-hole diameters.The results show that the camera with pinhole of 1 mm,1.5 mm and 2 mm diameter has respectively spatial resolution of 1.5 mm,2.25 mm and 3 mm and geometric sensitivity of 0.016%,0.022%and 0.036%,while the source to collimator distance is 3 cm.We chose the pinhole collimator with hole diameter size of 1.2 mm for our the gamma camera designed based on the trade-off between sensitivity and resolution.

Effects of Magnetic Fields on Neutrino-dominated Accretion Model for Gamma-ray Bursts

Many models of gamma-ray bursts suggest a common central engine; a black hole of several solar masses accreting matter from a disk at an accretion rate from 0.01 to 10 M⊙s^-1, the inner region of the disk is cooled by neutrino emission and large amounts of its binding energy are liberated, which could trigger the fireball. We improve the neutrino- dominated accreting flows by including the effects of magnetic fields. We find that more than half of the liberated energy can be extracted directly by the large-scale magnetic fields in the disk, and it turns out that the temperature of the disk is a bit lower than the neutrino-dominated accreting flows without magnetic field. Therefore, the outflows are magnetically-dominated rather than neutrino dominated. In our model, the neutrino mechanism can fuel some GRBs （not the brightest ones）, but cannot fuel X-ray flares. The magnetic processes （both BZ and electromagnetic luminosity from a disk） are viable mechanisms for most of GRBs and their following X-ray flares.

Slow Gamma Activity of Local Field Potentials (LFP) in the Freely Moving Rat Relates to Movement

Quantitative assessment of local field potentials by means of Fast Fourier Transformation (FFT) results in the so-called power density spectrum. Within this spectrum particular frequency ranges are defined in order to relate these to behavior. Frequencies above 35 Hz are generally labeled as gamma oscillations, especially as low gamma (40 - 55 Hz) or high gamma (70 - 100 Hz). In order to learn more about this feature, we implanted a set of 4 bipolar concentric steel electrodes in frontal cortex, hippocampus, striatum and midbrain reticular formation of 10 rats. After recovery, field potentials were recorded and wirelessly transmitted to our computer for frequency analysis. At the same time, motion was registered during the whole experimental period of 5.75 hours. Results revealed that low gamma activity only emerged when the animal moved—at least his head. FFT of the data showed—besides other frequencies—a slow gamma activity peaking around 47 Hz pre-dominantly within the striatum, less in frontal cortex and reticular formation and nearly none in the hippocampus. Spectral analysis was performed for single epochs of 4 seconds and all 15 minutes intervals. Correlation analysis of these intervals was done to motion data. All rats showed a highly significant correlation between gamma activity and movement. We therefore conclude from these experiments that this slow gamma activity of the field potentials is not only related to movement, but possibly part of the general neuronal coding of movement.

Total Indicative Dose Determination in Water from the North Riviera Well Field of SODECI in Abidjan, Cote d’Ivoire

The Uranium-238 (238U), Thorium-232 (232Th) families and Potassium-40 (40K) are of terrestrial origin and contribute generally to an individual’s external exposure through our presence in this environment. They also contribute to the internal exposure through the ingestion of products and beverages such as water that are close to the earth. The aim of this work is to determine the committed effective dose or Total Indicative Dose (TID) due to gamma radioactivity of the borehole water from the Nord Riviera (NR) well field operated by the Côte d’Ivoire Water Distribution Company (SODECI) for the supply of drinking water to part of the population of Abidjan. In addition, the populations, with their habits, could use these borehole waters directly as drinking water. To this end, water samples from the seven (07) functional boreholes were collected and analyzed on a gamma spectrometry chain, equipped with an HPGe detector in the laboratory of the Radiation Protection Institute (RPI) of the GHANA Atomic Energy Commission (GAEC). The results of the specific activities of 238U, 232Th and 40K obtained were transcribed into TID. As the natural radioactivity of the borehole water is high [1], the TIDs calculated from the activity results of the natural radionuclides238U, 232Th, and 40K vary for the seven boreholes from 0.150 to 0.166 mSv/yr with an average of 0.161 ± 0.034 mSv/yr. The TID of the control tower, where the borehole water is mixed and treated for household use, is equal to 0.136 ± 0.03 mSv/yr. The TIDs obtained are therefore all slightly greater than the WHO reference dose value of 0.1 mSv/yr. But all remain below the UNSCEAR reference dose of 0.29 mSv/yr.

