Identification of gamma-ray sources with Wolf-Rayet stars

An analysis of unidentified discrete sources of gamma-rays with energies E>100 MeV demonstrates that the spatial characteristics of this group of gamma-ray sources coincides with those of Wolf-Rayet stars. It is concluded that Wolf-Rayet stars are potential steady sources of high-energy gamma rays with mean luminosities L(>100 MeV)≈10³⁵ erg/s.     

Observable effects during gravitational microlensing of stars by NUT objects

We consider observable effects during the gravitational microlensing of stars of finite angular size with a given brightness distribution across their disks by exotic objects whose space-time environment is described with the NUT metric. We demonstrate that, under certain conditions, the microlensing light curves and chromatic effects due to the wavelength dependence of the disk brightness distributions can differ considerably from those observed for a Schwarzschild gravitational lens, so that their analysis can facilitate the identification of such objects.     

Observed effects of gravitational microlensing of stars by a spatial-temporal tunnel

We consider microlensing of stars by a spacetime tunnel (wormhole), which is manifest as a gravitational lens with negative mass and a circular caustic in the source plane. If a source with a small angular size does not cross the circular caustic, it is impossible to discriminate between gravitational lenses with positive and negative mass. Even for comparatively large stellar angular diameters, differences from a Schwarzschild lensing curve are on the order of the observational errors. When the angular size of a star is comparable to the radius of the Einstein cone, for a sufficiently large impact parameter, the shape of the observed light curves can be similar to that due to microlensing of a compact object surrounded by an extended gaseous envelope. Such an object can be easily distinguished from a negative-mass gravitational lens via analysis of chromatic and polarization effects of the lensing.     

Detection of gravitational waves through observations of a group of pulsars

We suggest a new approach to the detection of gravitational waves using observations of a group of millisecond pulsars. In contrast to the usual method, based on increasing the accuracy of the arrival times of pulses by excluding possible distorting factors, our method supposes that the additive phase noise that is inevitably present even in the most accurate observational data has various spectral components, which have characteristic amplitudes and begin to appear on different time scales. We use the “Caterpillar” (Singular Spectral Analysis, SSA) method to decompose the signal into its components. Our initial data are the residuals of the pulse arrival times for six millisecond pulsars. We constructed the angular correlation function for components of the decomposition of a given number, whose theoretical form for the case of an isotropic and homogeneous gravitational-wave background is known. The individual decomposition components show a statistically significant agreement with the theoretical expectations (correlation coefficient ρ = 0.92 ± 0.10).     

Simulations of motions of images of extragalactic sources due to weak gravitational microlensing

A statistical study of motions of images of distant extragalactic sources, such as quasars on the celestial sphere, due to the action of weak gravitational microlensing is presented. It was assumed that the parallax of the lens was 10 milliarcseconds (mas), the mass of the lens was 1 M _⊙, and the proper motion was μ = 30 mas. The initial point for the motion of the lens (a star in our Galaxy) was taken to be the boundary of a region with a radius of ϑ = 100 mas and its center coincident with the distant source. The simulations for each trajectory were carried out in steps, with the time step being 0.1 year. The number of sources “launched” over the computational period was 5000. The appearance of the trajectories for the source images is presented; 57% of the total number of sources that participated in the simulations showed motions of 0.7–1.0 mas. Original Russian Text ? T.A. Kalinina, M.S. Pshirkov, 2006, published in Astronomicheskiĭ Zhurnal, 2006, Vol. 83, No. 6, pp. 483–488.     

