Search

The authors present the current status of the NUCLEON-2 mission aimed at directly measuring the chemical and isotope composition of galactic cosmic rays. A model-independent method of analysis and the results of an analysis of the beam-test experiment are presented. Future plans as part the Detector Part of the System for Investigating and Irradiating Perspective Semiconductor Micro- and Nanoelectronic Products with High-Energy Ion Beams as Part of the Nica Megaproject (abbreviated DPS-NICA) project are presented.

The aim of the NUCLEON space experiment was to measure spectra of high-energy cosmic rays. Direct measurements of energy spectra of protons and nuclei of cosmic rays which allow separating particles in charge are required to solve important astrophysical problems. The satellite was launched on December 26, 2014, and operated for three years. Measured spectra of protons and alpha particles in the energy range of 2–500 TeV per particle have been presented. The results have been analyzed and compared to other experimental data for lower energies. The ratio of fluxes of protons and alpha particles is nearly constant in a wide range of magnetic rigidities (3–100 TV). Thus, the behavior of the ratio of the spectra is significantly different from a similar dependence in the region of lower magnetic rigidities measured in other experiments. One of the possible explanation of this effect can be given within a model with one close source.

The NUCLEON-2 experiment is aimed at the investigation of isotope and charge composition of medium, heavy and ultra-heavy ions ( Z 82 ) in the 300 MeV/N - 1 GeV/N energy range. The concept design of HICRS for the NUCLEON-2 satellite cosmic ray experiment is presented. The performed simulation confirms the isotope resolution algorithms and techniques. Argon isotopes’ resolution in the NUCLEON-2 prototype is presented.

In this paper, the goals and scientific tasks of the space experiment “High Energy Rays Observatory” (HERO) are established. The preliminary design of the scientific equipment is presented, the characteristic features of which are its high geometric factor (up to ∼20 m2 sr) and adequate energy measurement resolution (20–30% or better, depending on the type of components). The ionisation tungsten-scintillator calorimeter is used for energy measurement. The total calorimeter weight is equal to 12 tons. The technical characteristics of the equipment permit the direct study of cosmic rays in a wide energy range, including the unexplored region of 1015–1016 eV. The current status of the space experiment is discussed. Currently, the HERO project is in its pre-R&D phase. The launch of the satellite is planned for between 2025 and 2030.

The NUCLEON experiment is aimed to investigate the composition and energy spectra of high energy cosmic rays. Direct measurements of the energy spectra of cosmic ray protons and nuclei over the range of 1–100 TeV are very important for the solution of a general astrophysical problem of origin of cosmic rays. The satellite was launched on 26 December 2014. The measured charge composition is analyzed and compared with data obtained by other experiments at lower energies. The proton to helium ratio is close to constant over the wide magnetic rigidity area (3–100 TV). The charge composition dependence on magnetic rigidity can be explained by means of the single source model.

In 2015–2016 regular observations within the SETI program were carried out at the RATAN-600 radio telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. The aim of observations was to search for artificial signals from about 30 Sun-like stars and two metal-rich globular clusters. The main underlying idea of these studies was to perform multiple repeated observations (monitoring) of the same objects. The data were analyzed using three methods: we (1) searched for a strong single signal, (2) estimated the flux averaged over the entire observing time, and (3) analyzed the correlations between signals at different frequencies. Collecting the data over two observing years made it possible to perform a search for weak signals at the detection level of several mJy at 2.7 and 6.3 cm wavelengths. The power limits on the signals of extraterrestrial civilizations averaged over the entire data set lie in the 1016–1020 Winterval practically for all objects, whereas the upper luminosity limits for single observations (the beam crossing time was 7–19 s) are 1017–1021 W and the effective isotropic emitted power of the hypothetical transmitters of the said civilizations do not exceed 2 × 109–2 × 1013 W, which is close to the corresponding parameter for the biggest planetary radars. The resulting luminosity limits are indicative of the absence of radio emission from the observed Sun-like stars, which is stationary on average and exhibits flare-like behavior during some observing sessions.

