Neutrons and antiprotons in ultrahigh-energy cosmic rays

The neutron fraction in the very high-energy cosmic rays near the Greisen-Zatsepin-Kuzmin (GZK) cutoff energy is analyzed by taking into account the time dilation effect of the neutron decays and also the pion photoproduction behaviors above the GZK cutoff. We predict a non-trivial neutron fraction above the GZK cutoff and a negligibly small neutron fraction below. However, there should be a large antiproton fraction in the high-energy cosmic rays below the GZK cutoff in several existing models for the observed cosmic-ray events above and near the GZK cutoff. Such a large antiproton fraction can manifest itself by the muon charge ratio μ⁺/μ^- in the collisions of the primary nucleon cosmic rays with the atmosphere, if there is no neutron contribution. We suggest to use the muon charge ratio as one of the information to detect the composition of the primary cosmic rays near or below the GZK cutoff.     

A theory of cosmic rays

We present a theory of non-solar cosmic rays (CRs) in which the bulk of their observed flux is due to a single type of CR source at all energies. The total luminosity of the Galaxy, the broken power-law spectra with their observed slopes, the position of the ‘knee(s)’ and ‘ankle’, and the CR composition and its variation with energy are all predicted in terms of very simple and completely ‘standard’ physics. The source of CRs is extremely ‘economical’: it has only one parameter to be fitted to the ensemble of all of the mentioned data. All other inputs are ‘priors’, that is, theoretical or observational items of information independent of the properties of the source of CRs, and chosen to lie in their pre-established ranges. The theory is part of a ‘unified view of high-energy astrophysics’ — based on the ‘Cannonball’ model of the relativistic ejecta of accreting black holes and neutron stars. The model has been extremely successful in predicting all the novel properties of Gamma Ray Bursts recently observed with the help of the Swift satellite. If correct, this model is only lacking a satisfactory theoretical understanding of the ‘cannon’ that emits the cannonballs in catastrophic processes of accretion.     

High energy physics in the atmosphere: phenomenology of cosmic ray air showers

The properties of cosmic rays with energies above 10⁶ GeV have to be deduced from the spacetime structure and particle content of the air showers which they initiate. In this review we summarize the phenomenology of these giant air showers. We describe the hadronic interaction models used to extrapolate results from collider data to ultra high energies, and discuss the prospects for insights into forward physics at the LHC. We also describe the main electromagnetic processes that govern the longitudinal shower evolution, as well as the lateral spread of particles. Armed with these two principal shower ingredients and motivation from the underlying physics, we provide an overview of some of the different methods proposed to distinguish primary species. The properties of neutrino interactions and the potential of forthcoming experiments to isolate deeply penetrating showers from baryonic cascades are also discussed. We finally venture into a terra incognita endowed with TeV-scale gravity and explore anomalous neutrino-induced showers.     

Axion-like particles,cosmic magnetic fields and gamma-ray astrophysics

Axion-like particles (ALPs) are predicted by many extensions of the Standard Model and give rise to characteristic dimming and polarization effects in a light beam travelling in a magnetic field. In this Letter, we demonstrate that photon-ALP mixing in cosmic magnetic fields produces an observable distortion in the energy spectra of distant gamma-ray sources (like AGN) for ranges of the ALP parameters allowed by all available constraints. The resulting effect is expected to show up in the energy band 100 MeV–100 GeV, and so it can be searched with the upcoming GLAST mission.     

Direct photons at forward rapidities in high-energy pp collisions

We investigate direct photon production in pp collisions at the energies of RHIC, CDF and LHC, at different rapidities employing various color-dipole models. The cross section peaks at forward rapidities due to the Abelian dynamics of photon radiation. This opens new opportunities for measurement of direct photons at forward rapidities, where the background from radiative hadronic decays is strongly suppressed. Our model calculations show that photon production is sensitive to the gluon saturation effects, and strongly depends on the value of the anomalous dimension.     

Galactic neutrino communication

We examine the possibility to employ neutrinos to communicate within the galaxy. We discuss various issues associated with transmission and reception, and suggest that the resonant neutrino energy near 6.3 PeV may be most appropriate. In one scheme we propose to make Zo$Z^o$ particles in an overtaking e⁺−e⁻$e^{+}-e^{-}$ collider such that the resulting decay neutrinos are near the W⁻$W^{-}$ resonance on electrons in the laboratory. Information is encoded via time structure of the beam. In another scheme we propose to use a 30 PeV pion accelerator to create neutrino or anti-neutrino beams. The latter encodes information via the beam CP state as well as timing. Moreover the latter beam requires far less power, and can be accomplished with presently foreseeable technology. Such signals from an advanced civilization, should they exist, will be eminently detectable in existing neutrino detectors.     

