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.

     

No sign of cosmic-ray generation from Jupiter, detectable at ground-based stations

Summary By using thirteen years of cosmic-ray data from the muon telescope at Nagoya and the neutron monitor at Kiel, it is demonstrated that Jupiter is not the source of the cosmic rays observable at the ground-based stations, contrary to the recent suggestion by Mitraet al.

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Riassunto Usando i dati di tredici anni di raggi cosmici del telescopio muonico a Nagoya e del monitor a neutroni di Kiel, si dimostra che Giove non è la sorgente di raggi cosmici osservabili in stazioni terrestri, contrariamente alla recente ipotesi di Mitraet al.

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Резюме Используя данные за тридцать лет с мюонного телескопа в Нагойе и с нейтронного монитора в Киле, показывается, что юпитер не является источником космических лучей, детектируемых наземными станциями, в противоположносстщ недавнему предположению, высказвнному Митра и др.

     

Formulation of cosmic-ray solar daily variation and its seasonal variation, produced from generalized stationary anisotropy of solar origin

Summary In previous papers, we presented a formulation of the cosmic-ray solar daily variation and of its seasonal variation, produced from an axis-symmetric stationary anisotropy of solar origin. On the other hand, based on their theoretical study of cosmic-ray diffusionconvection in the solar system, Munakata and Nagashima have recently pointed out the existence of an axis-asymmetric anisotropy with respect to the IMF axis, which is not covered by the formulation. In order to include such a case, we extend, in this paper, the above formulation to a case of a generalized anisotropy, which is expressed by surface harmonics in the IMF polar-co-ordinate system.

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Riassunto In precedenti lavori abbiamo presentato una formulazione della variazione diurna solare dei raggi cosmici e della sua variazione stagionale, prodotta da un'anisotropia stazionaria assi-simmetrica di origine solare. D'altra parte, basandosi sui loro studi teorici della diffusione-convezione dei raggi cosmici nel sistema solare, Munakata e Nagashima hanno recentemente messo in evidenza l'esistenza di un'anisotropia assisimmetrica rispetto all'asse IMF che non è compresa nella formulazione. Per poter includere anche tale caso, abbiamo esteso, in questo lavoro, la suddetta formulazione al caso di un'anisotropia generalizzata che è espressa da armoniche di superficie nel sistema di coordinate polari IMF.

     

Application of solar arrays in high-energy gamma-ray astronomy

Summary The previously suggested use of large solar-energy arrays for additional applications in astronomy and astrophysics is herein analysed for the case of high-energy gamma-ray astronomy. We have studied by Monte Carlo techniques the response of an array of 800 m² reflective area to the Čerenkov light produced by relativistic electrons of high-energy cascades, initiated by primary cosmic rays (gamma-rays and protons) in the Earth's atmosphere. The calculation shows that night-time use of these devices may give information on the study of gamma-ray sources which is consistent with the results obtained from specific apparatuses, from the point of view of both energy threshold and detectable fluxes. This result confirms the possibility of designing multiscope arrays operating daily as solar-energy collectors and at night-time as cosmic gamma-ray detectors, with obvious advantages from the financial point of view.

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Riassunto Si analizza la possibile utilizzazione dei campi eliostatici per applicazioni di tipo astrofisico nel caso dell'astronomia gamma di alta energia. Le prestazioni di un apparato con superficie riflettente di 800 m² come raccoglitore della luce Čerenkov emessa dagli elettroni relativistici di sciami estesi atmosferici (EAS) sono state studiate con un metodo di Montecarlo. I calcoli mostrano che l'uso notturno di questo sistema per la ricerca di sorgenti gamma può fornire risultati confrontabili con quelli ottenuti da apparati specifici, sia per quanto riguarda la soglia di rivelazione (E _s<100 GeV) che i flussi rivelabili. Dati gli ovvi vantaggi di tipo economico, questo risultato suggerisce la possibilità di progettare gli apparati in modo multiuso, cioè tali da poter operare come collettori solari nelle ore diurne e come rivelatori di EAS in quelle notturne.

