Cutoff in the hard X-ray spectra of the ultraluminous X-ray sources HoIX X-1 and M82 X-1

Using data from the XMM-Newton and INTEGRAL observatories, we have detected a cutoff at energies above 10 keV in the X-ray spectra of the ultraluminous X-ray sources HoIX X-1 and M82 X-1. The spectra obtained can be described by amodel of Comptonization of radiation in a gas cloud of moderate temperature (kT ～ 2–3 keV) and high optical depth (τ ～ 15–25). Such conditions can be fulfilled during supercritical accretion of matter onto a stellar-mass black hole accompanied by a strong gas outflow. The results of this work confirm the existence of a spectral state specific to ultraluminous X-ray sources, which is unlike any of the known spectral states in normal X-ray binaries.     

The spectrum and polarization of a source of synchrotron emission with components flying apart at relativistic velocities

In the present paper we consider the frequency spectrum, time variations and polarization of the flux of synchrotron radio emission from a source which consists of two components flying apart in opposite directions with relativistic velocities at the same time expanding. A comparison of the calculations with unusual double-humped spectra of some radio sources suggests the existence in their nuclei of such double components which are at an early stage of relativistic ejection. In particular the double-humped spectra of 3C 84 and 4C 50.11/NRAO-150 can be interpreted in the proposed model (see Figures 6, 7, 12 and Equations (22), (32)). In this model the ratio of maximum frequenciesv _1m/v _2m should be larger than that of the maximum fluxesF _v1m ⁽¹⁾/F _v2m ⁽²⁾.The linear polarization of the double-humped spectrum is analysed. It is found under rather specific conditions that at the low-frequency maximum of the spectrum of the type given in Figures 6 and 7 a lower degree of linear polarization is expected than at the high-frequency maximum. In addition, it is natural to expect the appearance of circular polarization in sources with internal largescale relativistic motions. The time variations of the radio flux of some QSS, N-galaxies, and nuclei of Seyfert galaxies can also be interpreted in the suggested model of two clouds of relativistic electrons flying apart in different directions with relativistic velocities while simultaneously expanding. For example, Figure 11 shows the flux variations at 3 frequencies whose ratio is 16:4:1. This picture is similar to the observations of 3C 279 at 3.4 mm, 2 cm and 6 cm, and several other sources (Kellermann andPauliny-Toth, 1968).There have been a number of attempts to explain the flux variations of radio sources in the model of successive, but unrelated outbursts of clouds of relativistic electrons caused by supernova explosions. This model meets many difficulties and seems improbable. In this paper we suggest experimental tests to make a final choice between the model of double components flying apart relativistically and the model of two successive, but unrelated, outbursts from supernovae.If the suggested model of explosions in radio sources is correct, then the processes of variable energy output in such different populations as QSS, N-galaxies, radio-galaxies and the nuclei of normal galaxies have a similar nature, differing only in quantity.Translated by D. F. Smith.     

The Olivinite of the Krestovskaya Intrusion—the Product of Larnite-Normative Alkali Ultramafic Magma: Melt Inclusion Data

Olivinites of the Krestovskaya Intrusion consist of predominant amount of olivine, and minor Ti-magnetite, perovskite, and clinopyroxene (from single grain to a few vol %). Primary crystallized melt inclusions were found and studied in olivine, perovskite, and diopside of the olivinites. Daughter phases in olivine-hosted melt inclusions are monticellite, perovskite, kalsilite, phlogopite, magnetite, apatite, and garnet andradite. Perovskite-hosted melt inclusions contain such daughter phases as kalsilite, pectolite, clinopyroxene, biotite, magnetite, and apatite, while daughter phases in clinopyroxene-hosted melt inclusions are represented by kalsilite, phlogopite, magnetite, and apatite. According to melt inclusion heating experiments, olivine crystallized from above 1230°C to 1180°C. It was followed by perovskite crystallizing at ≥1200°C and clinopyroxene, at 1170°C. According to analysis of quenched glass of the melt inclusions, the chemical composition of melts hosted in the minerals corresponds to the larnite-normative alkali ultramafic (kamafugite) magma significantly enriched in incompatible elements. The high incompatible element concentrations, its distribution, and geochemical indicator ratios evidenced that the magma was derived by the partial melting of garnet-bearing undepleted mantle.     

