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.     

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.     

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.

     

On the production mechanism of MF-HF radiopulses associated with large extensive air showers

Summary The existing theories on radio-emission from extensive air showers (EAS) are inadequate to explain the observed high fields associated with the emission of LF-MF-HF radiopulses. One of the attempts has been to explain the phenomenon in the light of the transition radiation (TR) mechanism from the excess negative charge of EAS on striking the ground. However, experimental data are very meagre. In order to concretise the theoretical basis of LF-MF-HF emission, experimental investigations on different aspects of radio-emission are essential. The present paper reports the experimental studies on radio-emission at some preselected frequencies (LF-HF) using a sophisticated data acquisition system. Results on i) variation of field strength with age parameter (S) for different primary energies (E _p) and different core distance (R), ii) lateral distribution of field strength for differentE _p andS and iii) frequency spectrum of radio-emission, are presented and analysed in the light of the TR mechanism.     

Readout technique of thermoluminescence calorimeter for large cascade detectors

Summary A spatial distribution readout system of thermoluminescence [TL] sheets is developed. This system consists of high-gain image intensifier, a CCD-TV camera, a video image processor and a host computer. This system has been applied to artificial TL sheets (BaSO₄: Eu doped) for detecting high-energy electromagnetic shower and to TLC pair meter for determining muon energy. To accomplish these aims, new techniques have been introduced for frame pictures of TL signals in electromagnetic shower:a) the self-correlation method andb) the mutual-correlation method.

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Riassunto Si mette a punto la distribuzione spaziale del sistema di lettura e trasferimento dalla memoria a fogli termoluminescenti (TL). Questo sistema consiste in un intensificatore d'immagine ad alto guadagno, una telecamera CCD-TV, un processore d'immagine video ed un elaboratore principale. Questo sistema è stato applicato a fogli termoluminescenti artificiali (BaSO₄ drogati con Eu) per rilevare sciami elettromagnetici ad alta energia e al TLC-pair meter per determinare l'energia muonica. Per raggiungere questi obbiettivi sono state introdotte nuove tecniche per fotogrammi dei segnali di TL negli sciami elettromagnetici:a) un metodo di autocorrelazione eb) un metodo di correlazione reciproca.

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Резюме Предлагается система термолюминентных пластин для определения пространственного распределения. Эта система состоит из усилителя изображения с высоким коэффициентом усиления, CCD-TV камеры, видеопроцессора и первичного компьтера. Эта техника применяется к искуссттвенным термолюминесцентным пластинам (BaSO₄, легированный Eu) для детектирования электромагнитных ливней высоких энергий и к TLC-парному счетчку для определения энергии мюонов. Для достижения этих целей были разаботаны новые методики: для считывания термолюминесцентных сигналов электромагнитного ливия,a) само-коррелированный метод иb) взаимно-коррелированный метод.

     

Observations of high-energy hadron-gamma families with extremely large lateral spreads

Summary Two very high-energy hadron-gamma families, named ?Halina? and ?C141G4836?, with unusually large lateral spread were detected by the carbon chamber of the Pamir emulsion chamber experiment. The total observed energies of the events are 3540 TeV and 2290 TeV, respectively (E ^(γ)≥2 TeV). The events have extraordinarily wide lateral spread both in electromagnetic component and hadronic component and they are rich in hadrons. One of the lateral characteristics of the events is described in the form of ER-flow density, Δ≡d(ΣER)/d(InR). Both of the experimental events have a very largeER-flow density of gamma-rays, Δ∼17 GeV·km forE _γ≥4 TeV and a high value ofER-flow density is arising from both high particle density and largeER of individual particles. It is shown that the longitudinal and lateral characteristics of the experimental data cannot be fully explained by model calculations even when we consider the contributions of heavy nuclei in primary particles if we assume no fundamental change in elementary process. To speed up publication, the authors of this paper has agreed to not receive the proofs for correction.     

The homestake scintillation detectors: A status report

Summary We describe the 140 ton, 1200 m²sr Large-Area Scintillation Detector located underground at a depth of 4850 ft and the 0.8 km² surface air shower array at the Homestake Mine. Half of the underground detector is currently operating. We discuss its performance and describe the monopole sensitivity of the LASD and the ability of the surface-underground telescope to detect cosmic point sources.