Some results of studies of cosmic rays obtained during the NUCLEON space experiment in 2015–2017 are presented. This experiment was intended for direct measurements of the energy spectra and chemical composition of cosmic rays (Z = 1−30) in the energy range 2–500 TeV. Results presented include energy spectra for various abundant nuclei measured using the new Kinematic Lightweight Energy Meter (KLEM). The primary energies are established using the spatial densities of secondary particles produced in inelastic interactions with a carbon target.

The aim of the NUCLEON space was to measure spectra of high-energy cosmic rays. The cosmic ray acceleration and propagation processes are determined by the magnetic rigidities of the particles. Thus the magnetic rigidity spectra of cosmic ray carbon and oxygen nuclei obtained by the NUCLEON experiment are analyzed and compared to some other experimental results. The spectral indices calculated for different thresholds with regard to magnetic rigidity are presented. The carbon and oxygen nuclei spectra are steeper than helium nuclei spectra in the 400-10000 GV area. The spectra of carbon and oxygen nuclei are similar to the proton spectrum before the “knee”.

This introductory chapter discusses the overall place of the twenty-first-century Singularity within the overall Big History. It is shown that to place the accelerating trend of complexity in the context of Big History, we need to distinguish the two forms (arms) of megaevolution so far in the universe. The first arm of evolution is the decelerating development of physical matter and energy into galaxies, stars, and planets from the initial Big Bang. The second arm of evolution is the accelerating rate of complexity evolution in the form of life, humans, and civilizations, which is the main concern of this book. The book is organized to present these historical megatrends, models, interpretations, future scenarios, and more philosophical questions along with the realization and debate about their limitations and uncertainty.

Initially, this chapter was motivated by questions raised in the SETI project (Search for Extraterrestrial Intelligence). If intelligent life is a normal phenomenon in the Galaxy, and if its rate of technological evolution is at least as advanced as on Earth, then the Galaxy must be full of highly developed technological civilizations, and we should be able to see them in all directions or they should even be here. So why do we not see them? This question is well known and referred to as the “Fermi paradox” or the “astrosociological paradox” (ASP). Panov’s focus is on the following form of that question: “Taking intelligent life to be a usual phenomenon in the Galaxy, then what would their technological civilizations look like, such that they are ‘invisible’ to us now?” This question has great practical importance. If we would like to find extraterrestrial civilizations, then we should try to understand what we are looking for. The method should depend on the aims. And we need to understand civilizations’ potential for technological evolution. It is a difficult problem, but not impossible. The idea is to look at technological development in light of the general laws of evolution. The question then turns out to have significance for our own possible future as a “post-singular” civilization and could assist us in overcoming the challenges of a transitional singularity crisis, which our societies on Earth are just now entering.

The main aims of the NUCLEON satellite experiment are direct measurement of the energy spectra of cosmic ray protons and nuclei in the 2–500 TeV range of energies by two different methods (an ionization calorimeter and the new Kinematic Lightweight Energy Meter (KLEM) technique). The energy spectra of protons and helium nuclei are presented, and their characteristics are discussed.

The NUCLEON space observatory was developed to measure the spectra of cosmic ray nuclei with individual charge resolution in the energy range of several TeV to 1 PeV per particle. The NUCLEON was launched into a heliosynchronous orbit as an additional load on the Resurs-2P production satellite on December 28, 2014, and it is still in operation (2019). This work is a brief review of the results from the NUCLEON observatory over three years of operation in orbit. The spectra of the main primary abundant nuclei and product nuclei of cosmic rays (CRs) are presented. Some new interesting features of the CR spectra found in the NUCLEON data are discussed.

The aims and scientific tasks of the space High-Energy Ray Observatory experiment are determined. The design of the scientific equipment is described. It is characterized by an unprecedently high geometric factor (~20 m2 sr) and fairly high accuracy of measurement. The performance of the equipment allows precise study of cosmic rays in a wide range of energies, including the completely unstudied region of 1015–1016 eV. The current status of the space experiment is determined.