埋入源下半无限体中瑞利波可激性研究

埋入源激发波场分析对岩土工程勘探非常重要。基于模态叠加法给出均匀半无限体中埋入球形膨胀点源激发波场位移表达式,由此研究瑞利波可激性及其传播特性,分析埋入源下瑞利波可激性机制,并通过有限元模拟验证分析方法有效性。结果显示:在均匀半无限体中瑞利波可激性受源埋深与波长比影响,比值越小,瑞利波可激程度越高;当比值大于1时,瑞利波不易激发。与自由状态下以平面波阵面传播的简正瑞利波相比,半无限体中埋入源激发瑞利波速度随传播距离变化,传播具有空间特性,距中心轴线越近,竖直向质点振动相速度越小,当距离大于一个波长时,激发瑞利波传播特性趋于简正瑞利波。     

表面源激发的瑞利波传播特性分析

自由状态下层状介质中平面瑞利波相速度与频率及层状介质特性参数有关,表面源激发的瑞利波以柱面波阵面传播,传播速度不仅与频率有关,而且还与传播距离有关,这样,自由状态下层状介质中平面瑞利波传播特性理论不能有效地用于激发瑞利波相速度分析。以薄层法得到的圆盘状表面垂直源激发瑞利波位移响应为基础,导出激发瑞利波相速度,比较激发模态与简正模态相速度差异,分析激发模态空间特性,揭示这种空间特性形成机制。结果表明:源对激发模态传播影响距离不超过一个波长,波场距源越近,激发模态竖直振动传播速度越低;在多模波场,激发模态间相长相干或相消相干导致表观相速度具有较明显的空间特性。该研究可为发展考虑瑞利波频率及空间特性反演数学模型及算法提供指导。     

Levels of coronal and chromospheric activity in late-type stars and various types of dynamo waves

We analyze the X-ray emission and chromospheric activity of late-type F, G, and K stars studied in the framework of the HK project. More powerful coronas are possessed by stars displaying irregular variations of their chromospheric emission, while stars with cyclic activity are characterized by comparatively modest X-ray luminosities and ratios of the X-ray to bolometric luminosity L _X/L _bol. This indicates that the nature of processes associated with magnetic-field amplification in the convective envelope changes appreciably in the transition from small to large dynamo numbers, directly affecting the character of the (α-Ω) dynamo. Due to the strong dependence of both the dynamo number and the Rossby number on the speed of axial rotation, earlier correlations found between various activity parameters and the Rossby number are consistent with our conclusions. Our analysis makes it possible to draw the first firm conclusions about the place of solar activity among analogous processes developing in active late-type stars.     

Early formation of (super)massive black holes and gravitational waves from their coalescence

Astronomical observations of last few years have presented a surprising evidence that the Universe at redshift of order 10 is densely populated by supermassive black holes (quasars), supernovae, and contains very large amount of dust. All these data are in conflict with the canonical theory of quasar and supernova formation. A model is discussed which in a simple and natural way solves all these problem. In addition it explains an existence of supermassive black holes in each large galaxy and even in small ones. An inverted picture of galaxy formation is suggested when primordial black holes serve as seeds of galaxy formation. Simultaneously the origin and properties of black hole binaries, sources of gravitational waves registered by LIGO are explained. As a by-product the model may lead to abundant cosmological antimatter even in the Galaxy.     

High-velocity stars as a result of encounters between stars and massive binary black holes in galactic nuclei

Numerical simulations of the motions of stars in the gravitational fields of binary black holes with various component mass ratios have been carried out. Two models are considered: (1) the two-body problem with two fixed centers; (2) the general three-body problem. The first model is applicable only over short times Δt ? T, where T is the period of the binary system. The second model is applicable at all times except for during close encounters of stars with one of the binary components, r ≤ 0.00002 pc, where r is the distance from the star to the nearer black hole. In very close passages, relativistic corrections must be taken into account. Estimates of the probability of formation of high-velocity stars as a result of such interactions are obtained. It is shown that this mechanism is not suitable for the nucleus of our Galaxy due to the probable absence of a second massive black hole in the central region of the Galaxy.     

