A Problem Manifests Itself

The purpose of the article is to generalize the positions of the theories of cyclic fashion development and to identify their relevance in fashion trends forecasting of the end of XX – beginning of XXI centuries. Methodology. Methodological basis of the research is formed by the principles of historicism and objectivity, the laws of the system approach, a comparative and historical method of analysis. The scientific novelty of the article is to find out the relevance of the inciples of "cyclic theories" in the dynamics of fashion forecasting of the end of XX – beginning of XXI centuries. Conclusions. The analysis of the cyclicity of fashion theories confirms the topicality of a number of their principles in fashion trends forecasting of the end of XX – beginning of XXIcenturies. At the same time, the topical tasks of scientific studies are the concretization of the fashion cycles duration taking into account the dynamization of fashion changes; the analysis of the combination of natural cyclic dynamics with ascending general tendencies; the substantiation of style parameters of fashion cycles; the in-depth study of the periods of acceptance and dissemination of fashion.Key words: theories of cyclic dynamics of fashion, principles of forecasting in design, methods of prediction in design, modeling method, extrapolation

We analyze the dynamics of a class of cosmological solutions of the Einstein–Vlasov equations. These equations describe an ensemble of collisionless particles (which represent galaxies or clusters of galaxies) that interact gravitatively through Einstein's equations of general relativity. The cosmological models we consider are spatially homogeneous, of Bianchi type IX, and locally rotationally symmetric (LRS). We prove that generic solutions exhibit an oscillatory behavior close to the singularities (the “big bang” in the past and the “big crunch” in the future); this is in contrast to the behavior of Einstein-vacuum or Einstein–Euler solutions. To establish this result we make use of dynamical systems theory; we introduce dimensionless dynamical variables that are defined on a compact state space. In this formulation the oscillatory behavior of generic solutions is represented by the existence of heteroclinic cycles on the boundary of the state space.

Dynamic Vacuum Field Theory (DVFT) posits a unified framework where spacetime curvature and quantum phenomena emerge from distortions in a physical vacuum field described by a complex scalar , with as the amplitude (inertial density) and as the phase (coherence and oscillatory behavior). This theory eliminates the need for dark matter particles by attributing gravitational effects in galaxy clusters, such as those observed in the Bullet Cluster (1E 0657-56), to vacuum stress-energy contributions that behave collisionlessly during mergers. We derive the core DVFT equations, including the Lagrangian, stress-energy tensor, and field equations, and apply them to the Bullet Cluster. Calculations show that vacuum perturbations align with collisionless galaxies, reproducing the observed lensing offset (~250 kpc) and effective mass (~2.0 × 10^{14} M_\odot within 250 kpc) using only baryonic mass, matching Chandra X-ray and HST lensing data. DVFT resolves Bullet Cluster observations without exotic matter, offering a physical alternative to CDM while aligning with broader cosmological data.

The preparation of a report dealing with such a large domain is almost an impossible task. Because so many different questions, problems and expertises are assembled under the word “Cosmology”, my approach has been the following: first to divide this field in a somewhat arbitrary fashion into the following sections: very early universe – elementary particle and cosmology – early nucleosynthesiscosmological parameters (Hubble constant, deceleration parameter, cosmological constant) – large scale structures, intergalactic gas, missing mass – clusters of galaxies and intercluster gas – anisotropy of the black body radiation – formation of galaxies – quasars and their evolution – cosmological evolution of radiosources. I have then asked to the most knowledgeable specialists to review briefly each of these most important questions on which many excitinq and very new results have been obtained not only by the astrophysicists themselves but also by particle physicists, nuclear physicists, theoretical physicists, … This is why the reader will read in section 1 the report on primordial nucleosynthesis written by G. Steigman, in section 2 Anisotropy of the black body radiation by D.T. Wilkinson and E. Meichiorri, in section 3 Clusters of galaxies by 3. Einasto, in section 4 Galaxy formation by B.J.T. Jones, in section 5 Quasars and their evolution by M. Schmidt and in section 6 the Cosmological evolution of radio sources by R.A. Windhorst. Let me thank these colleagues for their excellent work in writing these various reviews.