孔径对γ测井饱和模型内部辐射场影响的计算

γ测井模型,可用于校准铀矿勘查领域的γ测井仪,为我国铀矿勘查提供计量保障。研究其内部辐射场分布规律尤为重要,可为标准建造和量值确定提供理论基础。文章为讨论模型孔径参数对模型内部辐射场强度的影响,开展了孔径变化对饱和模型中心点γ射线辐射强度影响因素分析,并以现有规格γ饱和模型体源为例,通过γ辐射场理论计算及蒙特卡洛模拟方法研究,得到了模型中心点γ射线辐射强度与孔径的协变关系。结果表明现有饱和模型体源钻孔半径r_(0)≤6.5 cm时,孔径对模型中心点γ射线辐射强度影响<5%,满足γ测井仪的校准需求,可为后续开展模型制作时对钻孔参数调整提供理论参考。

图像梯度场的Gamma混合分布模型及其求解

梯度是图像处理中常用的重要信息,但目前还缺乏较准确的数学模型来描述图像梯度与图像组成之间的联系。为此,在分析图像梯度直方图的特点的基础上,提出了一种基于Gamma混合分布的梯度数学模型,随后推导了基于EM算法的模型求解方法,最后通过应用实例和结果分析验证了该模型的准确性和有效性。

经颅磁声电刺激对大鼠工作记忆局部场电位gamma节律的影响

经颅磁声电刺激(TMAES)是一种新型无创的神经调控技术,利用超声与静磁场相互耦合产生感应电场,调节相应脑区的神经节律振荡活动,从而影响大脑学习、记忆等认知功能。为探究经颅磁声电刺激对大鼠工作记忆(WM)行为学实验中gamma节律神经振荡活动的影响,将20只健康成年Wistar大鼠随机分为对照组和刺激组,刺激组大鼠接受0.05~0.15 T、1.33~13.33 W/cm^(2)的经颅磁声电刺激,持续10 d,对照组不接受刺激;采集T型迷宫工作记忆任务中大鼠前额叶皮层(PFC)的局部场电位信号(LFPs),对比分析两组间的行为学差异、LFPs的时频分布和互信息相关性。结果显示,刺激组大鼠执行工作记忆任务达到正确率80%以上所需时间为(7.57±0.99)d,明显少于对照组(10.65±2.32)d(P<0.05);在经过选择点位置前后,2.66~13.33 W/cm^(2)组、0.10~0.15 T组大鼠LFPs信号gamma频段的能量密度明显高于对照组的相应值(P<0.05),6.65~13.33 W/cm^(2)组、0.10~0.15 T组大鼠gamma频段12通道信号间的相关性明显强于对照组的相应值(P<0.05)。研究结果表明,经颅磁声电刺激能够增强大鼠工作记忆中前额叶皮层神经元集群gamma节律振荡活动,为进一步探索经颅磁声电刺激调节大脑记忆功能的作用机制奠定基础。

结合马尔可夫随机场和混合模型的海岸线提取

为了高效且准确地实现基于遥感影像的海岸线提取,提出一种结合马尔可夫随机场和混合模型的合成孔径雷达(synthetic aperture radar,SAR)影像海岸线提取算法。该算法以统计模型理论为研究基础,考虑SAR影像中同一地物像素反射强度的统计分布具有非对称和重尾的统计特性,利用伽马混合模型建立SAR影像内像素强度的概率分布。为了建模像素的空间相关性,采用马尔可夫随机场构建伽马混合模型的组分权重概率分布以克服SAR影像相干斑噪声的影响。结合马尔可夫随机场和伽马混合模型构建出SAR影像海陆分割模型,通过最大期望方法估计模型参数以实现准确的海陆分割,进而实现海岸线提取。在Sentinel-1卫星SAR影像上进行海岸线提取实验,实验结果表明该算法可实现准确的海岸线提取。

基于层次Gamma混合模型的高分辨率SAR影像分割方法

为了准确地对高分辨率合成孔径雷达(SAR)影像内像素强度统计分布建模并得到高精度的分割结果,提出基于层次Gamma混合模型(HGa MM)的高分辨率SAR影像分割方法.HGa MM由多个Gamma混合模型构成,用于对非对称、重尾和多峰等复杂的像素强度统计分布建模.为了减少影像噪声对分割的影响,采用马尔科夫随机场建模像素标号场,将像素邻域位置关系引入HGa MM.根据贝叶斯理论,利用后验分布构建影像分割模型.马尔科夫链蒙特卡罗算法用于模拟影像分割模型.在模拟和真实SAR影像上的分割实验表明,文中方法可得到较高精度的分割结果.

