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The long-term modulation of galactic cosmic rays is investigated from 1957 up to 1992 analysing the dynamic and the quasi-stationary components, separately. It has been found that the dynamic component is characterized by the presence of two peaks at the maximum phase of each solar activity cycle. We infer that the time interval between the two peaks corresponds to a period (well-related to the polar heliomagnetic reversal) in which somewhat decreased activity occurs for intense and long-lasting solar events. In fact, a contemporary dip in the magnetic energy released from the Sun was observed, in agreement with the suggested double maximum displayed by the basic features of the 11-year solar-activity cycle (Gnevyshev, 1977, and references therein). Moreover, the dynamic component of cosmic-ray modulation often shows a multi-structured profile in both peaks of activity, fairly well-connected with the pattern of the green corona brightness. On the other hand, analysing the quasi-stationary long-term trend of cosmic-ray intensity we pick out a good relationship between periods of enhanced cosmic-ray modulation and the area expansion of coronal intensity levels. The relevance of our results for solar-terrestrial forecasting is underlined. 相似文献
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The results of the white-light polarization measurements performed during three solar eclipses (1973, 1980, 1991) are presented. The eclipse images were processed and analysed by the same technique and method and, consequently, the distributions of the polarization and coronal intensity around the Sun were obtained in unified form for all three solar eclipses. The mutual comparisons of our results, and their comparison with the distributions found by other authors, allowed the real accuracy of the current measurements of the white-light corona polarization, which is not worse than ±5%, to be estimated. We have investigated the behaviour of the polarization in dependence on heliocentric distance in helmet streamers and coronal holes. Simultaneous interpretation of the data on polarization and intensity in white-light helmet streamers is only possible if a considerable concentration of coronal matter (plasma) towards the plane of the sky is assumed. The values obtained for the coronal hole regions can be understood within the framework of a spherically symmetrical model of the low density solar atmosphere. A tendency towards increasing polarization in coronal holes, connected with the decrease of the hole's size and with the transition from the minimum to the maximum of the solar cycle, was noticed. The problem of how the peculiarities of the large-scale coronal structures are related to the orientation of the global (dipole) solar magnetic field and to the degree of the goffer character of the coronal and interplanetary current sheet is discussed briefly. 相似文献
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Kees C. WELTEN Matthias M. M. MEIER Marc W. CAFFEE Matthias LAUBENSTEIN Kunihiko NISHIZUMI Rainer WIELER Phil A. BLAND Martin C. TOWNER Pavel SPURNÝ 《Meteoritics & planetary science》2012,47(2):186-196
Abstract– Bunburra Rockhole is the first meteorite fall photographed and recovered by the Desert Fireball Network in Australia. It is classified as an ungrouped achondrite similar in mineralogical and chemical composition to eucrites, but it has a distinct oxygen isotope composition. The question is if achondrites like Bunburra Rockhole originate from the same parent body as the howardite‐eucrite‐diogenite (HED) meteorites or from several separate, differentiated parent bodies. To address this question, we measured cosmogenic radionuclides and noble gases in the Bunburra Rockhole achondrite. The short‐lived radionuclides 22Na and 54Mn confirm that Bunburra Rockhole is a recent fall. The concentrations of 10Be, 26Al and 36Cl as well as the 22Ne/21Ne ratio indicate that Bunburra Rockhole was a relatively small object (R approximately 15 cm) in space, consistent with the photographic fireball observations. The cosmogenic 38Ar concentration yields a cosmic‐ray exposure (CRE) age of 22 ± 3 Myr, whereas 21Ne and 3He yield approximately 30% and approximately 60% lower ages, respectively, due to loss of cosmogenic He and Ne, mainly from plagioclase. With a CRE age of 22 Myr, Bunburra Rockhole is the first anomalous eucrite that overlaps with the main CRE peak of the HED meteorites. The radiogenic K‐Ar age of 4.1 Gyr is consistent with the U‐Pb age, while the young U,Th‐He age of approximately 1.4 Gyr indicates that Bunburra Rockhole lost radiogenic 4He more recently. 相似文献