The mass function of galaxy clusters is a sensitive tracer of the gravitational evolution of the cosmic large-scale structure and serves as an important census of the fraction of matter bound in large structures. We obtain the mass function by fitting the observed cluster X-ray luminosity distribution from the REFLEX galaxy cluster survey to models of cosmological structure formation. We marginalise over uncertainties in the cosmological parameters as well as those of the relevant galaxy cluster scaling relations. The mass function is determined with an uncertainty less than 10% in the mass range 3 x 10^12 to 5 x 10^14 M$_\odot$. For the cumulative mass function we find a slope at the low mass end consistent with a value of -1, while the mass rich end cut-off is milder than a Schechter function with an exponential term exp($- M^\delta$) with $\delta$ smaller than 1. Changing the Hubble parameter in the range $H_0 = 67 - 73 km s^-1 Mpc^{-1}$ or allowing the total neutrino mass to have a value between 0 - 0.4 eV causes variations less than the uncertainties. We estimate the fraction of mass locked up in galaxy clusters: about 4.4% of the matter in the Universe is bound in clusters (inside $r_200$) with a mass larger than 10^14 M$_\odot$ and 14% to clusters and groups with a mass larger than 10^13 M$_\odot$ at the present Universe. We also discuss the evolution of the galaxy cluster population with redshift. Our results imply that there is hardly any clusters with a mass > 10^15 M$_\odot$ above a redshift of z = 1.

SPECIALTY GRAND CHALLENGE article Front. Immunol., 11 August 2011Sec. Cancer Immunity and Immunotherapy volume 2 - 2011 | https://doi.org/10.3389/fimmu.2011.00034

We consider how galaxy clustering data, from Mpc to Gpc scales, from upcoming large scale structure surveys, such as Euclid and DESI, can provide discriminating information about the bispectrum shape arising from a variety of inflationary scenarios. Through exploring in detail the weighting of shape properties in the calculation of the halo bias and halo mass function we show how they probe a broad range of configurations, beyond those in the squeezed limit, that can help distinguish between shapes with similar large scale bias behaviors.We assess the impact, on constraints for a diverse set of non-Gaussian shapes, of galaxy clustering information in the mildly non-linear regime, and surveys that span multiple redshifts and employ different galactic tracers of the dark matter distribution. Fisher forecasts are presented for a Euclid-like spectroscopic survey of Hα-selected emission line galaxies (ELGs), and a DESI-like survey, of luminous red galaxies (LRGs) and [O-II] doublet-selected ELGs, in combination with Planck-like CMB temperature and polarization data.While ELG samples provide better probes of shapes that are divergent in the squeezed limit, LRG constraints, centered below z<1, yield stronger constraints on shapes with scale-independent large-scale halo biases, such as the equilateral template. The ELG and LRG samples provide complementary degeneracy directions for distinguishing between different shapes. For Hα-selected galaxies, we note that recent revisions of the expected Hα luminosity function reduce the halo bias constraints on the local shape, relative to the CMB. For galaxy clustering constraints to be comparable to those from the CMB, additional information about the Gaussian galaxy bias is needed, such as can be determined from the galaxy clustering bispectrum or probing the halo power spectrum directly through weak lensing. If the Gaussian galaxy bias is constrained to better than a percent level then the LSS and CMB data could provide complementary constraints that will enable differentiation of bispectrum with distinct theoretical origins but with similar large scale, squeezed-limit properties.

After the enthusiasm raised by the discovery of multiple quasars and a few years later of giant luminous arcs in clusters of galaxies, gravitational lensing has proven to be a versatile tool to study a broad range of astrophysical problems. I will illustrate recent results obtained in several domains such as: the mass determination for galaxies and clusters of galaxies, the mapping of large scale structures, and the use of lenses to constrain the Hubble constant.

Dark Energy dominates the mass-energy content of the universe (about 73%) but we do not understand it. Most of the remainder of the Universe consists of Dark Matter (23%), made of an unknown particle. The problem of the origin of Dark Energy has become the biggest problem in astrophysics and one of the biggest problems in all of science. The major extant X-ray observatories, the Chandra X-ray Observatory and XMM-Newton, do not have the ability to perform large-area surveys of the sky. But Dark Energy is smoothly distributed throughout the universe and the whole universe is needed to study it. There are two basic methods to explore the properties of Dark Energy, viz. geometrical tests (supernovae) and studies of the way in which Dark Energy has influenced the large scale structure of the universe and its evolution. DUO will use the latter method, employing the copious X-ray emission from clusters of galaxies. Clusters of galaxies offer an ideal probe of cosmology because they are the best tracers of Dark Matter and their distribution on very large scales is dominated by the Dark Energy. In order to take the next step in understanding Dark Energy, viz. the measurement of the 'equation of state' parameter 'w', an X-ray telescope following the design of ABRIXAS will be accommodated into a Small Explorer mission in lowearth orbit. The telescope will perform a scan of 6,000 sq. degs. in the area of sky covered by the Sloan Digital Sky Survey (North), together with a deeper, smaller survey in the Southern hemisphere. DUO will detect 10.000 clusters of galaxies, measure the number density of clusters as a function of cosmic time, and the power spectrum of density fluctuations out to a redshift exceeding one. When combined with the spectrum of density fluctuations in the Cosmic Microwave Background from a redshift of 1100, this will provide a powerful lever arm for the crucial measurement of cosmological parameters.