The disruption of close binaries in the gravitational field of a supermassive black hole and the formation of hypervelocity stars

The formation of hypervelocity stars due to the dynamical capture of one component of a closebinary system by the gravitational field of a supermassive black hole (SMBH) is modeled. The mass of the black hole was varied between 10⁶ and 10⁹ M _⊙. In the model, the problem was considered first as a three-body problem (stage I) and then as an N-body problem (stage II). In the first stage, the effect of the inclination of the internal close-binary orbit (the motion of the components about the center of mass of the binary system) relative to the plane of the external orbit (the motion of the close binary around the SMBH) on the velocity with which one of the binary components is ejected was assessed. The initial binary orbits were generated randomly, with 10 000 orbits considered for each external orbit with a fixed pericenter distance r _p . Analysis of the results obtained in the first stage of the modeling enables determination of the binary-orbit orientations that are the most favorable for high-velocity ejection, and estimation of the largest possible ejection velocities V _max. The boundaries of the region of stellar disruption derived from the balance of tidal forces and self-gravitation are discussed using V _max-r _p plots, which generalize the results of the first stage of the modeling. Since a point-mass representation does not enable predictions about the survival of stars during close passages by a SMBH, there is the need for a second stage of the modeling, in which the tidal influence of the SMBH is considered. An approach treating a star like a structured finite object containing N bodies (N = 4000) enables the derivation of more accurate limits for the zone of efficient acceleration of hypervelocity stars and the formulation of conditions for the tidal disruption of stars.     

Ijolite versus carbonatite as sources of fenitization

Ijolite-carbonatite complexes are ubiquitously surrounded of an aureole of metasomatically altered rocks. The process of alteration is termed fenitization and is generally caused by peralkaline fluids emanating from cooling alkaline, i.e. ijolite and carbonatite magmas. Ijolites and carbonatites normally occur together and attempts to determine the source of the fenitizing fluids may therefore lead to controversial, if not erroneous, conclusions.
Mineralogical and chemical data of fenites from Oldoinyo Lengai (Tanzania), Fen (Norway), and Alnö (Sweden) are reviewed in the present paper in order to reveal the main factors controlling the fenitization around ijolite and carbonatite. Despite the overall alkaline nature of the process, variables such as XCO₂ of the fluid, activity gradients of SiO₂, Al₂O₃ and CaO, FeO/MgO ratio, f O₂ and temperature gradients may differ, producing distinctive patterns of fenitization around the two magmatic sources. The ijolitic-type fluid has low XCO₂, high activities of alkalies, SiO₂ and Al₂O₃, and low activity of CaO. The f O₂ evolves along the hm-mt buffer conditions and the temperature falls gradually with distance from the magmatic source. The carbonatitic-type fluid has high XCO₂, high activities of alkalies and CaO, and low activities of SiO₂ and Al₂O₃. Temperatures and f O₂ are initially high, but decrease sharply with distance from the source. Moreover, the CO₂-rich fluid may complex and transport the REE.     

Seismic response of 3D topographical irregularities under incoming elastic waves from point sources

We study some effects that produce 3D topographical irregularities under incoming elastic waves from point sources using the indirect boundary element method. This technique is based on the representation of elastic waves in terms of single-layer boundary sources. In this way reflected and diffracted waves are constructed at the boundaries from where they are radiated by means of boundary sources. The field emited from the point source is computed with the moment tensor for a shear dislocation and analytical expressions of the elastodynamic 3D Green's functions. In this way we can construct a double couple with variable orientation. We compare the technique with that of Bouchon, who used the discrete wave number method for a shear dislocation in a halfspace with a triangular source function. We subsequently apply our method to simulate the seismic response of a mountain of ellipsoidal geometry. The source function that we have considered is a triangular pulse and we show results corresponding to the velocity registered over the surface of the irregularity and that of the halfspace. This motion is presented by means of snapshots showing the evolution of the wavefields that are present in the problem.     