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Riassunto Si descrive il rivelatore a scintillazione di 140 tonnellate a grande area situato sottoterra ad una profondità di 4850 piedi e l'apparecchiatura di superficie di 0.8 km² per rivelare i raggi cosmici a Homestake Mine. Metà del rivelatore sotterraneo è attualmente in funzione. Si discute il suo funzionamento e si descrive la sensibilità del monopolo del LASD e la capacità del telescopio di superficie-sottosuolo di rilevare sorgenti cosmiche puntiformi.

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Резюме Мы описываем 140-тонный 1200 м² сцинтилляционный детектор большой площади, расположенный под землей на глубине 4850 футов и антенную решетку площадью 0.8 км² для атмосферных ливней в шахте Хоумстейк. Половина подземного детектора в настоящее время уже действует. Мы обсуждаем конструкцию и описываем чувствительность к монополям сцинтилляционного детектора большой площади и возможность подземного телескопа—детектировать точечные космические источники.

     

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).

     

Geomagnetic turbulence at L'Aquila (Italy): Preliminary results of a variance analysis

Summary Some preliminary measurements of the geomagnetic turbulence at L'Aquila, in the range of frequency of micropulsations, have been conducted during November 1983. The 60 s variances of the horizontal components show a clear peak around the local noon, while the vertical component is better correlated with the local index of geomagnetic activity which, in the period of interest, has peak values in the afternoon and evening hours. Real-time ?alert? algorithms select the most significant events. These events, which tend to occur in the range of frequency of Pc 2 and Pc 3, perturb mainly the horizontal components and the field fluctuations is often oriented along the averageH. This activity is supported by the Ministero della Pubblica Istruzione (40%) and by the Gruppo Italiano di Fisica Cosmica del C.N.R.     

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.     

Effect of binarity on the local stellar mass density

Summary Considering the existence of many unresolved binary systems among the stars used to derive the stellar luminosity function, we have estimated the increase in the total mass density in the solar neighbourhood. Such an increase depends on the fraction of stars which are unresolved binaries, but conservative estimates give a value larger than 0.004M _⊙ pc⁻³. Paper presented at the Congress ?Galactic and Extragalactic Dark Matter?, Roma, 28 to 30 June 1983.     

Analysis of the time structure of the GLE on February 16, 1984

Summary The time structure of the ground-level event on February 16, 1984 was studied by using 30 s data of the Turku double neutron monitor. The onset time of the event was found to be (09:06:00±1) min U.T. The time between the injection of protons from the flare site and release of relativistic particles into interplanetary space was (6÷7) min. The linear rise rate of the event at Turku was 5.4%/min and the rise time (5±1) min. The event was complicated in structure consisting of at least two separate pulses of particles, the first lasting for about 14 min and the second about 8 min.

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Riassunto Si è studiata la struttura dell'evento a livello del suolo verificatosi il 16 Febbraio 1984 usando i dati a 30 s del doppio monitor neutronico Turku. Si è trovato che il tempo all'inizio dell'evento a Turku era (09:06:00±1) min U.T. Il tempo tra l'iniezione di protoni dal sito di brillamento e il rilascio di particelle relativistiche nello spazio interplanetario era di (6÷7) min. Il tasso lineare d'incremento dell'evento a Turku era di 5.4%/min e il tempo di incremento era di (5±1) min. L'evento era complicato nella sua struttura, che consiste in almeno due impulsi separati di particelle, il primo di durata di circa 14 min e il secondo di circa 8 min.

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Резюме Исследуется временная структура события на уровне земли 16 февраля 1984 г., используя 30-секундные данные с двойного нейтронного монитора в Турку. Время начала события составляет 09:06:00±1 минут U.T. Время между инжекцией протонов от места вспымки и высвобождением релятивистских частиц в межпланетное пространство составило (6÷7) минут. Линейная скорость возрастания события в Турку была 5.4%/мин, а время возрастания было (5±1) минут. Это событие имело сложную структуру, которая состоит, по крайней мере, из двух изолированных импульсов частиц, первый имеет продолжительность около 14 минут, а второй—около 8 минут.

     

High-energy cosmic-ray physics with an EAS array on the top of the Gran Sasso Laboratory

Summary An air shower array on top of the underground Gran Sasso Laboratory (GSL) can give valuable information in the field of high-energy cosmic-ray physics. We discuss the performances of a specific apparatus (EAS-TOP) operating both in coincidence with the underground array (i.e. for measuring the total primary energy of multimuon events) and as an autonomous air shower detector (for studies of ultra-high-energy gamma-ray astronomy, cosmic-ray anisotropies and primary composition).

