Cosmic ray air showers in the knee energy region

The cosmic ray extensive air showers in the knee energy region have been studied by the North Bengal University array. The differential size spectra at different atmospheric depths show a systematic shift of the knee towards smaller shower size with the increase in atmospheric depth. The measured values of spectral indices at below and above the knee are −2.45 ±0.03 and −2.91 ±0.05 respectively. Measurements at different atmospheric depths correspond to the same values within the error limits both for below and above the knee. The present experimental results have been compared with similar such experiments     

利用羊八井广延大气簇射阵列探测来自壳型超新星遗迹G40.5-0.5的TeV Gamma射线发射

利用羊八井广延大气簇射阵列从2000年10月到2001年9月的数据,对壳型超新星 遗迹G40.5-0.5可能的TeV gamma射线发射进行了探测. 用对扩展源的二维分析方法发现一个最高超出为4.4σ的天区,EGRET不明源GeV J1907+0557非常接近 这一最高超出天区的中心.     

Search for heavy mass particles in extensive air showers

A large multiplate cloud chamber with fast timing scintillators inside is being operated with the extensive air shower array at Ootacamund to further elucidate the time structure of high energy hardons in air showers. The major interest in the present investigation is to understand the nature of the large delay (>20 ns) high energy (>40 GeV) events that appeared as strong cndidates for heavy mass particles in an earlier experiment carried out with a total absorption spectrometer. Two events observed during one year’s operation of the experiment are discussed. Now deceased.     

寻找超高能宇宙线源——西藏广延空气簇射实验

总结了１９９０年６月到１９９３年１０月期间西藏空气簇射阵列的观测结果。寻找了来自于蟹状星云、Ｘ射线双星、脉冲星、活动星系核和其它活动天体的能量为１０ＴｅＶγ射线连续发射，没有发现连续稳定发射的迹象，但给出了每个源的流强上限。在阵列所观测的天区寻找了１０ＴｅＶ的γ暴，结果没有发现能量１０ＴｅＶ的γ暴，最后也给出了发现此种γ暴的上限。应用该阵列，明显地观测到了能量为１０ＴｅＶ的宇宙线流强的太阳和月亮阴影。观测了朝向和远离太阳的行星际空间磁场对宇宙线阴影的影响，这是行星际磁场对阴影位移影响的第一次直接观测。研究并发现在实验期间，太阳阴影的位置每年都在变化。同时观测在此期间，朝向和远离方向的宇宙线阴影的不同变化。另外，应用该实验的数据，给出了所谓的“膝”区的原初宇宙线能谱。     

Small shower CORSIKA simulations

Extensive Air Showers (EAS) induced by cosmic ray particles of very low energies, owing to the significantly steep cosmic ray energy spectrum, dominate the secondary particle flux measured by single detectors and small shower arrays. Such arrays connected in extended networks can be used to determine potentially interesting spatial correlations between showers, which may shed new light on the nature of ultra high-energy cosmic rays. The quantitative interpretation of showers recorded by small local arrays requires a methodology that differs from that used by ordinary large EAS arrays operating in the "knee" region and above. We present "small EAS generator," a semi-analytical method for integrating cosmic ray spectra over energies of interest and summing over the mass spectra of primary nuclei in arbitrary detector configurations. Furthermore, we provide results on the EAS electron and muon fluxes and particle density spectra.     

利用宇宙线直接测量结果对初级宇宙线能谱参数的调整

由JACEE?,RUNJOB和SOKOL等宇宙线直接测量结果和刚度截断模型,对于10¹⁴—10¹⁶eV能区的初级宇宙线微分能谱参数进行调整.利用调整后的能谱与选取QGSJET模型的CORSIKA程序进行EAS模拟,同HD,PD谱进行对比研究.采用相同的标准对模拟数据与实验数据进行分析.结果表明,调整后的谱和HD谱的模拟结果与甘巴拉山乳胶室实验结果符合较好,而PD谱的模拟结果与实验结果偏离较大.     

一个和X级太阳耀斑相关的甚高能GLE事件

分析怀柔宇宙线EAS阵列在1991年6月份的计数率,数据表明在6月15日的太阳X12/3B级大耀斑后的GLE事件持续期间,TeV能区的宇宙线强度在25min内比通常有将近4a的超出,增强过程持续约25min.     

Multiple penetrating particles with narrow separation associated with extensive air showers (EAS)

An experiment has been carried out at a vertical depth of 580 m.w.e. at Kolar Gold Fields, to investigate various characteristics of energetic muons (E _mln ⋍ 150 GeV) associated with extensive air showers (EAS). Double parallel penetrating particles with narrow separations (<1m) have an exponential decoherence distribution withe-folding separation of ⋍ 25 cm.     

