A search for heavy leptons in cosmic radiation underground

An experiment to search massive long-lived, weakly interacting particles (leptons) in cosmic radiation has been conducted at Kolar Gold Fields at a depth of 7.6 hg cm⁻² (1 hg cm⁻²=100 g cm⁻²) below surface. The apparatus was senstive to sub-relativistic (velocity<0.75 c) charged leptons of mass greater than that of a proton and life times greater than a microsecond. The method consists of selecting charged particles using a scintillator counter telescope and vetoing relativistic particles (velocity >0.75 c) by using a water Čerenkov detector. The range of the particle is observed in arrays of neon flash tubes interspersed with iron absorbers. During 3000 hours of observation 28 events were recorded satisfying the trigger and event selection criteria. Bulk of these events were interpreted as due to recoil protons (low energy) from the inelastic scattering of high energy muons in the overhead absorber. The remaining events were interpreted as either atmospheric stopping protons or stopping muons that failed to generate a Čerenkov signal. The observed events are thus consistent with the background and no heavy leptons were seen. From our observations an upper limit of 2.12×10⁻⁷ (with 90% confidence level) is set on the ratio of the flux of heavy leptons to that of all muons at this depth.     

Detection of Supersymmetric Dark Matter

A re-analysis of a heavy charged particle production event observed at the cloudy chamber of the Yunnan Cosmic Ray Station (YCRS) in 1972 indicates that the mysterious heavy particle may be identified as a supersymmetric (SUSY) particle produced by a bombard of a neutral SUSY cosmic ray particle on proton. Based on the assumption, following the literatures that the neutral SUSYparticle which constitutes the main fiaction of the cold dark matter is scalar neutrino (sneutrino) or neutralino (photino), we evaluate the flux of such SUSY particles which gain sufficient energies via elastic scattering with charged cosmic particles on the way to an Earth detector and the capture rates in both the sneutrino and photino cases respectively. The errors appearing in the study are briefly discussed and this work may provide a basis of designing cosmic ray detectors to search for SUSY particles from the heaven.     

临近空间大气中子环境的仿真研究

以大气模型、宇宙线模型和地磁截止刚度模型为基础,利用蒙特卡罗方法在国内首次建立了临近空间大气中子环境的计算机仿真模型,分别研究了银河宇宙线、太阳宇宙线诱发的大气中子环境分布规律以及地磁场屏蔽作用对大气中子环境的影响.通过与国外相关模型对比,证明本仿真模型是准确、可靠的,对太阳质子事件的详细分析,弥补了国外已有模型中的不足.该模型可用于临近空间大气中子诱发的元器件单粒子效应评估,以及航空机组人员飞行期间所接受的辐射剂量分析. 关键词： 临近空间 大气中子 单粒子效应 蒙特卡罗     

Two-decade experience of application of plastic nuclear track detectors to cosmic ray research on satellites and orbital space stations

The work generalizes the results obtained during the last two decades in our spaceborne experiments aimed at studying galactic cosmic rays and cosmic ray anomalous component and carried out using solid-state nuclear track detectors (SSNTD) mounted mostly outside spacecraft. The experimental equipment and the techniques for identifying cosmic ray ions and for calculating particle flux values are described. The experimental data are used to construct a modified model for the fluxes and spectra of cosmic ray protons and heavy nuclei to be calculated to within a higher accuracy compared with the earlier models.     

Evidence for the production of new particles in cosmic ray experiments deep underground

In the cosmic ray experiments deep underground in the Kolar Gold Mines, a special class of events has been observed, at present 6 in number, characterised by several, (in general 3), charged particles arising from a vertex, either in air or in the thin material of the detectors, with large opening angles; the vertex is at a distance of around 70–100 cms from the rock wall. The most plausible interpretation of these events is that they are due to the decay of new, massive and long-lived particles produced in neutrino collisions inside rock, or through hitherto unknown processes.     

宇宙线天体物理中的几个重要问题

宇宙线是来自宇宙空间的高能粒子流，研究宇宙线的起源、加速、传播机制及其所涉及的天体物理和宇宙学过程是宇宙线天体物理研究的重要内容。本文介绍并讨论其中几个涉及物理学一些基本问题的重要课题的研究现状及前景，其中包括极高能宇宙线的观测研究，太阳中微子能谱的实时测量，宇宙线中新粒子的搜寻等。     

宇宙线天体物理中的几个重要问题

宇宙线是来自宇宙空间的高能粒子流,研究宇宙线的起源、加速、传播机制及其所涉及的天体物理和宇宙学过程是宇宙线天体物理研究的重要内容。本文介绍并讨论其中几个涉及物理学一些基本问题的重要课题的研究现状及前景,其中包括极高能宇宙线的观测研究,太阳中微子能谱的实时测量,宇宙线中新粒子的搜寻等。     