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Резюме В этой работе анализируется применение больших солнечных антенных решеток для случая гамма-астрономии высоких энергий. Мы исследуем с помощью метода Монте-Карло отклик антенной решетки 800 м² на черенковское излучение, образованное релятивистскими электронами в широких атмосферных ливнях. Вычисления показывают, что использование таких приборов в ночное время может дать информацию об источниках гамма-лучей, которая согласуется с результатами, полученными с помощью специальной аппаратуры, с точки зрения энергетического порогаE _s<100 ГэВ и с точки зрения детектируемых потоков. Этот результат подтверждает возможность многоцелевого использования антенных решеток; в дневное время как коллекторов солнечной энергии, а в ночное время как детекторов космических гамма-лучей.

     

Solar neutrinos, the presolar abundance of helium and the solar metallicity

Summary The observational estimates of the presolar abundance of helium (Y _s) are reviewed and a lower value ofY _s ({-0.19 by mass fraction) is suggested to solve the solar-neutrino problem. With this reduced value ofY _s it is argued from the point of view of maintaining the luminosity of the Sun at its observed level that the metallicity requirement isZ _s{-0.013. Previous workers, while considering lowerY _s in the range of 0.15÷0.20, have assumedZ _s in the range of either 0.018÷0.020 or 0.001÷0.004. We suggest that forY _s=0.15÷0.20, one should rather considerZ _s=0.01÷0.02 in order to obtain a global solution that explains the observed modes of solar oscillation as well as the observed neutrino flux. This solution is quite interesting as we find that the real uncertainties in the determination of the solar metallicity arising from the diversity in existing models of the solar atmosphere suggestZ _s{-{0.018±0.005.

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Riassunto Si esaminano le stime di osservazione dell'abbondanza presolare di elio (Y _s) e si sugge risce un valore diY _s inferiore ({-0.19 in posizione di massa) per risolvere il problema dei neutrini solari. Con questo valore ridotto diY _s si deduce dal punto di vista di mantenere la luminosità del Sole al livello osservato che il requisito di metallicità èZ _s=0.013. Alcuni ricercatori in precedenza, considerando unY _s inferiore, nell'intervallo 0.15÷0.20, hanno ipotizzato cheZ _s si trovi nell'intervallo 0.018÷0.020 o 0.001÷0.004. Si suggerisce che perY _s=0.15÷0.20, si dovrebbe piuttosto considerareZ _s=0.01÷0.02 per ottenere una soluzione globale che spieghi i modi osservati di oscillazione solare cosí come il flusso di neutrini osservato. Questa soluzione è piuttosto interessante poiché si trova che le incertezze reali nella determinazione della metallicità solare che derivano dalla diversità in modelli esistenti dell'atmosfera solare suggeriscono cheZ _s{-0.018±0.005.

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Резюме Предлагается обзор оценок распространенности гелия на солнце (Y _s). Предполагается, что низшая величинаY _s ({-0.19 массовой доли) решает проблему солнечных нейтрино. Эта величинаY _s приводит к требованию металлических свойствZ _s{-0.013. В предыдущих работах, где рассматривалась меньшая величинаY _s в области 0.15÷0.020, предполагалось, чтоZ _s находится либо в области 0.018÷0.020, либо в области 0.001÷0.004. Мы предполагаем, что дляY _s=0.15÷0.20 следует принятьZ _s в областиZ _s=0.01÷0.02, чтобы получить глобальное решение, которое объясняет наблюдаемые моды солнечных осцилляций и наблюдаемый поток нейтрино. Это решение представляет интерес, т.к. мы получаем, что реальные неопределенности при определении металлических свойств солннца, обусловленные разбросом существующих модей солнечной атмосферы, предлагают, чтоZ _s{-0.18±0.005.

     

Detection of magnetic monopoles with superheated type-I superconductors

Summary We present a proposal to detect magnetic monopoles with a suspension of metastable superconducting granules. The method is independent of the speed of the monopole, and provides timing and tracking information. The speed and direction of the monopole can be determined with good accuracy. The electronic signal exceeds by two orders of magnitude that of induction experiments, and conventional electronics can be used. As a consequence, large-area detectors can be built at a reasonable cost. The physical principle of detection uses a specific effect associated to the magnetic charge in the static limit. Therefore, the monopole signal cannot be faked by any charged particle. This provides a very high background rejection. We discuss the present status of the project, as well as some of the main technical problems.