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Riassunto Un apparato per EAS posto in superficie nella zona sovrastante il laboratorio sotterraneo del Gran Sasso può fornire utili informazioni sulla radiazione cosmica primaria. Qui si presenta un apparato (EAS-TOP) the funzionerà sia in coincidenza con gli apparati posti nel tunnel per misure sull'energia primaria degli eventi multimuonici sia in modo autonomo come rivelatore EAS per ricerche di γ-astronomia ad energie molto elevate, di anisotropia dei raggi cosmici primari, e di composizione primaria.

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Резюме Установка для регистрации ШАЛ над подземной лабораторией Гран Сассо может дать полезную информацию для физики космических лучей высоких энергий. Мы обсуждаем возможности установки EAS-TOP, работающей как в совпадении с подземными детекторами (для измерения полной начальной энергии в многомюинных событиях), так и в автономном режиме—для исследований в области гамма-астрономии сверхвысоких энергий, измерений анизотропии космических лучей и химического состава первичного излучения.

     

Investigation on the effectiveness of VHE gamma-ray astronomy techniques based on imaging of ?erenkov light flashes

Summary A high-velocity Monte Carlo method is applied to very-high-energy gamma-ray astronomy techniques. The discrimination effectiveness against the cosmic-ray background is investigated for the technique based on the two-dimensional imaging of the Čerenkov light flashes created by the extensive air showers in the atmosphere. It is shown that previously proposed discrimination methods using the difference in the Čerenkov light flash shape of gamma-rays—and background-induced showers have low effectiveness. Two new discrimination methods are proposed, based on the difference in the orientation of Čerenkov light spot and fluctuations of the light density. The combination of these methods allows us to increase the ?signal/noise? ratio by 4–5 times.

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Riassunto Si applica un metodo di simulazione Monte Carlo veloce alle tecniche in uso in astronomia gamma di altissima energia. Si studia l'efficienza di discriminazione contro la radiazione di fondo cosmica per il metodo basato sulle immagini bidimensionali degli impulsi di luce Čerenkov creati dai grandi sciami nell'atmosfera. Si dimostra che i metodi di discriminazione precedentemente proposti, basati sulla differenza di forma tra gl'impulsi di luce Čerenkov prodotti da sciami iniziati da fotoni gamma o da radiazioni di fondo, hanno una bassa efficienza. Si propongono, quindi, due nuovi metodi di discriminazione basati sulla differenza di orientazione della macchia luminosa Čerenkov e sulle fluttuazioni della densità luminosa. L'uso di entrambi i metodi permette di aumentare il rapporto segnale-rumore di un fattore 4–5.

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Резюме В технике гамма-астрономии очень высоких энергий используется метод Монте-Карло. Исследуется эффективность дискриминации космических лучей для техики, основанной на двумерной визуализации вспышек черенковского излучения, образованных широкими атмосферными ливнями. Показывается, что ранее предложенные методы дискриминации, используюжие различии в форме вспышек черенковского излучения для гамма-лугей и фоновыми ливнями, имеют низкую эффективность. Предлагаются два новых метода дискриминации, которые основаны на различиии в ориентации пятна черенковского излучения и флуктуаций интенсивности света. Комбинация этих методов позволяет нам увеличить отношение сигнала к шуму в 4–5 раз.

     

Limit on monopole flux in the Mont Blanc NUSEX experiment

Summary A trigger dedicated to the search of superheavy monopoles operates since about two years in the NUSEX apparatus, installed in the Mont Blanc tunnel. Monopoles are identified by time of flight and visualization of the pulses involved in a trigger. The present upper limit on monopole flux is 2.3·10⁻¹³ cm⁻² s⁻¹ sr⁻¹ (90% c.l.).

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Riassunto Da circa due anni è operativo sull'apparato NUSEX, installato nel tunnel del Monte Bianco, un trigger dedicato alla ricerca dei monopoli previsti dalle teorie di grande unificazione. L'identificazione dei monopoli è basata sul tempo di volo e sulla localizzazione nello spazio degli impulsi coinvolti nel trigger. Il limite superiore fino ad oggi raggiunto per il flusso di monopoli è 2.3·10⁻¹³ cm⁻²s⁻¹ sr⁻¹ (90% c.l.).