The NUCLEON experiment aims to study chemical composition and energy spectra of galactic cosmic rays for nuclei charges Z = 1 − 30 and energies 10 11 − 10 15 eV. The research is conducted with the help of the NUCLEON scientific equipment installed on the Russian satellite “Resurs-P” No. 2 as an additional payload. This article describes the results of the first year of the space experiment NUCLEON, including methodological features of data acquisition mode setup, evaluation of the equipment’s performance and methods it provides, as well as preliminary results of data analysis.

A brief survey of the data on the isotopic composition of superheavy nuclei in galactic cosmic rays is presented. The scientific goals of the planned experiment are outlined, and the design of the NUCLEON-2 scientific equipment is given.

The NUCLEON space observatory is a direct cosmic ray spectrometer designed to study cosmic ray nuclei with Z = 1 - 30 at energies 10 12 - 10 15 eV. It was launched as an additional payload onboard the Russian Resource-P No. 2 satellite in December of 2014. In this work B/C, N/O and subFe/Fe ratios are presented. The experiment has worked for half of its expected time, so the data have preliminary status, but they already give clear indications of several astrophysical phenomena, which are briefly discussed in this paper.

Data from the NUCLEON space observatory give a strong indication of the existence of a new universal cosmic ray "knee", which is observed in all groups of nuclei, including heavy nuclei, near a magnetic rigidity of about 10\,TV. Universality means the same position of the knee in the magnetic rigidity scale for all groups of nuclei. The knee is observed by both methods of measurement of particles energy implemented in the NUCLEON observatory---the calorimetric method and the kinematic method KLEM. This new cosmic ray "knee" is probably connected with the limit of acceleration of cosmic rays by some generic or nearby source of cosmic rays., 12 pages, 4 figures, 4 pages of Supplemental material (pictures). References improved

The NUCLEON-2 experiment is aimed at the investigation of isotope and charge composition of ions from carbon up to trans-uranium elements in the energy range over about a hundred MeV/N. The concept design of the NUCLEON-2 satellite cosmic ray experiment is presented. The performed simulation and preliminary prototype beam test confirms the isotope resolution algorithms and techniques.

The NUKLON-2 experiment is aimed at measuring the isotope and charge composition of cosmic rays for medium, heavy, and superheavy ions (Z < 82) with energies between 300 MeV/nucleon and 1 GeV/nucleon. The design of the planned satellite-borne NUKLON-2 cosmic-ray detector is presented. Modeling of the detector’s performance indicates the adopted isotope-separation techniques are effective.

One of the most important results from the ATIC experiment is its collection of the energy spectra of abundant cosmicray nuclei: protons, He, C, O, Ne , Mg, Si, and Fe, measured in terms of energy per par� ticle in the energy range of 50 GeV to tens of TeV. Starting with the spectra measured in the ATIC experiment, abundant nuclei spectra in sources are calculated using a number of propagation models. The results from comparing the spectra in sources of different nuclei are shown to depend only weakly on the propagation model. The spectrum of helium in sources is found to be harder than that of protons; this result is of high sta� tistical significance and is virtually modelindependent. From helium up to iron nuclei, the steepness of the spectra in sources is seen to grow notably as the charge of nuclei rises.

The NUCLEON space experiment was designed to measure energy spectra of cosmic ray nuclei from protons to iron in the energy range approximately from 1 TeV per particle to 1 PeV per particle with good individual charge resolution. The apparatus started the collection of data at the beginning of 2015 and it is in operation up to now. The duration of the mission is expected to be no less than five years. One of the main feature of the experiment is an implementation of two different methods of energy measurement on board of the apparatus -- the calorimetric method and the new kinematic KLEM method (Kinematic Lightweight Energy Meter). The data obtained after two years of operation are presented. A multiple signs of complex behavior of the nuclei spectra and the ratios of spectra violating of a simple universal power-law behavior of the spectra will be presented in the report.