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Riassunto Si presenta un progetto per rilevare i monopoli magnetici con una sospensione di granuli metastabili superconduttori. Il metodo è indipendente dalla velocità del monopolo e formisce informazioni sul tempo e sulla traccia. La velocità e la direzione del monopolo si possono determinare con buona accuratezza. Il segnale elettronico eccede di due ordini di grandezza quello degli esperimenti d'induzione, e si può usare l'elettronica convenzionale. Di conseguenza i rivelatori di grande superficie si possono costruire con un costo ragionevole. Il principio fisico dela rilevazione usa un effetto specifico associato alla carica magnetica nel limite statico. Perciò il segnale del monopolo non può essere alterato da una particella carica. Ciò produce una grande reiezione di sfondo. Si discute lo stato attuale del progetto e alcuni dei principali problemi tecnici.

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Резюме Предлагается метод детектирования магнитных монополей с помощью суспензии метастабильных сверхпроводящих гранул. Этот метод не зависит от скорости монополя, дает временную и пространственную информацпю. Скорость и направление движения монополя могут быть определены с хорошей точностью. Электронный сигнал на два порядка превышает сигнал в экспериментах по индукции, поэтому может быть использована обычная электроника и сооружение детекторов на большой площади может быть осуществлено при разумных затратах. Физический принцип детектирования использует эффект, связанный с магнитным зарядом в статистическом пределе. Следовательно, сигнал от монополя нельзя спутать с сигналом от любой заряженной частицы. Зто обстоятельство позволяет устранить очень высокий уровень шума. Обсуждаются современное состояние проекта, а также основные технические проблемы.

     

Detection of EAS ?erenkov light reflected from mountain snow

Summary Fast (typical duration (400÷500) ns) light pulses are detected pointing three mirrors at a snowy mountain surface. The characteristics of the pulses are in agreement with expectations from EAS Čerenkov light reflected from the snow. The technique can be applied to the study of the cosmic-ray primary spectrum at high energies.

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Riassunto Si sono rivelati impulsi luminosi di durata tipica (400÷500) ns orientando tre specchi verso una regione innevata in alta montagna. Le caratteristiche dei segnali sono in accordo con quanto atteso per impulsi di luce Čerenkov da EAS riflessi dalla neve. La tecnica può essere utilizzata per lo studio dello spettro primario dei raggi cosmici alle alte energie.

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Резюме Детектируются световые импульсы с типичной длительностью (400÷500) нс, ориентируя три зеркала на поверхность горных снегов. Характеристики импульсов согласуются с предсказаниями для Черенковского излучения широких атмосферных ливней, отраженного от снега. Предложенная техника может быть использована для изучения первичного спектра космических лучей при высоких энергиях.

     

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.

     

Detection of coherent elastic neutrino scattering on nuclei, a status report for a detector development based on metastable superconductors

Summary Coherent elastic neutrino scattering on nuclei can only be detected via the recoil energy of the nucleus. We try to develop a detector based on metastable superconducting grains to detect these small recoil energies. Experiments testing some fundamental properties of a detector using metastable Sn and Cd grains are presented. In the case of Cd a sensitivity of at least 24 eV/μm³ (normalized to the volume of the grains) was achieved. We expect a still higher sensitivity if superconductors with very lowT _c are used and the quality of the grains (sphericity, size distribution, solid state properties) is improved.

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Riassunto Lo scattering elastico coerente di neutrini su nuclei si può rilevare solo attraverso l'energia di rinculo del nucleo. Si cerca di mettere a punto un rivelatore basato su grani metastabili superconduttori per rilevare queste piccole energie di rinculo. Si presentano esperimenti per saggiare alcune proprietà fondamentali di questo rivelatore usando grani metastabili Sn e Cd. Nel caso di Cd è stata raggiunta una sensibilità di almeno 24 eV/μm⁶ (normalizzata al volume dei grani). Si prevede una sensibilità ancora piú grande se si usano superconduttori conT _c molto bassa e si migliora la qualità dei grani (sfericità, distribuzione di volume, proprietà dello stato solido).