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Резюме Триггерная схема, предназначенная для поиска сверхтяжелых монополей, действует в течение почти двух лет в установке NUSEX, расположенной в туннеле под Мон Бланом. Идентификация монополей основана на времени пролета, а локализация в пространстве осуществляется с помощью импульсов в триггерной схеме. Настоящий верхний предел на поток монополей составляет 2.3· ·10⁻¹³ см⁻² с⁻¹ ср⁻¹ (к 90% вероятностью).

     

Study on the structure functions of electrons and the energy flow in the soft component of cosmic-ray extensive air showers

Summary Cosmic-ray air shower structure functions for the distance dependence of electron density in cosmic-ray air showers in the size range 10⁴⋎10⁸ have been computed for their intercomparison and comparison with Monte Carlo simulation results and measurements from recent experiments. The analysis has yielded the present status of theoretical structure functionsvis à vis experimental results and Monte Carlo simulation distributions. The effect of core location error on the lateral distribution of electrons is also discussed from the point of view of different theoretical and experimental results. The energy flow in the soft component of air showers of size ∼4·10⁵ has been evaluated within a ring of radius 10m about the axis of the showers.     

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.

     

On the use of clocks in satellites for the detection of gravitational radiation and oscillations of the sun

Summary It is shown that, by using the path dependence of synchronization of clocks in a gravitational field, it is in principle possible not merely to observe bursts of gravitational radiation but also oscillations of the Sun. Estimates are made of the effect of the solar oscillations on the clocks. It is also pointed out that, by making use of the binary pulsar and millisecond pulsars as clocks, it is possible to observe gravitational radiation without interference from the solar oscillation.

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Riassunto Si mostra che, usando la dipendenza del percorso di sincronizzazione degli orologi in un campo gravitazionale, è possibile, in linea di principio, osservare non soltanto impulsi di radiazione gravitazionale ma anche oscillazioni del Sole. Si fanno stime dell'effetto delle oscillazioni solari sugli orologi. Si sottolinea inoltre che facendo uso delle pulsar binarie e delle pulsar a millisecondi come orologi, è possibile osservare radiazioni gravitazionali senza interferenza da parte dell'oscillazione solare.

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Резюме Показывается, что использование зависимости синхрононизации часов от траектории в гравитационном поле, в принципе, позволяет не только наблюдать вспышки гравитационнного излучения, а также осцилляции Солнца. Оценивается влияние солнечных осцилляций на часы. Отмечаетсь, что использование бинарного пульсара и миллисекундных пульсаров в качестве часов, позволяет наблюдать гравитационное излучение вез интерференции от солнечных осцилляций.

     

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.

     

Atmospheric effects on cosmic-ray muon intensities at deep underground depths

Summary On the basis of the theoretical calculation of the atmospheric effect on the cosmic-ray muon intensity, it is demonstrated that the following two anomalous facts recently reported from muon observations at deep underground stations can be attributed to the atmospheric-temperature effect. One is the remarkable dependence of the muon intensity on the atmospheric pressure observed at Poatina (365 m w.e. in depth) and Matsushiro (250 m w.e. in depth), which is contradictory to theoretical expectations, and the other is the semi-annual variation in the muon intensity at Matsushiro, which exhibits a striking contrast to annual variations usually observed at underground stations shallower than Matsushiro. In the present paper, the barometer coefficient and the partial temperature coefficient are also provided for various combinations of parameters such as the muon threshold energy and the zenith angle to meet any requirement of observations.

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Riassunto Sulla base del calcolo teorico dell'effetto atmosferico sull'intensità dei muoni dei raggi cosmici, si dimostra che due fatti anomali riportati recentemente riguardanti osservazioni muoniche in stazioni a grande profondità si possono attribuire all'effetto della temperatura atmosferica. Uno è la notevole dipendenza dell'intensità muonica dalla pressione atmosferica osservata a Poatina (365 m w.e. di profondità) e Matsushiro (250 m w.e. di profondità), che è in contraddizione con previsioni teoriche, e l'altro è la variazione semiannuale nell'intensità muonica a Matsushiro, che mostra un contrasto stridente con le variazioni annuali osservate solitamente in stazioni sotterranee meno in profondità di Matsushiro. In questo lavoro si forniscono il coefficiente barometrico e il coefficiente parziale di temperatura per varie combinazioni di parametri come l'energia di soglia muonica e l'angolo zenitale per soddisfare ogni esigenza di osservazione.