Constraints to the radiative lifetime of a light neutral fermion in the galactic halo from IUE

Summary We present the negative result of a search for the radiative decay of a light neutral fermion, that might be the neutrino (if massive) or the photino, gravitationally bounded to our Galaxy. The limit obtained for the radiative lifetime of a particle of mass between 12.5 and 21.5 eV is ≈10¹⁸ years. These new data on UV background in the range (1250÷2000) ? show the presence of continuum emission and diffuse lines emission at high galactic latitude (|b ^II|>45°). The lines are identifiable with C IV, λ-1549 ? and N III, λ=1749 ?. The continuum level sharply rises at 1680 ? to the level of (314±136) photons/(cm²s sr ?) and remains nearly constant up to 2000 Å. Below 1680 Å we found no emission with an upper limit of ≈100 units. These new data are briefly discussed in comparison with the results of previous experiments and theoretical expectations. Paper presented at the Congress ?Galactic and Extragalactic Dark Matter?, Roma, 28 to 30 June 1983.     

Diffuse galactic and extragalactic radiation in the far infra-red

Summary We present the results of a balloon flight devoted to the observation of the diffuse sky radiation in the wave-length region (150÷400) and (350÷3000) μm, at angular scales larger than six degrees. Observations of dust emission and distribution are discussed. Paper presented at the Congress ?Galactic and Extragalactic Dark Matter?, Roma, 28 to 30 June 1983.     

Search for WIMPs with enriched xenon at Gran Sasso

Summary A low-activity liquid-xenon scintillator is running at the Gran Sasso National Laboratory of INFN using liquid Kr-free xenon enriched at 99.5% in¹²⁹Xe. The result of adark matter direct search—looking also for the annual modulation effect—is presented. Preliminary exclusion plots both for coherent and spin-dependent coupled WIMPs are evaluated. The authors of this paper have agreed to not receive the proofs for correction.     

Response and yield functions of neutron monitor, galactic cosmic-ray spectrum and its solar modulation, derived from all the available world-wide surveys

Summary The differential response functionR(p, x, t) of cosmic-ray neutron monitors and its altitude and time dependence are obtained by a new method of analysis which uses all the available data obtained by oversea, overland and airborn surveys at different periods together with those of the space exploration. The simultaneous use of these data enables us to decomposeR(p, x, t) further into three terms; the unmodulated energy spectrumG(U) of galactic cosmic rays, the modulation functionM(p, t) of cosmic rays in solar system and the yield functionY(U, x) of neutrons in the atmosphere (x g/cm²). It is demonstrated that 1) the power exponent ofG(U) shows fairly a good agreement with those so far obtained, 2)Y(U, x) shows also fairly a good agreement with the theoretical expectation in the energy region ≥10 GeV and 3)M(p, t) gives the cosmic-ray mean free path showing a consistent rigidity spectrum with those obtained by the solar proton events. Using these terms, we can obtainR at any time and at any atmospheric depth. A brief historical review of the study of the response function is also made in the introduction.

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Riassunto La funzione di risposta differenzialeR(p,x,t) dei monitor a neutroni dei raggi cosmici e la sua dipendenza dall'altitudine e dal tempo sono ottenuti con un nuovo metodo di analisi che utilizza tutti i dati disponibili ottenuti con rilevamenti aerei, in mare e a terra effettuati in periodi diversi insieme ai dati delle esplorazioni spaziali. L'uso simultaneo di questi dati permette di scomporreR(p,x,t) ulteriormente in tre termini: lo spettro di energia non modulatoG(U) dei raggi cosmici galattici, la funzione di modulazioneM(p,t) dei raggi cosmici nel sistema solare e la funzione di produzioneY(U,x) di neutroni nell'atmosfera (x g/cm²). Si dimostra che 1) l'esponente della potenza diG(U) presenta un buon accordo con quelli ottenuti fino ad ora, 2)Y(U,x) presenta anche un buon accordo con i valori teorici attesi nella regione d'energia ≥10 GeV e 3)M(p,t) dà il percorso libero medio dei raggi cosmici che mostra un consistente spettro di rigidità ottenuto dagli eventi dei protoni solari. Usando questi termini, si può ottenereR in ogni momento e a tutte le profondità atmosferiche. Nell'introduzione c'è una breve rassegna storica dello studio della funzione di risposta.