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Резюме Когерентное упругоерассеяние нейтрино на ядрах может быть зарегистрировано только с помоцью энергии отдачи ядра. Мы предлагаем детектирующую систему, основанную на метастабильных сверхпроводящих зернах, чтобы зарегистрировать эти малые энергии отдачи. Предлагаются эксперименты для проверки некоторых фундаментальных свойств такого детектора, с использованием метастабильных зерен Sn и Cd. В случае Cd может быть достигнута чувствительность 24 эВ/(мкм)³ (нормированная на объем зерна). Мы ожидаем еще большую чувствительность, если использовать сверхпроводники с очень низкойT _c и улучшить качество зерен (сферичность, распределение по размерам, твердотельные свойства).

     

Cosmic-ray neutron spectrometry by solid state detectors

Extensive data have been gathered since the early 1990s on the response of different detectors based on the registration of neutron-induced fission in bismuth, gold, tantalum by the spark replica counter and the thin film breakdown counter. These detectors make it possible to exploit the excellent characteristics of the fission reactions in bismuth, gold and tantalum for the measurements of high-energy neutrons.

Most of the investigations have been carried out at the quasi-monoenergetic neutron beam facility at The Svedberg Laboratory-TSL of the Uppsala University in cooperation with the Khlopin Radium Institute (KRI).

The responses of different fission detectors in the intermediate range of neutron energy (35–180 MeV) have been evaluated: a region where the predictive power of available nuclear reaction models and codes is not reliable yet. For neutron energy greater than 200 MeV, the fission-detector responses have been derived from the data of the proton fission cross-sections.

Finally, by using the ratio of the responses of these detectors, a simple and accurate way to evaluate the spectrum hardness can be obtained, thus providing a tool to obtain spectral information needed for neutron dosimetry without the need to know the entire spectrum.

The experimentally measured spectra obtained to-date have different shapes and they are also different from those calculated.

In this paper, a new approach will be reported to analyse the existing spectra by using response ratios of different detectors. Preliminary data have been already obtained for the high-energy neutron spectrum from the CERN concrete facility.     

Low-energy gamma-ray sources observed by the MISO telescope

Summary The MISO telescope is a gamma-ray detector operating in the (0.1÷20) MeV energy range. This instrument was flown success-fully from Palestine, Texas (U.S.A.) in May 1977, October 1978, September 1979 and May 1980. During the four flights, the telescope observed a number of galactic and extragalactic sources. The Crab Nebula was detected in 1980 and its spectrum was measured up to 2 MeV. Cygnus X-1 was observed in 1979 and 1980 and was found to be in different hard X-ray states on each occasion: in a superlow state in 1979 and in a low state in 1980. The COS-B high-energy (E>50 MeV) gamma-ray sources CG 135+1 (1978) and CG 195+4 (1978) were also observed by the same instrument. From the region containing CG 135+1 a 5σ excess was measured in the counting rate of the telescope above 120 keV. No statistically significant low-energy gamma-ray flux was detected from CG 195+4. The Seyfert galaxies NCG 4151 (1977, 1979, 1980), and MCG 8-11-11 (1979), the BL LAC object MK 501 (1979) and the ?peculiar? galaxy NGC 1275 (1979) were also searched for gamma-ray emission. The data on NGC 4151 and MCG 8-11-11 are consistent with power law spectra having photon indices α∼1 in the (0.1÷3) MeV energy range. Above this energy, the MISO and SAS-2/COS-B measurements require spectral breaks to α≥3. Upper limits were obtained on the emission from both MK 501 and NGC 1275. Paper presented at the 2° Convegno Nazionale di Fisica Cosmica, held at L'Aquila, 29 May–2 June 1984.     

Hadrons and other secondaries generated by cosmic-ray muons underground

Summary The production of nuclear-active and electromagnetic particles, as well as long-lived isotopes in nuclear and electromagnetic showers generated by cosmic-ray muons at different depths underground is discussed. Characteristics of the secondary components and their dependence on the depth and the muon energy, obtained in experiments and calculations, are presented.     

The ground-level cosmic-ray event of September 29, 1989 as recorded by the rome detectors

Summary An extraordinary increase in cosmic-ray intensity has been recorded on September 29, 1989 by the Rome detectors (rigidity threshold ∼6.2 GV). We show the time evolution of the event as recorded at Rome in the nucleonic component and in the total ionizing and muon components; as well as at Campo Imperatore (2300 m a.s.l. near Rome) in the nucleonic component by a special monitor designed for the detection of solar-neutron events. The one-minute time resolution of the Campo Imperatore data offers the possibility to follow in detail the development of the event for most of the time. The possible contribution of solar neutrons to the early phase of the Campo Imperatore event has been not clarified so far, further results may be obtained by the analysis of the multiplicity data registered in the event.     