The NUCLEON-2 experiment is aimed at the investigation of isotope and charge composition of medium, heavy and ultra-heavy ions (Z < 82) in the 300 MeV/N — 1 GeV/N energy range. The concept design of HICRS for the NUCLEON-2 satellite cosmic ray experiment is presented. The performed simulation confirms the isotope resolution algorithms and techniques.

The NUCLEON satellite experiment is designed to investigate directly the energy spectra of cosmic-ray nuclei and the chemical composition (Z=1−30) at energy range 100 GeV–1000 TeV. The satellite has been launched in 26 December 2014. The planned exposition time is more than 5 years. The first preliminary results are presented including charge distributions and all particles energy spectra

One of the main results of the ATIC (Advanced Thin Ionization Calorimeter) experiment is a collection of energy spectra of abundant cosmic-ray nuclei: protons, He, C, O, Ne, Mg, Si, Fe measured in terms of energy per particle in the energy range from 50 GeV to tens of teraelectronvolts. In this paper, the ATIC energy spectra of abundant primary nuclei are back-propagated to the spectra in sources in terms of magnetic rigidity using a leaky-box approximation of three different GALPROP-based diffusion models of propagation that fit the latest B/C data of the AMS-02 experiment. It is shown that the results of a comparison of the slopes of the spectra in sources are weakly model dependent; therefore the differences of spectral indices are reliable data. A regular growth of the steepness of spectra in sources in the range of magnetic rigidity of 50--1350~GV is found for a charge range from helium to iron. This conclusion is statistically reliable with significance better than 3.2 standard deviations. The results are discussed and compared to the data of other modern experiments., 8 pages, 11 figures

The ratios of heavy nuclei from Sulfur (Z=16) to Chromium (Z=24) fluxes to the flux of iron nuclei were measured recently in the ATIC-2 experiment. These ratios were the decreasing functions of energy from 5 GeV/n to approximately 50 GeV/n as expected. However, an unexpected sharp upturn in the ratios was observed at energy ∼ 50 GeV/n. In this paper, we revise the data and show that the statistical confidence of the observed upturn in the ATIC data is 99.7% and some additional argumets supporting the phenomenon are presented. A possible cause of the upturn is discussed and it is demonstrated that it can be partially understood within a model of ‘Closed Galaxy with Bubbles’ (CGB). Some features and problems of the CGB model are discussed.

in the energy range from 50 GeV to tenths of TeV. In this report the ATIC energy spectra of abundant nuclei are back propagated to the spectra in sources in terms of magnetic rigidity using a number of GALPROP-based models of cosmic rays propagation. It is shown that the results of comparison of the slopes of the spectra are relatively weakly model-dependent within a set of studied models. It is shown that the helium spectrum in sources is flatter than the proton spectrum with high statistical significance. A regular growth of steepness of the spectra is found for a charge range from helium to iron, and this conclusion is also statistical significant. The results are discussed and compared with data of other modern experiments

The description of the Advanced Thin Ionization Calorimeter (ATIC) experiment and its main results are presented. The ATIC experiment is an important step in Galactic cosmic-ray investigations that use the direct methods that were first carried out in the PROTON experiment in the 1960s. We consider the contribution of the ATIC experiment to the understanding of the Galactic cosmic ray origin and propagation.

The author demonstrates that researchers in quantum physics and inflationary cosmology have in practice loosened the rigorous traditional principles of scientific methodology (in particular, observability and experimental reproducibility). He formulates some principles of the new methodology.