Resonant scattering in galaxy clusters for anisotropic gas motions on various spatial scales

The determination of the characteristic amplitudes and directions of hot gas motions in galaxy clusters from observations of the brightest resonance lines is discussed. Gas motions affect (i) the spectral line shape through the Doppler effect and (ii) the distortions of the radial surface brightness profiles in lines during resonant scattering. Radiative transfer calculations have been performed by the Monte Carlo method in the FeXXV resonance line at 6.7 keV for the Perseus cluster A426. As a result, (a) radial motions have been shown to reduce the scattering efficiency much more dramatically than purely tangential motions; (b) large-scale gas motions have been shown to affect weakly the scattering efficiency; and (c) the uncertainty in measuring the characteristics of gas motions using resonant scattering has been estimated from existing and future observations of clusters.     

Suture zones of the Urals as integral prospective ore-bearing tectonic structures

Rift-related (1.2 Ga) and collision (380–240 Ma) suture zones of the Urals are described. The riftrelated suture zones comprise an ultramafic-gabbro complex with titanomagnetite mineralization, an ultramafic complex with chromite mineralization, and a complex of alkali granitoids with rare-metal (including REE) mineralization accompanied by K-feldspathites, albitites, and calcite metasomatic rocks. The collision suture zones are distinguished by early collision granitoids specialized for tungsten (scheelite) and gold, as well as by raremetal granites and such derivatives of them as pegmatite and greisen with rare-metal and colored-stone mineralization. The suture zones are characterized by long-term (up to 80 Ma or more) continuous-discontinuous periods of ore deposition; heterogeneous sources of ore matter and ore-bearing fluids; a polyelemental composition of lithogeochemical halos and an integral mineral composition of altered wall rocks; and the occurrence of mafic, intermediate, and felsic dikes at large gold deposits, as well as wide variations in PT parameters of the ore-forming process: T = 620?150°C and P = 3.2?0.6 kbar. Collision played a dual role in ore formation. On the one hand, collision led to deformation and metamorphism of precollision massive sulfide deposits and, to a lesser degree, Au-bearing Fe and Cu skarn and porphyry copper deposits, and, on the other hand, to the formation of new gold, rare-metal, quartz, colored-stone, talc, muscovite, and noble serpentine deposits. As a rule, this polygenetic mineralization differs in age and is related to collision volcanic and plutonic complexes. This diversity can be a good basis for metallogenic analysis, forecasting, and prospecting of various metallic deposits and industrial minerals. Polygenetic mineralization of various age known in suture zones is accompanied by integral lithogeochemical and metasomatic halos characterized by a continuous-discontinuous history. The complexity of ore mineralization and often nonlinear metallogeny increase the practical value of suture zones.     

Polarization of X-ray emission from the Sgr B2 cloud

The Sgr B2 giant molecular cloud is claimed to be an 'X-ray reflection nebula'– the reprocessing site of a powerful flare of the Sgr A* source, which occurred a few hundred years ago. The shape of the X-ray spectrum and the strength of the iron fluorescent line support this hypothesis. We argue that the cleanest test of the origin of X-rays from Sgr B2 would be a detection of polarized emission from this source.     

Annihilation of positrons in the Galaxy

Observations of electron-positron annihilation radiation from the Galactic Center region with the SPI instrument aboard INTEGRAL are summarized. The measured width of the 511 keV line and inferred fraction of positrons annihilating through positronium formation are consistent with the annihilation taking place in the warm ISM phase, although combinations of several ISM phases are also allowed by the data. The spatial distribution of 511 keV emission suggests that positron sources are concentrated toward the Galactic bulge and avoid the Galactic disk.     

On the explosive prevention of collisions of asteroidal and cometary bodies with the earth at their late detection

We consider the questions of an explosive impact on asteroids and comets that approach the Earth in the case of a late forecast of the dangerous situation. Based on models for the destruction of the material of a celestial body in the shock wave produced by a strong self-buried explosion, we estimate the radius of the destroyed region, the ejected mass, and the recoil momentum. We determine the charges needed to completely destroy bodies of various sizes and compositions or to divert bodies from the Earth by the required distance. When comets are dangerous bodies, we compare the efficiencies of the explosive and sublimation methods of changing their orbits. We discuss how to increase the efficiency of the explosive impact on a dangerous body through the use of a high relative velocity of the encounter between this body and a charge-carrying rocket.