Ionization states of cosmic rays:Anuradha (IONS) experiment in Spacelab-3

The measurements of the ionization states, composition, energy spectra and spatial distribution of heavy ions of helium to iron of energies 10–100 MeV/amu in the anomalous cosmic rays are of major importance in understanding their origin which is unknown at present.Anuradha (IONS) cosmic ray experiment in Spacelab-3 was designed to determine the above properties in near earth space and this had a highly successful flight and operations aboard the shuttle Challenger at an orbital altitude of 352 km during 29 April to 6 May 1985. The instrument employs solid state nuclear track detectors (CR-39) of high sensitivity and large collecting area of about 800 cm² and determines the arrival time information of particles with active elements. Experimental methods, flight operations and preliminary results are briefly described. Initial results indicate that relatively high fluxes of low energy cosmic ray α-particles, oxygen group and heavier ions were obtained. The flight period corresponded to that of quiet Sun and the level of solar activity was close to solar minimum. It is estimated that about 10,000 events of low energy cosmic ray alpha particles with time annotation are recorded in the detector together with similar number of events of oxygen and heavier ions of low energy cosmic rays. The authors felicitate Prof. D S Kothari on his eightieth birthday and dedicate this paper to him on this occasion.     

Gamma ray line astronomy as a probe of cold dark matter

Some annihilation processes of cold dark matter particles in the galactic halo may result in monochromatic gamma rays with an astrophysically significant rate. This paper summarizes the calculation of these rates and discusses the expected gamma ray line flux in comparison with the diffuse cosmic background.     

New Universal Cosmic-Ray Knee near a Magnetic Rigidity of 10 TV with the NUCLEON Space Observatory

Data from the NUCLEON space observatory give a strong indication of the existence of a new universal cosmic ray “knee”, which is observed in all groups of nuclei, including heavy nuclei, near a magnetic rigidity of about 10 TV. Universality means the same position of the knee in the magnetic rigidity scale for all groups of nuclei. The knee is observed by both methods of measurement of particles energy implemented in the NUCLEON observatory—the calorimetric method and the kinematic method Kinematic Lightweight Energy Meter. This new cosmic ray knee is probably connected with the limit of acceleration of cosmic rays by some generic or nearby source of cosmic rays.     

Cosmic Ray Electrons and Protons,and Their Antiparticles

Cosmic rays are a sample of solar, galactic, and extragalactic matter. Their origin, acceleration mechanisms, and subsequent propagation toward Earth have intrigued scientists since their discovery. These issues can be studied via analysis of the energy spectra and composition of cosmic rays. Protons are the most abundant component of the cosmic radiation, and many experiments have been dedicated to the accurate measurement of their spectra. Complementary information is provided by electrons, which comprise about 1 % of the cosmic radiation. Because of their low mass, electrons experience severe energy losses through synchrotron emission in the galactic magnetic field and inverse Compton scattering of radiation fields. Electrons therefore provide information on the local galactic environment that is not accessible from the study of the cosmic ray nuclei. Antiparticles, namely antiprotons and positrons, are produced in the interaction between cosmic ray nuclei and the interstellar matter. They are therefore intimately linked to the propagation mechanisms of the parent nuclei. Novel sources of primary cosmic ray antiparticles of either astrophysical (e.g., positrons from pulsars) or exotic origin (e.g., annihilation of dark matter particles) may exist. The nature of dark matter is one of the most prominent open questions in science today. An observation of positrons from pulsars would open a new observation window on these sources. Several experiments equipped with state-of-the art detector systems have recently presented results on the energy spectra of electrons, protons, and their antiparticles with a significant improvement in statistics and better control of systematics. The status of the field will be reviewed, with a focus on these recent scientific results.     

用重离子实验数据推算质子翻转截面和轨道翻转率

空间单粒子辐射环境主要由重离子和高能质子构成,但在地面利用两种离子评估器件单粒子效应敏感度成本太高,因此利用重离子实验数据推算质子敏感参数成为一个非常活跃的研究课题.利用Barak经验公式,在重离子实验获得器件的σ LET值曲线的基础上,计算了几种典型器件在不同能量下的质子翻转截面以及典型轨道上质子引起的翻转率,并同FOM方法预示的质子翻转率进行了比较,其结果将对卫星电子系统抗辐射加固设计具有重要参考价值. The radiation environments concerned with single event upset mainly consist of heavy ions from cosmic ray and large flux proton from solar events and planetary radiation belts. The most reliable calculation for SEE rate induced by proton and henvy ions are the way to use the experimentally measured data rospectively. But it is too expensive to test devices with both heavy ions and protons. So it is necessary to derive models for predicting proton cross sections and rates from heavy ion test data....     