Galactic cosmic rays consist of protons, electrons and ions, most of which are believed to be accelerated to relativistic speeds in supernova remnants. All components of the cosmic rays show an intensity that decreases as a power law with increasing energy (for example as E(-2.7)). Electrons in particular lose energy rapidly through synchrotron and inverse Compton processes, resulting in a relatively short lifetime (about 10(5) years) and a rapidly falling intensity, which raises the possibility of seeing the contribution from individual nearby sources (less than one kiloparsec away). Here we report an excess of galactic cosmic-ray electrons at energies of approximately 300-800 GeV, which indicates a nearby source of energetic electrons. Such a source could be an unseen astrophysical object (such as a pulsar or micro-quasar) that accelerates electrons to those energies, or the electrons could arise from the annihilation of dark matter particles (such as a Kaluza-Klein particle with a mass of about 620 GeV).

The purpose of the ATIC balloon experiment is to measure the energy spectra of primary cosmic rays with individual charge resolution from protons to iron over the energy range from ∼50 GeV to 200 TeV. The particle energy is measured by a bismuth germanate (BGO) scintillation calorimeter. The procedure of calorimeter calibration is described, in particular, calibration of the temperature dependence of the calorimeter sensitivity using the data of in-flight measurements. A technique for determining the energy deposited in the calorimeter in view of the temperature dependence of its sensitivity is presented. The maximum systematic error in determining the deposited energy by the calorimeter is 10% or less, and the probable error is estimated at 6%.

The Advanced Thin Ionization Calorimeter (ATIC) Balloon Experiment had a successful test flight and a science flight in 2000–01 and 2002–03 and an unsuccessful launch in 2005–06 from McMurdo, Antarctica, returning 16 and 19 days of flight data. ATIC is designed to measure the spectra of cosmic rays (protons to iron). The instrument is composed of a Silicon matrix detector followed by a carbon target interleaved with scintillator tracking layers and a segmented BGO calorimeter composed of 320 individual crystals totaling 18 radiation lengths to determine the particle energy. BGO (Bismuth Germanate) is an inorganic scintillation crystal and its light output depends not only on the energy deposited by particles but also on the temperature of the crystal. The temperature of balloon instruments during flight is not constant due to sun angle variations as well as differences in albedo from the ground. The change in output for a given energy deposit in the crystals in response to temperature variations was determined.

The Advanced Thin Ionization Calorimeter (ATIC) experiment is designed to investigate the charge composition and energy spectra of primary cosmic rays over the energy range from about 10(11) to 10(14) eV during Long Duration Balloon (LDB) flights from McMurdo, Antarctica. Currently, analysis from the ATIC-1 test flight and ATIC-2 science flight is underway and preparation for a second science flight is in progress. Charge identification of the incident cosmic ray is accomplished, primarily, by a pixilated Silicon Matrix detector located at the very top of the instrument. While it has been shown that the Silicon Matrix detector provides good charge identification even in the presence of electromagnetic shower backscatter from tile calorimeter, the detector only measures the charge once. In this paper, we examine use of the top scintillator hodoscope detector to provide a second measure of the cosmic ray charge and, thus, improve the ATIC charge identification. (c) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved.

This paper reports on the results of measurements performed in the course of the ATIC-2 balloon experiment (2002–2003) for the energy spectra of particles (such as protons; He, C, O, Ne, Mg, Si, and Fe nuclei; and some groups of nuclei) and the all-particle energy spectrum in primary cosmic rays at energies ranging from 50 GeV to 200 TeV. The conclusion is drawn that the energy spectra of protons and helium nuclei differ substantially (the spectrum of protons is steeper) and that the shape of the energy spectra of protons and heavy nuclei cannot be described by a power function.

The preliminary energy spectra of heavy nuclei C, O, Ne, Mg, Si, and Fe in the primary cosmic rays measured by the ATIC-2 experiment are presented and compared to previous data and to propagation models. Using previous data to extend the ATIC-2 results for all heavy nuclei to higher energy, the combined spectra can be best fit with diffusion model with weak reacceleration and scattering on random magnetic field with a Kolmogorov spectrum fluctuations becoming dominant at high energy. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved.