放疗计划参数对剂量验证计划γ通过率的相关性研究

目的 探讨头颈部放疗计划参数对剂量验证计划γ通过率的相关性。方法 选取2019年11月—2021年9月福建肿瘤医院放疗中心收治的184例放射治疗的头颈部肿瘤患者。其中85例采用调强放疗(intensity-modulated radio therapy,IMRT)计划,99例采用容积旋转调强放疗(volumetric modulated arc therapy,VMAT)计划,通过电子射野影像装置,使用ArcCHECK分别对IMRT和VMAT计划进行计量验证,并在不同的γ分析标准(选取1%/1 mm,2%/2 mm和3%/3 mm)下验证剂量通过率。分析不同放疗计划中射野复杂度指标,并判断其射野复杂度指标与γ通过率的相关性。结果 VMAT计划在1%/1 mm标准下γ通过率低于IMRT计划,差异有统计学意义(P <0.05);VMAT计划和IMRT计划在2%/2 mm标准下γ通过率分别为(90.72±2.84)%、(90.59±5.19)%,在3%/3 mm标准下γ通过率分别为(97.02±1.71)%、(98.64±1.00)%,2种计划在3%/3 mm标准下的平均γ通过率均较高,在2%/2 mm标准下的平均γ通过率均有所下降,2种计划比较差异无统计学意义(P> 0.05)。在不同射野复杂度指标中,VMAT计划的计划标准跳数(plan normalized MU,PMU)、计划平均射野不规则性(plan averaged beam irregularity,PI)、计划平均射野调制(plan averaged beam modulation,PM)均大于IMRT计划,VMAT计划的平均调制复杂度分数(modulation complexity score,MCS)、计划平均射野面积(plan averaged beam area,PA)小于IMRT计划,差异有统计学意义(P <0.05)。Spearman相关性检验结果表明,IMRT计划中,在2%/2 mm标准下,MCS、PM和γ通过率呈弱相关性(|r|<0.4,P <0.05),PMU和γ通过率呈中度相关性(0.4≤|r|≤0.7,P <0.05),在3%/3 mm标准下,PMU、MCS、PM和γ通过率呈中度相关性(0.4≤|r|≤0.7,P <0.05);PA、PI与γ通过率均无相关性(P> 0.05);VMAT计划中,在2%/2 mm标准下,PMU、MCS、PI、PM和γ通过率呈中度相关性(0.4≤|r|≤0.7,P <0.05),在3%/3 mm标准下,PMU、MCS、PM、PI和γ通过率呈中度相关性(0.4≤|r|≤≤0.7,P <0.05),PA与γ通过率均无相关性(P> 0.05)。结论射野复杂度指标与γ通过率具有不同程度的相关性,可在剂量验证前调整射野指标辅助设计放疗计划。

Beta-Gamma函数对余元公式的推导与实现

对构造的公式①,在复数域将其被积函数分解得2n个复根.在实数域将其实虚部积分取极限获证.对构造的公式②,由①将其被积函数的连续性、收敛性及一致收敛性与构造的有理数列用变量替换代入取极限获证.再由①与②应用Gamma-Beta函数的另一形式及(3),得到了余元公式的实现.

基于遗传算法的场堆叠硅基OLED微显示器伽玛校正研究

硅基有机发光二极管(OLED)微显示器的驱动方式主要分为数字驱动和模拟驱动。在数字驱动中,OLED器件的等效电容导致开启过程中产生亮度脉冲,特别是在场堆叠驱动方式中,固定小数子场的开关过程带来的亮度脉冲直接影响显示的亮度,导致灰阶曲线呈现出非线性递增,这为Gamma校正带来了挑战。为改善Gamma校正的过程及其结果,基于场堆叠数字驱动提出了一个新型亮度模型。该模型结合场顺序、场权值、Vcom电压值和Vcom电压配置,组成一个综合的参数空间。基于该模型,运用遗传算法对灰阶曲线进行了优化,并在分辨率为2560×2560×3的全彩硅基OLED微显示器上进行了实验验证。实验结果表明,通过优化参数空间,白色光灰阶曲线的均根方差和无效灰度点数从21.65 cd/m^(2)、15395个降至1.62 cd/m^(2)、2977个,得到显著改善。这一改进不仅使灰阶曲线更加线性和单调,还有效减少了无效灰度点,成功地实现了白色光Gamma 2.2曲线的精确校正。相比于模拟驱动,场堆叠数字驱动在低灰阶显示上展现出更佳的区分度,更符合人眼对显示效果的感知。