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Резюме С помощью новочо метода анализа, который использует все имеющие данные мировых исследований в различные периоды вместе с данными космических исследований, получаются дифференциальная функция откликаR(p, x, t) для мониторов космических нейтронов и ее зависимость от высоты и времени. Одновременное испльзование этих данных позволяет нам представитьR(p, x, t) в виде трех членов: немодулированный энергетический спектрG(U) галактических космических лучей, функция модуляцииM(p, t) космических лучей в солнечной системе и функция выходаY(U, x) нейтронов в атмосфере (х·г/см²). Показывается, что 1) показатель экспонентыG(U) довольно хорошо согласуется с полученной величиной, 2)Y(U, x) также довольно хорошо согласуется с теоретическими предсказаниями в области энергий≽10 Гэв и 3)M(p, t) дает величину средней длины свободного пробега космических лучей, которая соответствует величине, полученной для солнечных протонов. Используя эти три члена, мы можем получитьR в любое время и на любой гдубине в атмосфере. Во введении предлагается краткий исторический обзор исследований функции отклика.

     

Search for UHE cosmic sources with a large-area underground muon detector

Summary The newly discovered gamma-ray emission from Cyg-X 3 with energies up to 2·10¹⁶eV gives the first evidence that particle acceleration in galactic gamma-ray sources can reach energies of the order of 10⁴ TeV. We discuss the detectability of this type of sources by an underground muon tracking detector with area of the order of ∼1000 m² and the physical information which could be obtained in this way. Paper presented at the 2° Convegno Nazionale di Fisica Cosmica, held at L'Aquila, 29 May–2 June 1984.     

Calculation of capture rates of solar and galactic neutrinos by69Ga and71Ga

Summary Calculations of the neutrino-capture cross sections for^69,71Ga based on a microscopic treatment of the Gamow-Teller matrix elements are presented. A strong enhancement of the cross-section for high-energetic neutrinos is found compared to previous phenomenological estimates. As a consequence the present assumptions on the signal from⁸B neutrinos in⁷¹Ga have to be revised. A rather large solar model dependent background of⁸B neutrinos has to be expected in a gallium solarneutrino experiment together with the pp signal. This will complicate the interpretation of such an experiment particularly in the case of neutrino oscillations with not maximum mixing angle. The calculations yield a larger sensitivity of the gallium detector than assumed previously for galactic neutrinos.

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Riassunto Si presentano i calcoli delle sezioni d'urto di cattura neutrinica per^69,71Ga basati su un trattamento microscopico degli elementi di matrice di Gamow-Teller. Si trova un forte aumento della sezione d'urto rispetto a stime fenomenologiche precedenti. Di conseguenza gli assunti attuali sul segnale dai neutrini⁸B in⁷¹Ga devono essere riveduti. Si prevede un sottofondo abbastanza grande, dipendente dal modello solare di neutrini di⁸B in un esperimento di neutrini solari di⁷¹Ga con il segnale pp. Ciò complicherà l'interpretazione di questo esperimento particolarmente nel caso di oscillazioni neutriniche con angolo di mescolamento non massimo. I calcoli danno una sensibilità maggiore del rivelatore di gallio rispetto a quanto precedentemente assunto per i neutrini galattici.

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Резюме Проводятся вычисления поперечных сечений захвата нейтрино в^69,71Ga на основе микроскопического рассмотрения матричных элементов Гамова-Теллера. Обнаружено сильное увеличение поперечного сечения для нейтрино высоких энергий по сравнению с предыдущими феноменологическими оценками. В рамках предложенного подхода заново определяется сигнал от⁸B-нейтрино в⁷¹Ga. Отмечается наличие довольно большого фона нейтрино. Это приводит к проблемам при интерпретации эксперимента с солнечными нейтрино в галлии в случае нейтринных осцилляций с немаксимальным углом смешивания. Вычисления приводят к большей чувствительности галлиевого детектора, чем предполагалось ранее для галактических нейтрино.

     

Evidence for an increasing 59 s period in the X-ray emission from Geminga

Summary Einstein Observatory and EXOSAT X-ray data from 1E0630+178 reveal a ∼50% periodic emission at ≳59s. This confirms the early SAS-II and COS-B findings on 2CG 195+04 atE>50 MeV and provides the temporal signature for the identification of Geminga. The observations, spanning over a decade (1973–1983), also suggest a very high positive which has become still higher in 1979–1983. The X-ray data used for this work have been collected in part during the Einstein Observatory Guest Observer Program and in part from the EXOSAT mission.     