寻找超高能宇宙线源——西藏广延空气簇射实验

总结了１９９０年６月到１９９３年１０月期间西藏空气簇射阵列的观测结果。寻找了来自于蟹状星云、Ｘ射线双星、脉冲星、活动星系核和其它活动天体的能量为１０ＴｅＶγ射线连续发射,没有发现连续稳定发射的迹象,但给出了每个源的流强上限。在阵列所观测的天区寻找了１０ＴｅＶ的γ暴,结果没有发现能量１０ＴｅＶ的γ暴,最后也给出了发现此种γ暴的上限。应用该阵列,明显地观测到了能量为１０ＴｅＶ的宇宙线流强的太阳和月亮阴影。观测了朝向和远离太阳的行星际空间磁场对宇宙线阴影的影响,这是行星际磁场对阴影位移影响的第一次直接观测。研究并发现在实验期间,太阳阴影的位置每年都在变化。同时观测在此期间,朝向和远离方向的宇宙线阴影的不同变化。另外,应用该实验的数据,给出了所谓的“膝”区的原初宇宙线能谱。     

怀柔EAS阵列对初级宇宙线“膝”区能谱的测定

仔细分析了近年来怀柔广延大气簇射阵列记录的65万个大气簇射事例,得到了簇射Size(即荷电总粒子数)谱和10¹⁵—5×10¹⁶eV能段的初级宇宙线微分能谱.此谱呈明显的、平滑过渡的“膝”样结构,拐点在3×10¹⁵eV附近.除了“膝”较平滑不象明野谱那样尖锐拐折而外,怀柔谱在绝对流强和“膝”的位置上都与日本明野组吻合得很好.在银河磁场刚度截止模型框架下,怀柔实验Size谱界定的宇宙线质子谱拐折能量Ec的取值范围在160到240TeV之间.     

怀柔EAS阵列的Monte Carlo研究

用GENAS程序包为怀柔阵列产生了36万Monte Carlo模拟EAS事例,用它们研究了怀柔阵列的性能,确定了最佳的事例判造条件,对实验数据进行了正确性检验,得到了怀柔EAS Size(即簇射在观测面的总荷电粒子数)与初级宇宙线能量之间的转换关系.这项研究表明,怀柔阵列的EAS心位和方向测定精度分别好于3m和2.5°;EASSize测定误差典型值约8%;近垂直簇射的Size(N)与初能(E)的关系为E≈10^10.64N^0.84.     

The Fokker-Planck equation in the second-order pitch angle approximation and its exact solution

The diffusive particle propagation and its pitch angle scattering is studied using kinetic equation of the Fokker-Planck form. The case is considered when charged particles preferable propagate along the strong mean magnetic field direction and undergo the pitch angle scattering with respect to it. The paper deals with solution of the equation for particle distribution function in the second-order approximation in the pitch angle. The exact analytical solution is obtained in an integral form. The well-known solution in the first-order pitch angle approximation can be restored performing the small time limit in the result. Unlike the first-order solution the obtained solution in the second approximation rightly shows that the pitch angle diffusion is closely connected with the particle transport along the mean magnetic field. The expression for particle density for the point instantaneous unidirectional source also has been obtained.     

Cosmic age problem revisited in the holographic dark energy model

Because of an old quasar APM 08279+5255$08279+5255$ at z=3.91$z=3.91$, some dark energy models face the challenge of the cosmic age problem. It has been shown by Wei and Zhang [H. Wei, S.N. Zhang, Phys. Rev. D 76 (2007) 063003, arXiv:0707.2129 [astro-ph]] that the holographic dark energy model is also troubled with such a cosmic age problem. In order to accommodate this old quasar and solve the age problem, we propose in this Letter to consider the interacting holographic dark energy in a non-flat universe. We show that the cosmic age problem can be eliminated when the interaction and spatial curvature are both involved in the holographic dark energy model.     

宇宙线高能族事例产生特征的模拟与实验研究

利用在EAS实验的模拟计算中被广泛采用的CORSIKA程序,基于强相互作用模型QGSJET和DPMJET,对甘巴拉山乳胶室实验高能族事例的产生特征进行了Monte Carlo模拟.给出了不同能区原初宇宙线各种成分产生族事例的效率及其与原初能量的关系.将模拟计算得到的族事例的平均横向扩展、族中簇射成员数、族的总观测能等的分布及其平均值,与相应的实验结果进行了系统的比较,结果基本相符.此外,模拟族事例也存在与实验相类似的能量集中趋势     

Near space radiation dosimetry in Australian outback using a balloon borne energy compensated PIN diode detector

This paper reports the near space ballooning experiment carried out at Australian outback town West Wyalong (33°51′S, 147°24′E) on 19 July 2015. Several dedicated electronic detectors including digital temperature and acceleration (vibration) sensors and an energy compensated PIN-diode gamma ray dosimeter were installed in a thermally insulated Styrofoam payload box. A 9 V Lithium-Polymer battery powered all the devices. The payload box was attached to a helium-filled latex weather balloon and set afloat. The balloon reached a peak burst altitude of 30 km and then soft-landed aided by a self-deploying parachute 66.2 km away form the launch site. The payload box was retrieved and data collected from the electronic sensors analysed. The integrated cosmic ray induced photon ambient dose equivalent recorded by the PIN diode detector was evaluated to be 0.36 ± 0.05 μSv. Furthermore, a high-altitude extended version of commercially available aviation dosimetry package EPCARD.Net (European Program package for the Calculation of Aviation Route Doses) was used to calculate the ambient dose equivalents during the balloon flight. The radiation environment originated from the secondary cosmic ray shower is composed of neutrons, protons, electrons, muons, pions and photons. The photon ambient dose equivalent estimated by the EPCARD.Net code found to be 0.47 ± 0.09 μSv. The important aspects of balloon based near-space radiation dosimetry are highlighted in this paper.     