The importance of the problem under investigation is determined by the role of theatrical art in shaping the social and political position of the Volga region's population at the beginning of the twentieth century. The possibility of usage of the cultural and historical experience for the development of state policy in the sphere of preservation and development of historical memory, since in the period of major socio-cultural changes not only redefining the country's history happens, but also deliberately

Agriculture has served as a major contributor for the China’s rapid economic development over past decades. However, agroecosystems in this coutry have been intensively invaded by invasive alien species (IAS), in particular since the beginning of twentieth century, which cause huge losses to economy and ecological service values each year. Moreover, now China agroecosystems are at the stage of being introduced with new IAS at a greater rate due to rapid growth in international trade and human activities. And, a number of dangerous IAS already introduced are continuing to expand rapidly. For these reasons, biological invasions in China agroecosystems have attracted great attention since the beginning of this century, both from governments and research institutions. In this chapter, we first depict the status of IAS in China agroecosystems regarding their diversity, source, distribution, spread and damage, and the factors perceived to have contributed to the IAS introduction and spreading in this country. Then, we show the invasibility of China agroecosystems. The major findings of researches regarding invasiveness of IAS in China are reviewed. Next, invasiveness and the underlying invasion mechanisms of some serious IAS were reviewed. Lastly, the major approaches employed for control of IAS in China agroecosystems were presented, including risk analysis, detection, monitoring, regional prevention, biological control, replacement control, breeding and use of resistant crop cultivars, as well as integrated use of invasive plants. The trend of introducing new IAS into China agroecosystems and the corresponding tactics to be taken for dealing with IAS in the future were discussed.

The article highlights the history and features of parliamentarism development in the Latin America countries. In addition, the need for training on the subject and the effect of increasing students and educators’ awareness in this field is examined. This process was lengthy, replete with the examples of various social groups, political trends and parties struggle intensity increase. Since the beginning of the 19th century, there have been almost no favorable conditions for the practical implementation of democratic government in the countries of Latin America, and the institutionalization of the party system has not taken place yet. However, there have been exceptions to the general rule in the history of Latin America. Chile and Argentina were such an example. The success of democratic transformations in the countries of the region depended on various reasons: a) whether the country had a democratic experience in its past; b) the conditions for the political and economic development of this country to develop representative institutions in the future; c) the importance of the parties in the political course development and the adoption of state decisions. The results of democracy and parliamentarism development in the states of Latin America are rather complicated by the turn of the 20th and 21st centuries. On the one hand, the last decades of the XX-th century and the beginning of this century was marked by the democratization of political life, reforms, and the replacement of military regimes with civilian governments. Since the beginning of the 60-ies, they started the process of democratization and formation of independent island states in the Caribbean and Central America. Despite the successful development of the economy, culture, education, the presence of a large middle class in Argentina, the military governments overcame civilian ones in the 30-70-ies. Therefore, it is needed to consider this aspect as a part of education system to improve the educators’ level.

In this paper, we use large scale structure observations to test the redshift dependence of cosmic distance duality relation (CDDR), D_mathrm{L}(1+z)^{-2}/D_mathrm{A}=eta (z), with D_mathrm{L} and D_mathrm{A}, being the luminosity and angular diameter distances, respectively. In order to perform the test, the following data set are considered: strong lensing systems and galaxy cluster measurements (gas mass fractions). No specific cosmological model is adopted, only a flat universe is assumed. By considering two eta (z) parametrizations, It is observed that the CDDR remain redshift independent within 1.5sigma which is in full agreement with other recent tests involving cosmological data. It is worth to comment that our results are independent of the baryon budget of galaxy clusters.

An analysis of the Molonglo Reference Catalogue indicates that significant departures from isotropy are present in the sky distribution of strong extragalactic radio sources. This has been shown to be due to local large scale structure, specifically a concentration to the supergalactic plane, which also influences the slope of the source counts. A study of the three-dimensional distribution of local radio galaxies shows that they are more strongly concentrated to the supergalactic plane than are optically�selected galaxies, and that the supergalactic concentration is more extensive than hitherto believed. It appears that radio galaxies (and clusters of galaxies) trace the 'skeleton' of large scale structure, about which normal galaxies are more loosely distributed. Thus, while large scale structure evidently complicates the interpretation of radio source counts, it appears that radiO surveys can be of value in exploring structures on the largest scales.

The cosmic stories : beginning, evolution, and present days of the universe