The Advanced Thin Ionization Calorimeter (ATIC) balloon-borne experiment is designed to perform cosmic-ray elemental spectra measurement from 50 GeV to 100 TeV for nuclei from hydrogen to iron. These measurements are expected to provide crucial hints about some of the most fundamental questions in astroparticle physics today. ATTIC'S design centers on an 18 radiation length (X(sub Omnicron)) deep bismuth germanate (BGO) calorimeter, preceded by a 0.75 lambda(sub int) graphite target. In September 1999 the ATIC detector was exposed to high-energy beams at CERN's SPS accelerator, within the framework of the development program for the Advanced Cosmic-ray Composition Experiment for the Space Station (ACCESS). In December 2000 - January 2001, ATIC flew on the first of a series of long duration balloon (LDB) flights from McMurdo Station, Antarctica. We present here results from the 1999 beam-tests, including energy resolutions for electrons and protons at several beam energies from 100 GeV to 375 GeV, as well as signal linearity and collection efficiency estimates. We show how these results compare with expectations based on simulations, and their expected impacts on mission performance.

We analyze the characteristics of the albedo, or the backscatter current, which constitutes a background for charge measurements in calorimetric experiments in high-energy cosmic rays. We compare the experimental data obtained in the flights of the ATIC spectrometer with the simulations performed using the GEANT 3.21 code. We discuss the influence of the backscatter on the charge resolution in the ATIC experiment.

Fine structure of the X-ray photoelectron and conversion spectra of low-energy (0–40 eV) electrons of uranium dioxide UO2 was analyzed based on the electronic structure calculations for the UO 8 12− cluster with O h symmetry, simulating the nearest surrounding of uranium in UO2, by the relativistic X α discrete variation method. It was predicted theoretically and validated experimentally that, in UO2, the U5f electrons (∼1 U5f electron) can directly participate in chemical bonding: ∼2 U5f electrons weakly contributing to chemical bonding are localized at −1.9 eV; ∼1 U5f electron participating in chemical bonding is delocalized in the range of outer valence molecular orbital energies from −4 to −9 eV; and unfilled U5f states are localized mostly at low (from 0 to 5 eV above zero) energies. It was shown experimentally that the U6p electrons actively participate in formation of not only inner valence but also outer valence (0.6 U6p electron) molecular orbitals. The density of the U6p states in UO2 was estimated experimentally. The composition and sequence of the inner valence molecular orbitals at energies within 13–40 eV were also elucidated.

It is supposed that the sequence of the Earths biospheric revolutions obeys the scaling law. An estimation of the duration of the prebiological chemical evolution as (5–7) · 10 9 years is obtained by an extrapolation of the scaling law of the biospheric evolution. The expected scale of time of interstellar prebiological panspermia (� 0.2 · 10 9 yr) is much shorter then the estimated duration of the prebiological chemical evolution. The hypothesis of the long prebiological chemical evolution implies that: (a) the prebiological evolution and the origin of life may be a self-consistent Galaxy process and not a process localized on single planets and (b) life has the same chemical base and the same chirality everywhere in the Galaxy. � 2005 COSPAR. Published by Elsevier Ltd. All rights reserved.

It is argued that the upturn observed in heavy nuclei to iron ratios as measured in the ATIC experiment can be understood within a model of a closed galaxy with embedded local regions containing sources of cosmic rays. This model predicts a universal upturn near energies of 200–300 GeV/nucleon in the spectra of abundant primary nuclei. It also predicts the source spectral index to lie near 2.5.

The Advanced Thin Ionization Calorimeter (ATIC) was built for series of long- duration balloon flights in Antarctica. Its main goal is to measure energy spectra of cosmic ray nuclei from protons up to iron nuclei over a wide energy range from 30 GeV up to 100 TeV. The ATIC balloon experiment had its first, test flight that lasted for 16 days from 28 Dec 2000 to 13 Jan 2OO1 around the continent. The ATIC spectrometer consists of a fully active BGO calorimeter, scintillator hodoscopes and a silicon matrix. The silicon matrix, consisting of 4480 pixels, was used as a charge detector in the experiment. About 25 million cosmic ray events were detected during the flight. In the paper, the charge spectrum obtained with the silicon matrix is analyzed.