Pionic charge exchange on the proton from 40 to 250 MeV

The total cross sections for pionic charge exchange on hydrogen were measured using a transmission technique on thin CH₂ and C targets. Data were taken for π⁻${\pi }^{-}$ lab energies from 39 to 247 MeV with total errors of typically 2% over the Δ-resonance and up to 10% at the lowest energies. Deviations from the predictions of the SAID phase shift analysis in the 60–80 MeV region are interpreted as evidence for isospin-symmetry breaking in the s-wave amplitudes. The charge dependence of the Δ-resonance properties appears to be smaller than previously reported.     

An analysis of energetic cosmic ray interactions in graphite

Fifty two high energy cosmic ray interactions in graphite have been analysed. The analysis strongly suggests that some of the characteristics of high energy interactions are dependent on the total transverse momentum,Σp _t, of allγ-rays in an interaction. Out of the 52 events analysed, 29 haveΣp _t⩽2.5 GeV/c and the rest haveΣp _t>2.5 GeV/c; the former are called smallp _t events while the latter are designated as largep _t events. For these two types of events, the characteristics investigated are: (a) fractional energy distribution ofγ-rays, (b) the invariant mass ofγ-rays and (c) the energy distribution ofγ-rays in the emission system.     

Measurements of atmospheric antiprotons

We measured atmospheric antiproton spectra in the energy range 0.2 to 3.4 GeV, at sea level and at balloon altitude in the atmospheric depth range 4.5 to 26 g/cm². The observed energy spectra, including our previous measurements at mountain altitude, were compared with estimated spectra calculated on various assumptions regarding the energy distribution of antiprotons that interacted with air nuclei.     

胡乾善对宇宙射线的研究

胡乾善(1911—2004),振动专家和工程力学教育家,1934—1937年留学英国期间师从布莱克特研究宇宙射线,曾参与宇宙射线的国际合作研究,并与苏联物理学家去高加索山4km处进行宇宙射线测量．他是最早参与宇宙射线研究的中国物理学家之一,回国后由于无研究设备,后致力于机械振动研究．该文是在胡乾善的博士论文及已发表的论文的基础上,回顾并分析了上世纪30年代胡乾善在宇宙射线方面的研究工作,目的是使读者了解当时物理学界在此方面的研究进展．2011年是胡乾善百年诞辰,2012年是宇宙射线发现100周年,谨以此文纪念．     

Processing high-energy proton events: A new approach to searching for primary cosmic ray particles in emulsion chambers,using data from the RUNJOB experiment

Primary single-charged particles were identified in ～50% of the proton events in the Russian-Japanese RUNJOB balloon experiment. In reprocessing the experimental data obtained via long-term exposure of the RUNJOB-3B, 6A, 11A, and 11B emulsion chambers (ECs) using a new approach to searching for primary cosmic-ray particles in groups of proton events with primary particle energy E ₀ > 20 TeV and zenith angle tan(θ) ≤ 5, ～50% of the primary single-charged particles went unidentified, as was the case earlier. In this work, we describe the new approach to searching for and tracking particles in ECs and present the parameters of the processed events (energy, zenith angle, depth of particle penetration into an EC up to interaction).     

A QCD motivated model for soft interactions at high energies

In this paper we develop an approach to soft scattering processes at high energies which is based on two elements: the Good–Walker mechanism for low mass diffraction and multi-pomeron interactions for high mass diffraction. The principal idea, which allows us to specify the theory for pomeron interactions, is that the so called soft processes occur at rather short distances (r ² ∝1/〈p _t 〉² ∝ α′_ℙ≈0.01 GeV⁻²), where perturbative QCD is valid. The value of the pomeron slope α′_ℙ is obtained from a fit to the experimental data. Using this theoretical approach, we suggest a model that fits all soft data in the ISR-Tevatron energy range: total, elastic, single and double diffractive cross sections, as well as the t dependence of the differential elastic cross section, and the mass dependence of single diffraction. In this model we calculate the survival probability of diffractive Higgs production, and we obtain a value for this observable that is smaller than 1% at the LHC energy range.     

Processing of high-energy proton events using a new method for searching primary cosmic ray particles in X-ray emulsion chambers (according to the RUNJOB experiment data)

In the RUNJOB Russian-Japanese balloon experiment, tracks of primary singly charged particles are detected in approximately half the events related to the proton ones. During repeated processing of the experimental data obtained when exposing RUNJOB-3B, 6A, 11A, and 11B X-ray emulsion chambers (XRECs) using the new method for searching primary cosmic particles, approximately 50% of tracks of primary singly charged particles as before were not detected in the group of events related to the proton ones with primary particle energiesE ₀ > 20 TeV and zenith angle tan θ ≤ 5. In this paper,we present a new method for searching and tracing particles in the XREC; characteristics of processed events (the energy, zenith angle, and particle penetration depth in the XREC before the interaction) are given.     