Is astronomy possible with neutral ultrahigh energy cosmic ray particles existing in the standard model?

The recently observed correlation between HiRes stereo cosmic ray events with energies E ∼ 10¹⁹ eV and BL Lacertae objects occurs at an angle that strongly suggests that the primary particles are neutral. We analyze whether this correlation, if not a statistical fluctuation, can be explained within the Standard Model, i.e., assuming only known particles and interactions. We have not found a plausible process that can account for these correlations. The mechanism that comes closest—the conversion of protons into neutrons in the IR background of our Galaxy—still underproduces the required flux of neutral particles by about two orders of magnitude. The situation is different at E ∼ 10²⁰ eV, where the flux of cosmic rays at the Earth may contain up to a few percent of neutrons, indicating their extragalactic sources. The text was submitted by the authors in English.     

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.     

On Possible Sources of Heavy Neutral Particles in Cosmic Rays

We explore some possible mechanisms by which the heavy neutral cosmic particles are accelerated to gain sufficiently high kinetic energies and cause observable effects at detectors on the earth. Our results indicate that all the known sources which are based on the established theories and observations fail to give rise to very high energy with sizable flux intensity. If the heavy neutral particles of kinetic energies of GeV order indeed exist in cosmic rays, there must be certain mechanisms beyond our present knowledge of dark matter and universe evolution.     

Single event effect hardness for the front-end ASICs in the DAMPE satellite BGO calorimeter

The Dark Matter Particle Explorer(DAMPE) is a Chinese scientific satellite designed for cosmic ray studies with a primary scientific goal of indirect detection of dark matter particles. As a crucial sub-detector, the BGO calorimeter measures the energy spectrum of cosmic rays in the energy range from 5 Ge V to 10 Te V. In order to implement high-density front-end electronics(FEE) with the ability to measure 1848 signals from 616 photomultiplier tubes on the strictly constrained satellite platform, two kinds of 32-channel front-end ASICs, VA160 and VATA160,are customized. However, a space mission period of more than 3 years makes single event effects(SEEs) become threats to reliability. In order to evaluate SEE sensitivities of these chips and verify the effectiveness of mitigation methods, a series of laser-induced and heavy ion-induced SEE tests were performed. Benefiting from the single event latch-up(SEL) protection circuit for power supply, the triple module redundancy(TMR) technology for the configuration registers and the optimized sequential design for the data acquisition process, 52 VA160 chips and 32VATA160 chips have been applied in the flight model of the BGO calorimeter with radiation hardness assurance.     

Flux of Scalar Neutrino Dark Matter

Recently the exotic event observed at the Yunnan Cosmic Ray Station (YCRS) is reinterpreted as a neutral supersymmetric (SUSY) particle bombarding on proton to produce a charged SUSY particle which decays afterwards. The kinematics analysis determines the lower bounds of its mass and lifetime. Taking this bounds as inputs and following recent literatures to assume the scalar neutrino (sneutrino) as the main constituent of the cold SUSY dark matter, we calculate the flux of sneutrino at the earth detector in terms of the standard rate equation of cosmic matter.     

Energetic neutrons and gamma rays measured on the Aryabhata satellite

An experiment to measure energetic neutrons and gamma rays in space was launched in the first Indian scientific satellite,Aryobhata, on April 19, 1975. From this experiment, the first measurements in space of the Earth’s albedo fiux of neutrons of energy between 20 and 500 MeV have been made; the values obtained for two mean geomagnetic vertical cut-off rigidities of 5.6 and 17.0 GV are (6.3±0.4)×10⁻² and (1.4±0.3)×10⁻² neutrons cm⁻² sec⁻¹ respectively. These measurements confirm that protons arising from cosmic ray albedo neutron decay, can adequately account for the protons in the inner radiation belt. Observations on gamma rays of energy between 0.2 and 24 MeV have enabled the determination of the total background gamma ray flux in space as a function of latitude. This in turn has permitted useful information on the diffuse cosmic gamma rays. We have also observed four events that showed sudden increases in the gamma ray counting rates between 0.2 and 4.0 MeV. Observational details of these events are given.     

Impact of high-energy cosmic-ray protons and ions on the elements of spacecraft on-board devices

The radiation environment in space is reviewed in short as an impact factor affecting onboard spacecraft electronics. The mass and energy distributions of the heavy component of space radiation and the contribution of galactic cosmic rays to the general flux are analyzed during a quiet period in solar activity. The nature of the limitations in the concept of linear energy transfer, including the effects of electronic semiconductor component crystallinity, is discussed. Protective measures against upsets in onboard electronics, caused by cosmic ray ions, are considered.