The behaviour of the cosmic-ray equatorial anisotropy inside fast solar-wind streams ejected by coronal holes

Summary The cosmic-ray equatorial anisotropy inside broad high-speed solar-wind streams ejected by coronal holes,i.e. in quasi-stationary condition, is analysed over the years 1973–1974. From the beginning to the end of the stream the amplitudes of the first and second harmonics of the anisotropy are found to decrease remarkably by factors 2.5 and 2.0, respectively, while the phases do not show systematic variations. The development of the stream structure in the interplanetary space together with the Parker theory on the diurnal anisotropy in stationary condition give a plausible explaination for the large variation observed in the first harmonic of the anisotropy. The behaviour of the second harmonic is tentatively interpreted in the light of current theories. To speed up publication, the authors of this paper have agreed to not receive the proofs for correction.     

Dark material by fast protons on frozen methane

Summary In the light of the experimental results presented in a correlated paper on the production of organic residues by bombarding hydrocarbon frosts with fastions, we show that substantial amount of these materials can by synthesized on insterstellar grains and objects in the solar system by cosmic-ray fluence. The IR spectra of laboratory residues are shown. The main features we find at 2.9, 3.4, 6.2 and 6.8 μm resemble those observed on interstellar sources and on some meteoritic extracts. Some implications these results have on grain models and evolution and on the possible similarity between interstellar grains and objects in the solar system are also discussed.

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Riassunto Alla luce di risultati sperimentali, presentati in un precedente lavoro di questa serie e concernenti la produzione di residui organici del bombardamento di idrocarburi congelati tramite ioni veloci, noi dimostriamo che apprezzabili quantit? di questi materiali possono essere sintetizzati sui grani interstellari e su oggetti nel sistema solare a causa del bombardamento di raggi cosmici. Sono mostrati gli spettri IR dei residui di laboratorio le cui bande prineipali a 2.9, 3.4, 6.2 e 6.8 μm ricordano quelle osservate su sorgenti astrofisiche e su alcuni estratti da meteoriti. Si discutono anche alcune implicazioni che questi risultati hanno sui modelli e sull'evoluzione dei grani interstellari e sulle possibili similarità tra questi grani ed oggetti nel sistema solare.

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Резюме йспользуя экспериментальные резуьтаты, полученные ранее, по образованию органических остатков при бомбардировке замороженных углеводородов быстрыми ионами, мы показываем, что затемненные материалы могут быть синтезированы в заметных количествах на межзвездных зернах и обБектах в солнечной системе под действием космических лучей. Приводятся инфракрасные спектры лабораторных остатков. Главные особенности этих спектров при 2.9, 3.4, 6.2 и 6.8 мкм похожи на особенности, обнаруженные на межзвездных источниках и на некоторых метеорных экстрактах. Обсуждается применение полученных результатов к моделям зерен и эволюции. Также рассматривается возможное сходство между межзвездными зернами и обБектами в солнечной системе.

     

An analysis of pulsar timing irregularities: is it induced by a source of gravitational waves in the galaxy?

Summary A statistical analysis of the irregularities in the pulse arrival times for the some 30 pulsars, for which the timing noise measurements are available, indicates that, at a confidence level of 96%, the timing noise is induced by a hypothetical source within our Galaxy. The source would be located at 08 h 38 min right ascension, −3° declination and 0.9 kpc distance from the solar system. We suggest and discuss the possibility that the interaction between the ?source? and the pulsars is due to gravitational waves, emitted in bursts by the hypothetical source with yearly rate over the past 10⁵ years. Paper presented at the Congress ?Galactic and Extragalactic Dark Matter?, Roma, 28 to 30 June 1983.     

Identifying a “dark matter” signal by nonisotropic scintillation detector

Summary In this note we investigate the possibility to identify a “dark matter” signal by means of low-background anisotropic scintillators.     