Cosmic-muon results from the NUSEX experiment

Summary Muon underground data collected in the NUSEX experiment at Mont Blanc have been analysed concerning the following topics: I) vertical muon intensity, II) prompt muon flux, III) muons from the direction of Cygnus X-3. Preliminary results from the analysis of more than 20 000 muons are presented and discussed.

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Riassunto Gli eventi di muoni rivelati sottoterra nell'esperimento NUSEX al Monte Bianco sono stati analizzati per studiare I) l'intensità verticale dei muoni, II) il flusso di muoni pronti, III) l'eccesso di muoni dalla direzione di Cygnus X-3. In questo lavoro sono presentati c discussi i risultati preliminari ottenuti dal'lanalisi di piú di 20.000 eventi.

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Резюме Был проведен анализ данных, собранных в экспеимемнте NUSEX на Мон Блане. Анализировались следующие вопросы: 1) интенсивность вертикальных мюонов, 2) поток мгновенных (быстрых) мюонов, 3) мюоны, движущиеся в направлении от Лебедь X-3. Приводятся и обсуждаются предварительные результаты анализа для более, чем 20 000 муонов.

     

Derivation of the positron flux from the recent proton spectrum

Summary The energy spectrum of cosmic-ray positrons has been estimated by using precise CERN and Fermilab accelerator data for pp→π⁺X inclusive reactions and the latest primary nucleon spectrum based on the directly measured data. The derived positron spectrum has been found in accord with the positron flux data registered near the top of the atmosphere.

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Riassunto Lo spettro di energia dei positroni dei raggi cosmici è stato stimato usando dati precisi dell'acceleratore CERN e del Fermilab per le reazioni inclusive pp→π⁺X il piú recente spettro primario del nucleone basato su dati direttamente misurati. Lo spettro derivato del positrone è stato trovato in accordo con i dati del flusso di positroni registrato vicino alla parte piú alta dell'atmosfera.

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Резюме Оценивается энергетический спектр позитронов в космических лучах, используя ускорительные данные ЦЕРНа и лаборатории ферми для инклюзивных реакций pp→π⁺X и спектр первичных нуклонов, полученный из непосредственно измеренных данных. Получено, что вычисленный позитронный спектр согласуется с данными для позитронного потока, зарегистрированными вблизи верхней границы атмосферы.

     

Bounds on the neutrino mass from the dark matter in the universe

Summary The problem of the missing matter in the Universe is reviewed and discussed in terms of massive neutrinos. The primordial abundances of light elements produced during the big bang nucleosynthesis can be used to determine firm bounds on the number of neutrino flavours and on the ratio of baryon to photon densities in the Universe. These limits imply that nonbaryonic matter is the dominant constituent of large-scale cosmic structures, being massive neutrinos the best guess for such a matter. In order that the Universe be closed, a value of the neutrino rest mass is derived, which agrees with the bounds obtained from the dynamics of galaxies and clusters of galaxies. It is also shown that density perturbations can hardly grow in a nucleon-dominated Universe, and massive neutrinos may be the seed for nucleon condensations. All these astrophysical and cosmological considerations suggest a lower and an upper bound of the neutrino rest mass. Paper presented at the Congress ?Galactic and Extragalactic Dark Matter?, Roma, 28 to 30 June 1983.     

Radiation from Cygnus X-3 and the related muon puzzle—An explanation

Summary In recent times there have been widespread speculations and claims among the cosmic-ray as well as high-energy physicists about the detection of some ?signatures? for the formation of what one calls the quark-gluon plasma states in the ultrahigh-energy cosmic-ray collisions involving heavy nuclei. Furthermore, there are reportedly some hints to the detection of such states in laboratory experiments as well. We have collected here what are, in general, believed to be the diagnostics for such quark-gluon plasma states and have also provided alternative explanations for all the relevant observations at laboratory energies and cosmic-ray energies. Thus the obvious conclusion is: the evidences claimed so far are neither unique and decisive nor are very substantial, tenable and conclusive, as one can understand them almost completely from an altogether different theoretical framework.