Long Duration Balloon (LDB) scientific experiments, launched to circumnavigate the south pole over Antarctica, have particular advantages compared to Shuttle or other Low Earth Orbit (LEO) missions in terms of cost, weight, scientific “duty factor” and work force development. The Advanced Thin Ionization Calorimeter (ATIC) cosmic-ray astrophysics experiment is a good example of a university-based project that takes full advantage of current LDB capability. The ATIC experiment is currently being prepared for its first LDB science flight that will investigate the charge composition and energy spectra of primary cosmic-rays over the energy range from about 1010 to 1014 eV. The instrument is built around a fully active, Bismuth–Germanate (BGO) ionization calorimeter to measure the energy deposited by cascades formed by particles interacting in a thick carbon target. A highly segmented silicon matrix, located above the target, provides good incident charge resolution plus rejection of “backscattered” particles from the cascade. Trajectory reconstruction is based on the cascade profile in the BGO calorimeter, plus information from the three pairs of scintillator hodoscope layers in the target section above it. A full evaluation of the experiment was performed during a test flight occurring between 28 December 2000 and 13 January 2001 where ATIC was carried to an altitude of ∼37 km above Antarctica by a ∼850,000 m3 helium filled balloon for one circumnavigation of the continent. All systems behaved well, the detectors performed as expected, >43 GB of engineering and cosmic-ray event data were returned and these data are now undergoing preliminary data analysis. During the coming 2002–2003 Antarctica summer season, we are preparing for an ATIC science flight with ∼15 to 30 days of data collection in the near-space environment of Long Duration Balloon (LDB) float altitudes.

The role of the U6p,5f electrons in the chemical bond in γ-UO3 was studied on the basis of the low-energy X-ray photoelectron, conversion electron spectra from uranium trioxide, and the calculations for the [UO2O4]6− (D4h) cluster.

The fine structures of X-ray photoelectron (XPE) spectra of low-energy electrons and conversion electron spectra of γ-UO3 (0-40 eV energy) were analyzed taking into account relativistic calculations based on the Xα discrete variation method of the electronic structure of uranium cluster [(UO2)O4]6- (D4h symmetry group) representing the closest coordination of uranium in γ-UO3. The theoretical and experimental data show that U5f electrons directly participate in the chemical bonding. The density of states of 5f valence electrons in uranium trioxide was calculated. At the same time, U6p electrons participate in formation of both inner and outer valence molecular orbitals, and the density of such 6p states in uranium trioxide was also calculated. The order of the inner valence molecular orbitals in the 13-40 eV range was determined, which is of particular importance for development of a procedure to evaluate the uranium-ligand bond distances in axial and equatorial directions in uranyl compounds using their X-ray photoelectron spectra in the range of inner group) representing the closest coordination of uranium in γ-UO3. The theoretical and experimental data showthat U5f electrons directly participate in the chemical bonding. The density of states of 5f valence electronsin uranium trioxide was calculated. At the same time, U6p electrons participate in formation of both inner andouter valence molecular orbitals, and the density of such 6p states in uranium trioxide was also calculated. The order of the inner valence molecular orbitals in the 13-40 eV range was determined, which is of particular importance for development of a procedure to evaluate the uranium-ligand bond distances in axial andequatorial directions in uranyl compounds using their X-ray photoelectron spectra in the range of innermolecular orbitals.

A numerical model of spontaneous decay continuously monitored by a distant detector of emitted particles is constructed. It is shown that there is no quantum Zeno effect in such quantum measurement if the interaction between emitted particle and detector is short-range and the mass of emitted particle is not zero.

The structure of the experimental conversion spectra of an ultrasoft nuclear isomer transition of uranium-235 in oxygen-containing uranium compounds is investigated quantitatively. The behavior of the intensity of the U6p1/2 line in the spectrum is analyzed. It is established that the quasiatomic U6p1/2 orbital in uranyl compounds retains (69±9)% primary electron density on the uranium atom, the remainder passing to molecular orbitals.