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J. BOROVIĈKA H. W. WEBER T. JOPEK P. JAKEŜ Z. RANDA P. G. BROWN D. O. REVELLE P. KALENDA L. SCHULTZ J. KUCERA J. HALODA P. TÝCOVÁ J. FRÝDA F. BRANDSTÄTTER 《Meteoritics & planetary science》2003,38(7):1005-1021
Abstract— The properties and history of the parent meteoroid of the Morávka H5–6 ordinary chondrites have been studied by a combination of various methods. The pre‐atmospheric mass of the meteoroid was computed from fireball radiation, infrasound, seismic signal, and the content of noble gases in the meteorites. All methods gave consistent results. The best estimate of the pre‐atmospheric mass is 1500 ± 500 kg. The fireball integral bolometric luminous efficiency was 9%, and the acoustic efficiency was 0.14%. The meteoroid cosmic ray exposure age was determined to be (6.7 ± 1.0) × 106 yr. The meteorite shows a clear deficit of helium, both 3He and 4He. This deficit can be explained by solar heating. Numerical backward integration of the meteoroid orbit (determined in a previous paper from video records of the fireball) shows that the perihelion distance was probably lower than 0.5 AU and possibly as low as 0.1 AU 5 Ma ago. The collision which excavated Morávka probably occurred while the parent body was on a near‐Earth orbit, as opposed to being confined entirely to the main asteroid belt. An overview of meteorite macroscopic properties, petrology, mineralogy, and chemical composition is given. The meteorites show all mineralogical features of H chondrites. The shock level is S2. Minor deviations from other H chondrites in abundances of trace elements La, Ce, Cs, and Rb were found. The ablation crust is enriched with siderophile elements. 相似文献
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SPATIO‐TEMPORAL SPECIFICS OF HYDRO‐GEOMORPHIC PROCESSES IN HEADWATER PARTS OF MID‐MOUNTAINS RECONSTRUCTED BASED ON TREE‐RING DATA: A CASE STUDY FROM THE HRUBÝ JESENÍK MOUNTAINS (CZECH REPUBLIC) 
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下载免费PDF全文 Debris flows and debris floods cause frequent geomorphic hazards, even in the mid‐mountains of Central Europe. In the Hrubý Jeseník Mountains (Eastern Sudetes, Czech Republic), strong anthropogenic interventions have created specific conditions for erosion, transport and accumulation of material released by debris flow/flood events. We present a detailed spatio‐temporal reconstruction of the hydro‐geomorphic process activity in two adjacent sub‐catchments using dendrogeomorphic methods applied to the steep, narrow channels. An analysis of 172 sampled trees [Picea Abies (L.) Karst.] revealed 14 torrential events since 1943 in the Klepá?ský stream sub‐catchment and 11 events since 1897 in the Keprnický stream sub‐catchment. Identical events were identified in 1965, 1991, 1997, 2002 and 2010. The event return periods were comparable with return periods from the foothills of the European Alps. A higher frequency of events in the first sub‐catchment may be caused by the presence of a deep‐seated landslide, steeper slopes and a higher susceptibility to shallow slope deformations. Different spatial patterns of events were presented using the Kernel Density analysis in ArcMap 10.1. Clusters of affected trees in the valley floor during the last decades may be due to increased erosion below the check dams and increased accumulation above. The presence of check dams and slope stabilization works since the 1960s has mitigated the processes in several gullies, but due to the current non‐interventional management, the risk of their damage is increasing, particularly when increased activity is observed in the adjacent unprotected gullies. 相似文献
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Giacomo BRIANI Alessandro MORBIDELLI Matthieu GOUNELLE David NESVORNÝ 《Meteoritics & planetary science》2011,46(12):1863-1877