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Riassunto In tempi recenti vi sono state diffuse ipotesi ed affermazioni tra i fisici che si occupano dei raggi cosmici e dell'alta energia sulla scoperta di alcune ?impronte? per la formazione di quelli che si chiamano stati di plasma tra quark e gluoni in collisioni di raggi cosmici ad energia ultra alta che coinvolgono nuclei pesanti. Inoltre vi sono alcuni indizi a quanto viene riferito per la rivelazioni di questi stati anche negli esperimenti di laboratorio. Qui abbiamo raccolto quella che è in generale ritenuta la diagnostica per questi stati di plasma fra quark e gluoni ed abbiamo inoltre fornito spiegazioni alternative per tutte le osservazioni relative ad energie di laboratorio ed energie di raggi cosmici. Cosí la conclusione ovvia è: le prove non si sono dimostrate né uniche e decisive, né importanti, sostenibili e conclusive, come le si può ritenere quasi completamente da un modello teorico completamente diverso.

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Резюме В последнее время в физике космических лучей и физике высоких энергий интенсивно обсуждается вопрос детектирования некоторых ?сигнатур? для образования так называемых состояний кварк-глюонной плазмы при соударениях космических частиц ультравысоких энергий, включая тяжелые ядра. Более того, были также публикации о предлагаемом детектировании таких состояний в лабораторных экспериментах. В этой работе анализируется диагностика таких состояний кварк-глюонной плазмы, а также предлагаются альтернативные объяснения всех имеющихся наблюдений при лабораторных и космических энергиях. На основе анализа делается очевидный вывод: данные наблюденй пока не являются достаточными, чтобы их можно было бы понять из полностью друтих теоретических подходов.

     

Neutrinos from gravitational collapse

Summary A review is made of neutrino fluxes produced by gravitational collapse events (type-II supernovae?). Recent work of Mayle, Wilson and Schramm is used to examine those aspects of neutrino signal which are relatively independent of the collapse model and those aspects which are sensitive to model details. A discussion of the antineutrino background from the integral of all collapse events is also presented.

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Riassunto Si esaminano i flussi di neutrini prodotti da eventi di collasso gravitazionale (supernovae di tipo II?). Si usa il lavoro recente di Mayle, Wilson e Schramm per esaminare quegli aspetti del segnale del neutrino che sono relativamente indipendenti dal modello del collasso e quegli aspetti che sono sensibili ai dettagli del modello. Si presenta anche una discussione del background di antineutrini dall'integrale di tutti gli eventi di collasso.

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Резюме Анализируются нейтринные потоки, образованные в результате гравитационного коллапса. Недавняя табота Мейла, Вильсона и Шрамма используется для изучения таких аспектов нейтринного сигнала, которые не зависят от модели коллапса, а также таких аспектов, которые являются чувствительными к деталям модели. Проводится обсужление фона анти-нейтрино, исходя из интеграла всех событий коллапса.

     

High-energy multiple muons viewed from the observation of gamma-ray families at mountain altitudes

Summary Based on the knowledge of the nature of primary cosmic rays inferred from the observations of gamma-ray family events with the largescale emulsion chamber experiments at Mt. Fuji and at Mt. Kanbala, the three-dimensional Monte Carlo simulation on the high-energy multiple-muon events has been carried out. By comparing the simulation results with the presently available observed ones, it is concluded that the hypothesis for the composition of primary cosmic rays being heavy-nuclei dominant, given from the analysis of gamma-ray family events, is quite consistent with the observed results on the lateral spread of multiple-muon events.

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Riassunto Si effettua la simulazione di Monte Carlo tridimensionale sugli eventi di muoni multipli ad alta energia, basandosi sulla conoscenza della natura dei raggi cosmici primari inferita dalle osservazioni degli eventi della famiglia di raggi gamma con gli esperimenti su larga scala della camera ad emulsione sul Monte Fuji e sul Monte Kanbala. Confrontando i risultati della simulazione con quelli osservati attualmente disponibili, si conclude che l'ipotesi della composizione dei raggi cosmici primari in cui predominano i nuclei pesanti, data dall'analisi degli eventi della famiglia di raggi gamma, risulta del tutto coerente con i risultati osservati sulla diffusione laterale degli eventi a muoni multipli.

     

Neutrino emission from collapsed objects

Summary The possible emission fluxes from the matter spherically accreting onto a massive object (Schwarzschild black hole) are discussed. Assuming that the observed high-energy gamma-rays from point sources have hadronic origin, we evaluate the expected neutrino flux from the quasar 3C 273 and from galactic centre. We can say that the accretion process onto a massive object produces neutrinos in the low-energy regin (≈15 MeV).

