[en] According to the Unified Model of Active Galactic Nuclei (AGN), unobscured AGN based on its optical spectrum (detection of rest-frame UV-optical broad emission lines, type-1 AGN) should appear as X-ray unabsorbed AGN. However, there is an important fraction (10-30%) of AGN whose optical and X-ray classi cations do not match, and the origin of the discrepancy is not clear. To provide insight into this topic, we have conducted a statistical analysis of the optical obscuration and X-ray absorption properties of the optically type-1 AGN from the Bright Ultra-hard XMM-Newton Survey (BUXS) with >1042 erg s1 and z=0.05-1. We have high-quality spectra from XMM-Newton and either SDSS spectra or proprietary observations for the selected sample. In order to provide the most complete sample as possible, we have conducted a detailed analysis of the emission lines to provide a reliable classiffication of the AGNs. We derive the X-ray absorption by fitting their XMM-Newton spectra and the optical extinction using UV/optical spectral continuum fits. As BUXS is a flux limited X-ray selected sample at hard energies (f4:510keV 14 erg s1cm, it is complete for NH column densities up to the Compton-thick limit (1024 cm). Our preliminary results show that most type-1 AGN in our sample show consistent optical and X-ray classiffication, but there is a large fraction ( 20%) of objects with large NH column densities.

[en] New data on energy spectra of light and heavy nuclei at energy os 10-200 inside the Earth's magnetosphere are reported

[en] In the Indian cosmic ray experiment (IONS) in Spacelab-3 the intention is to study nuclei up to iron in low energy cosmic rays, using CR-39 (DOP) detectors. CR-39 (DOP) was exposed to He-4, C-12, O-16, Ne-20, Si-28, Ar-40, Cr-52 and Fe-56 accelerated beams from various accelerator facilities available around the world. Different beam energies and exposure angles were used. From these exposures, the charge resolution and energy resolution for the detector in the region of interest were studied. The effect of pre-annealing and depth on the response of our detector was studied. For isotopic resolution, the detector samples were exposed to Ne-2O and Ne-22 accelerated beams. Samples of CR-39 (DOP) exposed to different accelerated heavy ions were kept in the detector module to take into account the effect of ambient conditions on detector response during the flight

[en] An analysis is made of the current status of measurements on the energy spectrum and anisotropy of the cosmic rays of the highest energy, above 10¹⁸ eV. Measurements from Haverah Park (northern hemisphere) and Sydney (southern hemisphere) are consistent in energy spectrum and anisotropy in the common sky area. Events with energy above 5 x 10¹⁹ eV are largely of extragalactic origin. Several particles arrive preferentialy from the general direction of the local supercluster. There is also an excess of particles coming from the galactic South Pole direction, which is not understood

[en] A method to determine with gas Cerenkov counters the Lorentz factor, gamma = E/mc, of cosmic ray nuclei with high accuracy over the range gamma approx. 20 to 100 is discussed. The measurement of the Cerenkov emission angle theta, by use of a suitable imaging system is considered. Imaging counters, the ring imaging Cerenkov counters (RICH), were developed for use on accelerators. The image of off-axis particles to determine the amount of image distortion as a function of the direction of the incoming nucleus is examined and an acceptance solid angle, relative to the optical axis, within which the nucleus produces an image with an acceptable level of distortion is defined. The properties of the image, which becomes elliptical, for off-axis particles are analyzed

[en] The Early Universe is believed to have been in the form of quark gluon plasma till about a few microseconds after the Big Bang. We briefly discuss the basic concepts of the physics of quark gluon plasma and its formation in relativistic heavy ion collisions. Signatures of its formation and steps being taken to use these experiments to explore dynamics and properties of quark gluon plasma will be covered. (author)

[en] The life in the earth depends totally on the sun. The universe was born from great explosion, the Big Bang. Practically all the materials in the nature contain radioactive nuclides. The sources that give them origin can be categorized as: 1. Cosmogenic s 2. primordial 3. anthropogenic. The application for the first and two groups of natural radionuclides it is the age estimation. Although some of the primitive ones has application in therapy of oncological patient. 1: The three groups of age estimation methods, for nuclear phenomenons are: 1. Measure of the radioactive decline of the primitive isotopes, by accumulation of stable isotopes. 2. use of the descendants of radioactive isotopes of the families of the Uranium or of the Th. 3. Measure of the cosmogenic s isotopes

[en] Experimental results of investigation of primary cosmic rays spectrum at Kosmos-1543 sattelite, conducted in 1984, are presented. Energy spectrum of nuclei with 10≤Z≤16 charge, where Ne, Mg and Si nuclei prevail, are presented

[en] A self-bound object, which is composed of hyperon-mixed neutron-star matter with kaon condensates, is discussed as a candidate of baryonic dark matter. A kaon-condensed nucleus is obtained in a liquid-drop picture, and its relation to deeply bound kaonic nuclei is mentioned

[en] The workshop is concerned with the re-evaluation of radiation levels due to cosmic ray primaries in space, so as to provide the best estimates of the radiation hazard for manned space flights to the vicinity of Mars. This will determine the amount of shielding required. The Fe component is the most important single source of the radiation damage - it is abundant, it has high ionization loss and gives tracks with high LET that have a ''quality factor'', QF, equal to 20 for radiation hazard estimates. Hitherto, cosmic ray charge spectra have been obtained using Fe or Si as a substandard, with the absolute flux values being somewhat uncertain. Hence this workshop and hence our response to it. The data we present come from the satellite Ariel-6, launched from Wallops Island on 6 June 1979. The orbit inclination was 55^o and initial height 625 km. The experiment operated over a period of 3 yr before power problems eventually overcame the satellite. In total we intercepted some 8.7 x 10⁶Fe nuclei within our acceptance aperture of 1.40 m² sr (after allowing for the Earth's shadow and geometrical selection effects). The main purpose of the experiment was to study the ultra-heavy (UH) component of the cosmic rays (Z≥30) and, as a background to this aim, so as to obtain in-flight calibration, the Fe group (24.7 ≤ Z_eff ≤ 28.7) was continuously monitored. (author)