Combined measurements of conversion electron spectra and the decay constant (76.5 eV, (1/2)+→(7/2)−) of the E3-isomeric transition of the uranium-235 nucleus have been performed with collection of the isomer atoms on an indium surface. The conversion spectra are interpreted as corresponding to a mixture of two different oxides A and B of uranium, one of which (A) is similar to UO2, and the other (B) consists of a uranium-oxygen cluster based on the linear uranyl group O-U-O. From a set of mixed experimental spectra conversion spectra have been found corresponding to the chemical states A and B of the isomer atoms, and the variation of the absolute intensities of the conversion lines has been quantitatively investigated for them by varying the chemical composition of the isomer atoms and the ratio between the intensities of various conversion lines of the B spectrum. Experimental ratios between the intensities of the conversion lines are compared with the expected ratios in accordance with the distribution of the 6p electron density in the uranyl group. It is concluded that the experimental data agree with the calculation and that abrupt violations of proportionality of the partial probabilities of conversion of the electron density near the nucleus are absent. In accordance with the hypothesis of proportionality of the partial probabilities of conversion, an experimental estimate is given of the degree of localization of the deep-lying uranium 6p 1/2 shell during formation of the chemical bond in the uranyl group: around 70% of the 6p 1/2 electron density remains in the quasi-atomic uranium shell and around 30% is transferred to hybrid molecular orbitals.

This review concentrates on the results obtained, over the last ten years, on the astrophysics of high-energy cosmic ray electrons and positrons. The anomalies, observed in the data of recent experiments (possible bump in the electron spectrum and the PAMELA anomaly in the positron fraction) are discussed through the systematic use of simple analytical solutions of the transport equations for cosmic ray electrons. Three main ways of explaining the origin of the anomalies are considered: the conservative way supposing the positrons to be pure secondary particles; the nearby sources like pulsars origin; and the dark matter origin. This review discusses, also, the inability to select the pulsars model or the dark matter model to explain the electron anomalies on the basis of the electron spectra with the usual large energy binning ($\gtrsim15%$). It is argued that the signature of nearby pulsars origin of the anomalies against the dark matter origin could be the fine structure of the cosmic ray electron spectrum predicted in the Malyshev et al. paper (2009) and which was observed in the data from the high-resolution ATIC experiment (2009-2011). To date, the high-resolution ATIC data was the only experimental result of this type published in the literature. Therefore, they should be tested by other experiments as soon as possible. Generally, there is, also, rather controversial situations between the data of the majority of recent experiments and, consequently, there is a noted urgent need for new high-precision and high-statistical experiments., LaTeX2e, 27 pages, 28 figures, invited paper for 23rd European Cosmic Ray Symposium (2012)

In the Extended Everett Concept, proposed by M.B. Mensky, is assumed, that numerous quantum alternatives that are included in a superposition of many-world Everett universe, are available for the analysis to consciousness, being in some threshold states like sleep or meditation. Since this possibility is in the direct contradiction to no-cloning theorem of quantum mechanics, the question arises how this can be. The proposed solution is based on an analogy with the "miracle of cloning of states", which can be implemented for an observer living in the quantum world, simulated on a classical computer. The basis of the hypothesis is the algorithmic solvability of the quantum theory. NeuroQuantology | March 2013 | Volume 11 | Issue 1| Suppl 1 | Page 116-122

It is argued that the upturn observed in heavy nuclei to iron ratios as measured in the ATIC experiment could be understood within the model of closed galaxy with embedded local regions containing the sources of CR (Peters, Westergaard, 1977). The universal upturn near the energies of 200-300 GeV/n in the spectra of abundant primary nuclei is also predicted by this model, but it also predicts the source spectral index to be near 2.5., Comment: 4 pages, LaTeX2e, 23rd European Cosmic Ray Symposium (2012)