Charged-particle multiplicity distributions in different rapidity windows in 800 GeV proton-nucleus interactions

Multiplicity distributions of charged particles produced in interactions of 800 GeV protons with emulsion nuclei in various rapidity windows are presented. The data is also analyzed separately for the forward and the backward hemispheres, for rapidity windows of different widths. It is found that the Negative Binomial Distribution (NBD) describes well the multiplicity distribution of secondary particles in various rapidity windows and also in both the hemispheres. We have compared the NBD parameters, in both the hemispheres, at 200 GeV and 360 GeV, with those at 800 GeV. The behaviour of NBD parameters in rapidity windows of different widths and for different targets has also been studied. Received: 30 August 2001 / Accepted: 28 January 2002     

Determination of erosion rates with cosmic ray produced36Cl

We present results of the determination of³⁶C1 (T _1/2=3.0·10⁵a) in rock samples produced in situ by cosmic rays and natural radioactivities. These experiments were designed to determine the feasibility of using³⁶Cl for studying erosion processes in calcium rich minerals like limestone or dolomite. The³⁶Cl/Cl ratios in the samples have been determined with accelerator mass spectrometry (AMS) at the Munich accelerator laboratory. A first application is the investigation of the erosion in the last million years in Allchar (Yugoslavia) for the feasibility study of the geochemical²⁰⁵Tl solar neutrino experiment.Dedicated to Prof. Dr. P. Kienle on the occasion of his 60th birthday. Supported by DFG     

Predicted intensity of gamma rays from photonium

We have shown in a previous paper that stable electron-positron resonances (photonium) can account for the dark matter in the universe. In this paper we show that photonium in the galaxy will be dissociated by cosmic rays. We predict the intensity of the resulting 511 keV gamma rays as a test of the model. We find that the predictions exceed observations from the galactic center for model where the photonium has a similar distribution to the baryons. The predicted intensity is consistent with observations if the photonium is distributed in a large halo.One of us (JPV) acknowledges support from the U.S. Department of Energy under Grant DE-FG02-87ER40371, Division of High Energy and Nuclear Physics     

Variations of the flux and the energy spectrum of neutrons born in the galactic cosmic ray proton interactions with the matter of Earth''s satellites and orbital stations

This paper presents the energy spectra of secondary neutrons obtained from Monte Carlo simulations of the interactions of protons of galactic cosmic rays with the material of a spacecraft, and also the variation of the fluxes of these particles as a function of latitude. The variations of the secondary neutron flux with changing geometry and orientation of the craft, and detector position were evaluated as well. The simulations were conducted over a wide range of masses of spacecraft, from 300 kg (Earth Probe Total Ozone Mapping Spectrometer) to 420,000 kg (International Space Station in its full configuration), with calculations for the ISS also being carried out for its first development stage (mass of approx. 20,400 kg) and its configuration with a mass of approx. 81,000 kg. The calculations were carried out for circular orbits at altitudes of 500 km and for the energy intervals 0.001–10 MeV and 10–10,000 MeV, for both maximum and minimum solar activity. The results obtained agree reasonably well with results from previous calculations and do not contradict experimental data.     

Deuterons from 300 GeV proton collisions calculated from the Lund model

We present an alternative approach to describe deuteron production in high energy particle collisions. The phenomenological Lund-model has been used to give the number and momentum distribution of secondary nucleons produced in 300 GeV proton-proton collisions. Deuterons are assumed to be produced in a final state interaction between the nucleons inNN d reactions inside a volume of 1 F³. The results are compared to experimental data.Data became available for antideuteron production in e⁺e^– annihilation. * A Lund Monte Carlo calculation for the production of secondary nucleons in e⁺e^– collisions exist. The results from a final state interaction were too small by a factor 10³. A calculation for a coalescent model which uses the overlap of the proton-neutron momentum distribution with a distribution from a Hulthen wave function is in good agreement with the data. The coalescent model works well in this case. It is because the relative momentum of the coalescent nucleons produced for 10 GeV cm energy in e⁺e^– collisions is very much smaller than the relative momentum of the nucleons produced in 300 GeV fixed target energy ofpp collisions.     

Note on the impact parameter analysis of high-energy proton-proton collisions

Following a prior analysis of measured pp elastic differential cross-sections, the impact parameter representation in terms of profile functions is calculated from two different parametrizations of single diffractive dissociation data. The derivative of this quantity, with respect to the collision energy squared s, measures the growth rate of the reaction's blackness. Its distribution in impact parameter space allows detailed insight into the growth pattern of the total diffractive cross-section and the approaching unitarity limit. Comparing the results with the elastic case, the different mechanisms of unitarization of two parametrizations are discussed. Received: 19 January 2001 / Accepted: 11 July 2001