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Riassunto In questo lavoro si discutono i possibili flussi emessi dalla materia che si accresce sfericamente su un oggetto massiccio (buco nero di Schwarzschild). Assumendo che i raggi gamma di alta energia provenienti da sorgenti puntiformi abbiano origine adronica, noi valutiamo il flusso aspettato di neutrini dal quasar 3C 273 e dal Centro Galattico. Possiamo dire che processi di accrescimento su oggetti massicci producono neutrini nella regione di bassa energia (≈15 MeV).

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Резюме Обсуждаются возможмые потоки излучения от вешества, сферически аккретирующего на массивный обьект (черная дыра Шваршильда). Предполагая, что наблюдаемые гамма-лучи высокой энергии от точечных источников имеют адронное происхождение, мы оцениваем ожидаемый поток нейтрино от квазара 3C 273 и от центра Галактики. Можно сказать, что процесс аккреции на массивный обьект образует нейтрино в области низких энергий (≈15 МэВ).

     

Charm hadroproduction cross-section up to 100 TeV from measurements of the cosmic-ray muon angular distribution. Results of the Mont Blanc experiment

Summary Accurate calculations of the angular distributions of underground conventional and prompt muons have been performed. The dependence of the angular enhancement functions on the primary spectrum, cross-sections, inclusive distributions, K/π ratio and survival probability have been studied and found to be negligible. The results have been used to interpret the data from the Mont Blanc experiment in the depth range (4200ρ5800) hg/cm². Since the measurements extend over a limited angular range (<60°) the ratio between the flux of prompt to conventional muons of higher energy (>1 TeV) is obtained with large associated statistical errors. In order to obtain the charm production cross-section in the energy region (50ρ100) TeV, accurate measurements over a very large angular range (>70°) at depths higher than 5000 hg/cm² are required.

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Riassunto Sono state calcolate le distribuzioni angolari di muoni convenzionali e pronti sottoterra ed è stata studiata la loro dipendenza, risultata trascurabile, dalla forma dello spettro primario, sezione d'urto, distribuzioni inclusive, rapporto di produzione K/π e probabilità di sopravvivenza. Questi risultati sono stati usati per interpretare i dati ottenuti nell'esperimento del Monte Bianco nell'intervallo di profondità (4200ρ5800) hg/cm². Poiché le misure si estendono solo sino a 60° il rapporto tra muoni pronti e convenzionali di alta energia (>1 TeV) è ottenuto con grande errore statistico. Se ne conclude che per derivare la sezione d'urto di produzione di charm nell'intervallo di energia (50ρ100) TeV sono necessarie misure accurate ad alta profondità (>5000 hg/cm²) ed estese sino ad oltre 70°.

     

Calculation of muon range spectrum under sea-water from the latest JACEE primary spectrum using the modified energy loss formulation after Kobayakawa

Summary The muon range spectrum under sea-water has been estimated from the latest primary nucleon spectrum based on JACEE measurements. The hadronic-energy moments for p-nucleus collisions have been used for the calculation of meson production spectrum. The latest modified range-energy relation after Kobayakawa has been applied for the conversion of muon energy spectrum at sea-level to depth-intensity spectrum under sea. The calculated result has been compared with the measured data after Higashiet al., Davitaevet al. and Rogers and Tristam.

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Riassunto Si stima lo spettro dell'intervallo muonico sott'acqua dal piú recente spettro nucleonico delle primarie basandosi su misure JACEE. Si utilizzano i momenti di energia adronica nelle collisioni p-nucleo per il calcolo dello spettro di produzione mesonica. La piú recente relazione modificata tra intervallo ed energia secondo Kobayakawa è stata applicata per la conversione dello spettro d'energia muonica a livello del mare, allo spettro di profondità-intensità nel mare. I risultati calcolati sono stati confrontati con i dati misurati da Higashiet al., Davitaevet al. e Rogers e Tristam.

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Резюме На основе JACEE измерений оценивается спектр пробегов мюонов в слое морской воды, исходя из последнего первичного нуклонного спектра. Для расчета спектра рождения мезонов были использованы моменты энергии адронов при соударения протонов с ядрами. Новейшая модификация соотношения пробегзнергия, предложенная Кобайакавой, применяется для преобразования энергетического спектра мюонов на уровне моря в спектр под водой. Полученные результаты сравниваются с экспериментальными результатами Хигаши и др., Давитаева и др., и Роджерса и Тристана.