Seyfert nuclei as sources of ultrahigh-energy cosmic rays

Particles can be accelerated to ultrahigh energies E≈10²¹ eV in moderate Seyfert nuclei. This acceleration occurs in shock fronts in relativistic jets. The maximum energy and chemical composition of the accelerated particles depend on the magnetic field in the jet, which is not well known; fields in the range ～5–1000 G are considered in the model. The highest energies of E≈10²¹ eV are acquired by Fe nuclei when the field in the jet is B≈16 G. When B～(5–40) G, nuclei with Z<10 are accelerated to E≤10²⁰ eV, while nuclei with Z≥10 acquire energies E≥2×10²⁰ eV. Only particles with Z≥23 acquire energies E≤10²⁰ eV when B～1000 G. Protons are accelerated to E<4×10¹⁹ eV, and do not fall into the range of energies of interest for any magnetic field B. The particles lose a negligible amount of their energy in interactions with infrared photons in the accretion disk; losses in the thick gas-dust torus are also negligible if the luminosity of the galaxy is L≤10⁴⁶ erg/s and the angle between the normal to the galactic plane and the line of sight is sufficiently small, i.e., if the axial ratio of the galactic disk is comparatively high. The particles do not lose energy to curvature radiation if their deviations from the jet axis do not exceed 0.03–0.04 pc at distances from the center of R≈40–50 pc. Synchrotron losses are small, since the magnetic field frozen in the galactic wind at R≤40–50 pc is directed (as in the jet) primarily in the direction of motion. If the model considered is valid, the detected cosmic-ray protons could be either fragments of Seyfert nuclei or be accelerated in other sources. The jet magnetic fields can be estimated both from direct astronomical observations and from the energy spectrum and chemical composition of cosmic rays.     

Tree-ring growth curves as sources of climatic information

Regional growth curves (RGCs) have been recently used to provide a new basis for removing nonclimatic trend from tree-ring data. Here we propose a different use for RGCs and explore their properties along two transects, one meridional and the other elevational. RGCs consisting of mean ring width plotted against cambial age were developed for larch samples from 34 sites along a meridional transect (55-72°N) in central Siberia, and for 24 sites on an elevational gradient (1120 and 2350 m a.s.l.) in Tuva and neighboring Mongolia at approximately 51°N. There are systematic gradients of the parameters of the RGCs, such as I₀-maximum tree-ring width near pith, and I_min, the asymptotic value of tree-ring width in old trees. They are smaller at higher latitude and elevation. Annual mean temperature and mean May-September temperature are highly correlated with latitude here, and hence RGC parameters are correlated with these climatic variables. Correlations with precipitation are more complex, and contradictory between meridional and elevational transects. The presence of a similar gradient in the elevational transect is consistent with temperature being the causal factor for both gradients, rather than, for example, latitude-dependent patterns of seasonal photoperiod change. Taking ring measurements from collections of relict and subfossil wood, the RGC-latitude and RGC-temperature relationships are used to estimate paleo-temperatures on centennial time scales. These estimates are consistent with earlier “traditional” dendroclimatic approaches, and with independent information on the northern extent of forest growth in the early mid-Holocene. It may be possible to use this same approach to make estimates of century-scale paleo-temperatures in other regions where abundant relict wood is present.     

Natural seabed gas seeps as sources of atmospheric methane

Microbial and thermogenic methane migrates towards the seabed where some is utilised during microbially-mediated anaerobic oxidation. Excess methane escapes as gas seeps, which occur in a variety of geological contexts in every sea and ocean, from inter-tidal zones to deep ocean trenches. Some seeps are localised, gentle emanations; others are vigorous covering areas of >1 km²; the most prolific seeps reported (offshore Georgia) produce ~40 t CH₄ per year. Gas bubbles lose methane to the water as they rise, so deep water seeps are unlikely to contribute to the atmosphere. However, bubbles break the surface above some shallow water seeps. Estimates of the total methane contribution to the atmosphere are poorly constrained, largely because the data set is so small. 20 Tg yr^–1 is considered a realistic first approximation. This is a significant contribution to the global budget, particularly as methane from seeps is ¹⁴C-depleted. A seep measurement programme is urgently required.GEM