Radioactivity levels in soil of salt field area,Kelambakkam,Tamilnadu,India

Soil samples in and around salt field area have been analyzed for natural radioactivity concentration using gamma ray spectrometer.The activity concentration for ^(232)Th,^(238)U and ^(40)K are ranged from 27.88 to 45.27 Bq/kg, from BDL to 13.30 Bq/kg,and from 135.54 to 381.28 Bq/kg,respectively.The measured activity concentrations for these radionuclides were compared with world average activity of soil.The average activity concentration of ^(232)Th in the present study is 1.19 times higher than world median value while the activity of ^(238)U and ^(40)K is found to be lower. The absorbed dose rates due to these radionuclides were calculated.The average absorbed gamma dose rate due to the presence of ^(232)Th,^(238)U and ^(40)K in soil samples is 36.99 nGy·h^(-1).These results indicate no radiological anomaly. The data presented in this study will serve as a base line survey for primordial radionuclides concentration in the study area.

Monte-Carlo simulation of cement neutron field distribution characteristics in PGNAA

The distribution characteristics of the neutron field in cement was simulated using the MCNP code to comply with the requirements of an online Prompt Gamma Neutron Activation Analysis system.Simulation results showed that the neutron relative flux proportion reduced with increasing cement thickness.When the cement thickness remains unchanged,the reduced proportion of thermal neutrons increases to a small extent,but the epithermal, intermediate,and fast neutrons will decrease according to the geometric progression.H element in the cement mainly affects the reduction of fast neutrons and other single-substance elements,e.g.,O,Ca,56Fe,Si,and Al.It also slows down the reduction of the fast neutrons via inelastic scattering.O contributes more than other elements in the reduction of fast neutrons.Changing the H content affects the thermal,epithermal,intermediate,and fast neutrons, while changing the Ca,Fe,and Si contents only influences the thermal,epithermal,and intermediate neutrons;hence, there is little effect on the reduction of fast neutrons.

Hardening of Thermal Photons Through Inverse Compton Scattering in Strong Magnetic Fields

A new spectrum function is obtained by use of the Compton scattering cross section in the laboratory frame derived earlier. This spectrum function, besides some modifications in the coefficients of the resonant term, contains also a non-resonant term which is inversely proportional to the square of the magnetic field. Based on this spectrum function, the hardening of thermal photons through inverse Compton scattering by relativistic electron beams on the surface of a strongly magnetized neutron star is investigated. Two new features are found. First, there is a maximum scattered photon energy for a given resonant scattering, beyond which resonance disappears. This maximum depends on the electron energy and the magnetic field, but is independent of the incident photon energy. Second, beyond each resonant scattering, there is a high-energy tail, resulting from non-resonant scattering. It is also found that all the tails have a common upper limit which is the highest scattered photon energy for the given incident photon and electron energies. These two new features are absent in the Monte Carlo simulations and therefore, may have physical implications for y-ray emissions.

Time delay and extended halo for constraints on the intergalactic magnetic field

Primary gamma rays emitted from extragalactic very-high-energy （VHE） sources, such as blazars, will generate cascade radiation in intergalactic space with a scale of -- 100 Mpc, for z - 0.1 and Eγ -1 TeV. These cascades proceed through electron-positron pair production and inverse Compton （IC） scattering in the cosmic background radiation fields, mainly cosmic microwave background （CMB） radiation and extragalactic background light in the voids of the universe. The existence of an intergalactic magnetic field （IGMF） would deflect paths of electron-positron pairs that scatter CMB photons, causing some observable effects, such as time delay, an ex- tended halo, and a spectral change. Here we reanalyze the diffusion of an electron jet deflected by IGMF and propose a unified semi-analytical model. By using publicly available data from the Fermi/LAT detector and contemporaneous TeV observations, we find that the cascade photon flux is not significantly affected by the IGMF strength for non-variable blazars when the IGMF is weaker than ,-~ 10-16 G. This result is clearly different from previous works that analyzed the extended halo and time de- lay separately for non-variable blazars and flaring blazars. By applying our model to two extreme blazars （1ES 0229＋200 and 1ES 1218＋304）, we obtain the IGMF lower limit of order ≥10-13 --10-14 G in the non-variable case, which is a stronger constraint on the IGMF strength than previous works （≥10-16 ,-- 10-18 G）, and ≥10-18 -- 10-19 G in the case of flaring blazars. Furthermore, we study the light curves and extended halo of the cascade photons by considering the effects of the IGME