     

Neutrino detection at large distances from accelerators

Summary Fluxes and spectra of muon and hadron showers from neutrinos from an accelerator are calculated far from this accelerator. Decays of π⁺-, K⁺-mesons and charmed particles generated in nuclear interactions of protons are taken as neutrino sources. The calculations are made for different proton energies. At high energies muon and hadron shower fluxes from neutrinos from charmed particles begin to be equal and then tend to exceed the corresponding fluxes from neutrinos from pions and kaons. For a more correct knowledge of the neutrino flux it is useful to measure the depth-intensity curve for muons near the accelerator. The possibility of muon and hadron shower detection with small and ?DUMAND?-type installations is considered. The problem about whether we can use neutrinos from an accelerator and cosmic-ray neutrinos to study the Earth's interior is discussed. Remarks are made on the questions of the search of elements with highZ with neutrinos from accelerators and of energy depositions of these neutrinos in their path through the Earth matter.

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Riassunto I flussi e gli spettri degli sciami muonici e adronici dai neutrini di un acceleratore sono calcolati lontano da questo acceleratore. I decadimenti dei mesoni π⁺ e K⁺ e delle particelle con charm generate in interazioni nucleari di protoni sono considerati come sorgente di neutrini. Si effettuano i calcoli per diverse energie protoniche. Ad alte energie i flussi degli sciami adronici e muonici dai neutrini che derivano dalle particelle con charm cominciano ad essere uguali e in seguito ad essere maggiori dei flussi corrispondenti dervanti dai neutrini che derivano dai pioni e dai kaoni. Per una conoscenza piú corretta del flusso dei neutrini è utile misurare la curva profondità-intensità per muoni vicino all'acceleratore. Si considerano le possibilità di rilevare sciami muonici e adronici con installazioni piccole e di tipo DUMAND. Si discute il problema di poter usare neutrini di un acceleratore e neutrini dei raggi cosmici per studiare l'interno della Terra. Si fanno alcuni commenti sul problema della ricerca di elementi conZ grande con neutrini di acceleratori e sulla deposizione d'energia di questi neutrini durante il loro passaggio attraverso la materia terrestre.

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Резюме Вычислены потоки и спектры мюонов и адронных ливней от нейтрино от ускорителей на больших расстояниях от этих ускорителей. Как источники нейтрино рассмотрены распады π⁺-, K⁺-мезонов и чармированных частиц, генерируемых в ядерных взаимодействиях протонов. Вычисления проведены для различных энергий протонов. При высоких энергиях потоки мюонов и адронных ливней от нейтрино от чармированных частиц начинают сравниваться, а потом и превосходить соответствующие потоки от нейтрино от пионов и каонов. Для более точного знания потоков нейтрино, идущих от ускорителя, полезно измерять вблизи ускорителя кривую глубина-интенсивность для мюонов. Рассматриваются возможности детектирования мюнов и адронных ливней от нейтрино от ускорителей на больших расстояниях небольшими установками и установкми типа ДЮМАНД. Обсуждаются возможности использования нейтрино от ускорителей и нейтрино космических лучей для изучения внутреннего строения Земли. Сделаны небольшие замечания к вопросу о поиске с помощью нейтрино от ускорителей элементов с большимZ и к вопросу об энерговыделениях этих нейтрино вдоль пути их прохождения через вещество Земли.

     

Cosmic-ray low-energy abundances from calcium to nickel

Summary We have measured the elemental composition and mean masses of the cosmic rays from calcium to nickel using a Lexan polycarbonate stack exposed in a balloon flight. We obtain a 3% charge resolution for iron at an energy interval of (255÷545) MeV/nucleon at the top of the atmosphere. We have propagated the spectrum measured through the detector, the residual atmosphere, the solar cavity and the interstellar medium, obtaining the composition at sources with a 7% resolution for iron. We observe that it is not possible to resolve adjacent isotopes with the Lexan polycarbonate.     