Abstract– Micrometeoroids with 100 and 200 μm size dominate the zodiacal cloud dust. Such samples can be studied as micrometeorites, after their passage through the Earth atmosphere, or as microxenoliths, i.e., submillimetric meteorite inclusions. Microxenoliths are samples of the zodiacal cloud dust present in the asteroid Main Belt hundreds of millions years ago. Carbonaceous microxenoliths represent the majority of observed microxenoliths. They have been studied in detail in howardites and H chondrites. We investigate the role of carbonaceous asteroids and Jupiter‐family comets as carbonaceous microxenolith parent bodies. The probability of low velocity collisions of asteroidal and cometary micrometeoroids with selected asteroids is computed, starting from the micrometeoroid steady‐state orbital distributions obtained by dynamical simulations. We selected possible parent bodies of howardites (Vesta) and H chondrites (Hebe, Flora, Eunomia, Koronis, Maria) as target asteroids. Estimates of the asteroidal and cometary micrometeoroid mass between 2 and 4 AU from the Sun are used to compute the micrometeoroid mass influx on each target. The results show that all the target asteroids (except Koronis) receive the same amount (within the uncertainties) of asteroidal and cometary micrometeoroids. Therefore, both these populations should be observed among howardite and H chondrite carbonaceous microxenoliths. However, this is not the case: carbonaceous microxenoliths show differences similar to those existing among different groups of carbonaceous chondrites (e.g., CI, CM, CR) but two sharply distinct populations are not observed. Our results and the observations can be reconciled assuming the existence of a continuum of mineralogical and chemical properties between carbonaceous asteroids and comets. 相似文献
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Palaeoproterozoic black shales form an essential part of the Birimian volcanosedimentary belt in Burkina Faso, West Africa. The mean Rmax values and the atomic H/C values of the bulk carbonaceous matter (BCM), together with rock structures and mineral assemblages, indicate that these carbon‐rich rocks were metamorphosed to sub‐greenschist and low‐grade greenschist facies. X‐ray diffraction reveals that the (002) ‘graphite’ peak width in half maximum (FWHM) ranges from 0.43 to 0.71 °2θ in sub‐greenschist facies and from 0.27 to 0.41 °2θ in greenschist facies rocks, but the d(002) values in both groups of rocks are approximately the same (～3.35 Å). The BCM of individual samples is composed of particles with very variable shape, reflectance and Raman spectra. Type I particles that predominate in sub‐greenschist facies are fine‐grained, irregular or elongate bodies 1 to 3 μm in size. Their maximum reflectance (Rmax) ranges between 2.5% and 8.2%, and Raman parameters R1 and R2 range from 0.5 to 1.4 and 0.5 to 0.8, respectively. Type II particles are lath‐shaped, up to 40 μm large bodies, commonly arranged parallel to white mica flakes. The number of these particles increases from sub‐greenschist to greenschist facies. Maximum reflectance varies between 6% and 11.2% and R1 and R2 Raman parameters range from 0.05 to 0.7 and from 0.1 to 0.5, respectively. Type III particles occur in hydrothermally altered and sheared rocks; these are nodular aggregates composed of grains up to 10 μm in size. This type of particles has very high reflectance (Rmax = 11–15%) and its Raman spectra indicate a very high degree of structural ordering corresponding to well‐ordered graphite. Type I particles represent original organic matter in the metasediments. Type II particles are believed to have been formed either in situ by solid‐state transformation of Type I particles or by crystallization from metamorphic fluids. Gradual graphitization of the Type I organic particles and the growth of lath‐shaped Type II particles from a fluid phase is assumed to have taken place under the peak metamorphic conditions associated with the burial of Birimian sediments during thrust tectonism, progressive tectonic accretion and crustal thickening during the D1 event of the Eburnean orogeny. The growth of equant, high‐reflectance postkinematic nodular aggregates of Type III particles is ascribed to the reduction of CO2‐rich fluids during a hydrothermal event associated with Late Eburnean D2 exhumation and strike–slip movements. Type I carbonaceous particles were only slightly affected by high‐temperature, low‐pressure contact metamorphism during intrusion of Late Eburnean magmatic bodies, whereas formation of Type II or III particles was not recorded in contact‐metamorphosed rocks at all. 相似文献
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