Tracking of flare-generated interplanetary shock waves, responsible for Forbush decreases, by observing type-II radio bursts

Summary New possibilities are pointed out of a more accurate identification of solar flares, responsible for Forbush decreases of galactic cosmic rays, caused by flare-generated interplanetary shock waves, based on tracking type-II radio bursts. Nine solar flares, observed between September 1978 and December 1979, generated shock waves which produced intensive type-II radio bursts observed in the hectometric and kilometric wave range by the ISEE-3 satellite. All the type-II shocks were responsible for Forbush decreases. Since the observation of type-II radio bursts enables us to follow the propagation of shock waves practically from the place where they are generated deep in the solar corona, through interplanetary space as far as the Earth, these observations provide the possibility of exact identification of Forbush decreases with the corresponding flares. These observations have also supplied a further dimension for analysing interplanetary disturbances and forecasting Forbush decreases.

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Riassunto Sono messe in evidenza nuove possibilità per una piú accurata identificazione dei brillamenti solari responsabili delle diminuzioni di Forbush, nell’intensità dei raggi cosmici galattici, dovute ad onde d’urto interplanetarie. Tali possibilità sono basate sull’osservazione dello sviluppo spazio-temporale delle sorgenti della radioemissione di tipo II. Durante il periodo settembre 1978-dicembre 1979, sono stati osservati nove brillamenti solari, che generavano onde d’urto producenti un’intensa radioemissione di tipo II osservata dal satellite ISEE-3 nell’intervallo di lunghezze d’onda ettometrico e chilometrico. Tutte queste onde d’urto erano responsabili delle diminuzioni di Forbush. Poiché l’osservazione della radioemissione di tipo II ci permette di seguire la propagazione delle onde d’urto praticamente dal posto dove loro sono generate, in profondità nella corona, fin nello spazio interplanetario verso la Terra, i risultati ottenuti forniscono la possibilità di una precisa identificazione della connessione tra le diminuzioni di Forbush ed i brillamenti corrispondenti. Queste osservazioni danno anche un ulteriore contributo all’analisi delle perturbazioni interplanetarie ed alla possibilità di previsione di diminuzioni di Forbush.

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Резюме Указываются новые возможности, связанные с прослеживанием радиовспышек типа II, для более точной идентификации солнечных вспышек, ответственных за убывание Форбуша, которые вызывают межпланетные ударные волны. Девять солнечных вспышек, наблюдавшися между сентябрем 1978 и декабрем 1979, образовали ударные волны, которые вызвали интенсивные радио-вспышки типа II, которые наблюдались спутником ISEE-3. Все эти ударные волны типа II ответственны за убывания Форбуша. Так как навпюдения радио-вспышек типа II позволяет нам проследить распространение ударных волн практически от места их образования глубоко в солнечной короне через межпланетное пространство до Земли, то такие наблюдения обеспечивают возможность точной идентификации убываний Форбуша в зависимости от соответствующих солнечных вспышек. Эти наблюдения также позволяют анализировать межпланетные возмущения и предсказывать убывания Форбуша.

     

The enrichment of physics and astrophysics: The legacy of Victor Hess

Summary The Third Victor F. Hess Memorial Lecture traces the evolution of the cosmic-ray discipline from Hess' discovery in his balloon flights of 1911. Serendipitously, this led to the genesis of two major fields of research, high-energy elementary-particle physics and cosmic-ray astrophysics. The subsequent development of the latter field is traced from the early decades when its promise was not widely appreciated. Epochal discoveries in the 1930's and 1940's stimulated widespread interest among physicists. Identification of the positron, the ?soft component?, muons, pions, and the elaboration of the electromagnetic theory of shower production were among the major advances. The nuclear character of the main primary component was demonstrated in the forties. Symbiosis with radioastronomy, notably the understanding of the synchrotron radiation emitted from the Crab Nebula, revealed the role of supernova explosions in providing the energy for the galactic cosmic radiation. Fermi's use of magnetohydrodynamics in his acceleration mechanisms, and their subsequest realization in shock-wave theory are sketched. Detailed investigations of composition—especially measurements of the Li−Be−B and of the³He components—yielded knowledge of the propagation and transformations of the relativistic nuclei in passing through the interstellar medium. This, in turn, made possible the evaluation of path length distributions, predictions of the arriving isotopic composition, the source composition, and cosmic-ray age. Finally, some tantalizing problems that remain are mentioned, notably those of the highest-energy and the lowest-energy cosmic rays. Invited talk given at the XXIV International Cosmic-Ray Conference, Rome, August 28–September 8, 1995.