Estimation of elemental abundances of heavy cosmic-ray primaries at the top of the atmosphere using plastic emulsion chamber and the derived source spectrum from the steady-state leaky box model

Summary Final results of the experiment for the estimation of charge abundances using plastic emulsion chamber consisting of CR-39 (HCB) and Fuji ET-7B nuclear-emulsion sheet, launched from Alice Springs for 32 hours at an atmospheric depth of 9.8 g cm⁻² is presented. The latest long hour etching technique was used for track detection in plastics. The estimated reduced etch rate distribution presented was based on 2968 measured track diameter data in CR-39 (HCB) stacks. The observed charge spectrum from the reduced etch rate distribution was duly corrected for the top of the atmosphere by adopting the conventional formulation for cosmic-ray propagation along with the latest modified partial cross-sections for A-A collisions after Tsaoet al. The average value of the observed energy of the 77 very heavy primaries was estimated from the opening angle measurements of alpha fragments in Fuji ET-7B nuclear emulsion and was found to be 5.01 GeV/n which comes out to be 8.2 GeV/n, when corrected for the top of the atmosphere due to propagation in the residual atmospheric depth. The measured integral fluxes for NeMgSi and Fe groups above 4 GeV/n have been compared with the global data surveyed by Ichimuraet al. Our results on element/Si and element/Fe have been compared with the HEAO-3-C2 data after Englemannet al. Using SSLB model, the source abundance is derived from the observed result and that was compared with the results of Juliusson,et al., Lezniak and Webber and Garcia-Munozet al.     

High-energy neutrino emission from binary X-ray sources

Summary Recently γ-rays up to 10¹⁶ eV were observed from Cyg X3, Vela X1 and LMC X4. This is a strong indication that protons (or nuclei) are accelerated in the vicinity of the accreting pulsar. We discuss in this paper the production of high-energy neutrinos associated with the γ-ray production. We show that on the basis of observational parameters of the three binary systems, the time average of the ratio of the neutrino luminosity to the γ-ray luninosity will beL _ν/L_γ∼30. The neutrino flux will be modulated with the orbital period of the system and the neutrino light curve will be determined by the density profile of the companion star. In general some of the X-ray binaries can be both UHE γ-ray and neutrino emitters with a neutrino luminosity comparable to their X-ray luminosity. The brightest of these could be detected by future neutrino telescopes such as DUMAND and MACRO at Gran Sasso.

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Riassunto Recentemente è stata rivelata emissione di raggi gamma con energia sino a 10¹⁶eV da Cyg X3, Vela X1 ed LMC X4. Questa osservazione indica che protoni (o nuclei) sono accelerati nella vicinanza della pulsar contenuta in questi tre sistemi binari. In questo lavoro si calcola la produzione di neutrini di alta energia, associata alla produzione di raggi gamma. Il risultato ottenuto è che, tenendo conto dei parametri dedotti dalle osservazioni spettroscopiche dei tre sistemi considerati, il rapporto tra la luminosità in neutrini e la luminosità gamma èL _ν/L_γ∼30. Inoltre il flusso di neutrini sarà modulato con il periodo binario del sistema e la curva di luce dei neutrini sarà determinata dalla distribuzione di densità della stella compagna. In generale alcune delle binarie X possono essere sorgenti sia di gamma di altissima energia che di neutrini, con una luminosità in neutrini paragonabile alla luminosità in raggi X. Le piú intense tra queste potranno essere osservate da futuri telescopi per neutrini come DUMAND o MACRO.

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Резюме Недавно γ-кванты с энергиями вплоть до 10¹⁶ эВ наблюдались из Cyg X3, Vela X1 и LMC X4. Это является указанием, что протоны (или ядра) ускоряются в окрестности аккретирующего пульсара. Мы обсуждаем в этой статье образование высокоэнергетичных нейтрино, которые связано с рождением γ-квантов. Мы показываем, что на основе наблюденных параметров для трех бинарных сйстем среднее по времени отношение интенсивности испускания нейтрино к интенсивности испускания γ-квантов составляетL _ν/L_μ∼30. Модуляция потока нейтрино определяется орбитальным периодом системы, а кривая яркости нейтрино определяется профилем плотности сопутствующей звезды. Обычно ренттеновские бинарные системы могут представлять источники γ-квантов сверхвысоких энергий и источники нейтрино, причем интенсивность испускания нейтрино сопоставима с интенсивностью рентгеновского излучения. Наиболее яркие из них могут быть зарегистрированы в будущем с помощью нейтринных телескопов, таких как DUMAND и MACRO в Гран Сассо.