Constraints on axion-like particles with different magnetic field models from the PKS 2155–304 energy spectrum

Axion-like particles(ALPs) are a promising kind of dark matter candidate particle that are predicted to couple with photons in the presence of magnetic fields. The oscillations between photons and ALPs traveling in the magnetic fields have been used to constrain ALP properties. In this work, we obtain some new constraints on the ALP mass ma and the photon-ALP coupling constant g with two different magnetic field models through TeV photons from PKS 2155–304. The first is the discrete-Φ model in which the magnetic field has the orientation angle Φ that changes discretely and randomly from one coherent domain to the next, and the second is the linearly-continuous-Φ model in which the magnetic field orientation angle Φ varies continuously across neighboring coherent domains. For the discrete-Φ model, we can obtain the best constraints on the ALP mass m1 = ma/(1 neV)= 0.1 and on the photon-ALP coupling constant g11= g/(10^-11 GeV^-1)= 5. The reasonable range of the ALP mass m1 is 0.08 ~ 0.2 when g11 = 5,and the only reasonable value of the photon-ALP coupling constant is g11 = 5 when m1 = 0.1. For the linearly-continuous-Φ model, we can obtain the best constraints on the ALP mass m1 = 0.1 and on the photon-ALP coupling constant g11 = 0.7. The reasonable range of the ALP mass m1 is 0.05 ~ 0.4 when g11= 0.7, and the reasonable range of the photon-ALP coupling constant g11 is 0.5 ~ 1 when m1 = 0.1.All of the results are consistent with the upper bound(g < 6.6 × 10^-11 GeV^-1, i.e., g11 < 6.6) set by the CAST experiment.

Radio pulsars with expected gamma radiation and gamma-ray pulsars as pulsating radio emitters

Pulsars play a crucial astrophysical role as highly energetic compact radio, X-ray and gamma- ray sources. Our previous works show that radio pulsars identified as pulsing gamma-ray sources by the Large Area Telescope （LAT） on board the Fermi Gamma-Ray Space Telescope have high values of magnetic field near the light cylinder, two-three orders of magnitude stronger compared with the magnetic fields of radio pulsars： log Blc （G） are 3.60-3.95 and 1.75 correspondingly. Moreover, their losses of rotational energy are also three orders higher than the corresponding values for the main group of radio pulsars on average： logE（erg s-1） = 35.37-35.53 and 32.64. The correlation between gamma- ray luminosities and radio luminosities is found. It allows us to select those objects from all sets of known radio pulsars that can be detected as gamma-ray pulsars with high probability. We provide a list of such radio pulsars and propose to search for gamma emission from these objects. On the other hand, the known catalog of gamma-ray pulsars contains some sources which are not currently identified as radio pulsars. Some of them have large values of gamma-ray luminosities and according to the obtained correlation, we can expect marked radio emission from these objects. We give the list of such pulsars and expected flux densities to search for radiation at frequencies 1400 and 111 MHz.

Dependency of gamma oscillations in E/I neuronal network on illumination contrast of external stimulus

Synchronous gamma oscillations are believed to play a prominent role in the information processing of biological neural systems. Experimental observations have found that the frequency and power of gamma oscillations in the primary visual cortex(V1 zone) are regulated by the illumination contrast of visual stimulus. However, the underlying mechanism of how the synchronous oscillations depend on the illumination contrast has not been well explained. We propose a local excitatory/inhibitory(E/I) neuronal network of integrate-and-fire(IAF) neurons with the difference-of-Gaussians(DOG) receptive field to unveil this mechanism. Simulation results demonstrate that the higher the illumination contrast, the higher the frequency of gamma oscillations. The power of gamma oscillations also increases with the increase of illumination contrast. These results are consistent with the experimental findings.

基于贝叶斯框架和Gamma分布的SAR图像分割

图像分割作为图像处理的关键步骤之一,一种高精度的SAR图像分割方法在图像分析与解译中显得尤为重要。根据SAR图像的统计特性,本文主要研究基于贝叶斯框架和Gamma分布的SAR图像分割方法,分别以单一Gamma分布概率模型和Gamma混合模型定义像素属于聚类的或然率;此外,基于马尔科夫随机场理论定义像素与其邻域像素标号间相互作用关系,并以此作为先验概率;然后,根据贝叶斯定理得到像素属于聚类的后验概率。最后,分别基于上述两种方法对模拟SAR图像及真实SAR图像进行分割实验。结果表明,Gamma混合模型较单一Gamma分布能够更加准确地描述SAR图像分布特征,得到高精度的分割结果。