从乌蒙山到念青唐古拉——百年宇宙线研究的中国故事

百年前,宇宙线的发现曾极大地开阔了人们对宇观和微观世界的眼界,促成了粒子物理学的诞生．新中国成立之初,早年在国外在此领域业已成果卓著的几位前辈,组织起了中国本土第一支宇宙线研究队伍,在云南乌蒙山中建成了中国第一个宇宙线实验室,十年中收获了一系列高水平的实验成果．不幸,此后近20年的磋跎岁月扩大了中国与日新月异的国际新技术之间的差距,中国的宇宙线研究落到了自我边缘化的境地．幸好国家的改革开放政策为奋起直追提供了机会,中国第二代的宇宙线研究者经过种种摸索,选择了高海拔广延大气簇射观测的路线去实现我国宇宙线研究的复兴．20多年的埋头苦干,在海拔4300m的西藏念青唐古拉山脚下建成了一个现代化、国际化的宇宙线实验基地,完成了中国的宇宙线研究从云雾室、手工化向规模化、信息化的历史性转型,并以其特有的低阈能、高事例率、全天候、宽视场优势和国际合作,开展着多项前沿性的科研项目,迎来了丰收的季节．随着国家的日益富强,中国宇宙线研究的年青一代,必将从更高的起点出发,创造出中国宇宙线研究的更大的辉煌．     

A new lateral distribution function for electrons in extensive air showers (EAS) detected near sea level

Summary A detailed analysis of Extensive Air Showers in the size range 10⁴–10⁶ particles detected near sea level has yielded a new distribution function for the radial distribution of EAS electrons. The goodness-of-fit criteria applied to the present and already existing similar distribution functions confirm that the present function is appropriate in EAS at radial distances beyond 20 m from the shower axis.     

Single-particle space-momentum angle distribution effect on two-pion HBT correlation in high-energy heavy-ion collisions

We analyze the transverse momentum dependence of HBT radii in relativistic heavy-ion collisions using several source models.Results indicate that the single-particle space-momentum angle distribution plays an important role in the transverse momentum dependence of HBT radii.In a cylinder source,we use several formulas to describe the transverse momentum dependence of HBT radii and the single-particle space-momentum angle distribution.We also make a numerical connection between them in the transverse plane.     

Investigation of hypersonic flows through a cavity with sweepback angle in near space using the DSMC method

Near space has been paid more and more attentionin recent years due to its military application value.However,flow characteristics of some fundamental configurations(e.g.,the cavity) in near space have rarely been investigated due to rarefied gas effects,which make the numerical simulation methods based on continuous flow hypothesis lose validity.In this work,the direct simulation Monte Carlo(DSMC),one of the most successful particle simulation methods in treating rarefied gas dynamics,is employed to explore flow characteristics of a hypersonic cavity with sweepback angle in near space by considering a variety of cases,such as the cavity at a wide range of altitudes 20-60 km,the cavity at freestream Mach numbers of 6-20,and the cavity with a sweepback angle of 30°-90°.By analyzing the simulation results,flow characteristics are obtained and meanwhile some interesting phenomena are also found.The primary recirculation region,which occupies the most area of the cavity,causes pressure and temperature stratification due to rotational motion of fluid inside it,whereas the pressure and temperature in the secondary recirculation region,which is a small vortex and locates at the lower left corner of the cavity,change slightly due to low-speed movement of fluid inside it.With the increase of altitude,both the primary and secondary recirculation regions contract greatly and it causes them to separate.A notable finding is that rotation direction of the secondary recirculation region would be reversed at a higher altitude.The overall effect of increasing the Mach number is that the velocity,pressure,and temperature within the cavity increase uniformly.The maximum pressure nearby the trailing edge of the cavity decreases rapidly as the sweepback angle increases,whereas the influence of sweepback angle on velocity distribution and maximum temperature within the cavity is slight.     

The effect of single-particle space-momentum angle distribution on two-pion HBT correlation in relativistic heavy-ion collisions using a multiphase transport model

Using the string melting version of a multiphase transport (AMPT) model, we analyze the transverse momentum dependence of the HBT radius \begin{document}$R_{\rm s}$\end{document} and the single-pion angle distribution on the transverse plane in central Au+Au collisions at \begin{document}$\sqrt{S_{NN}}$\end{document}=19.6, 27, 39, 62.4, and 200 GeV. Additionally, a numerical connection between these two phenomena is established with a series of functions. We can estimate the single-pion angle distribution on the transverse plane from HBT analysis.