Early formation of galaxies induced by clusters of black holes

A model for the formation of supermassive black holes at the center of a cluster of primordial black holes is developed. It is assumed that ～10^?3 of the mass of the Universe consists of compact clusters of primordial black holes that arose as a result of phase transitions in the early Universe. These clusters also serve as centers for the condensation of dark matter. The formation of protogalaxies with masses of the order of 2 × 10⁸ M _⊙ at redshift z = 15 containing clusters of black holes is investigated. The nuclei of these protogalaxies contain central black holes with masses ～10⁵ M _⊙, and the protogalaxies themselves resemble dwarf spherical galaxies with their maximum density at their centers. Subsequent merging of these induced protogalaxies with ordinary halos of dark matter leads to the standard picture for the formation of the large-scale structure of the Universe. The merging of the primordial black holes leads to the formation of supermassive black holes in galactic nuclei and produces the observed correlation between the mass of the central black hole and the bulge velocity dispersion.     

Black holes in close binary systems and galactic nuclei

After 50 years of observational studies of black holes, great progress has been achieved in this branch of astrophysics. Several dozen stellar-mass black holes have been discovered in X-ray binaries, and several hundred supermassive black holes in galactic nuclei. The remarkable recent discovery of gravitational waves from merging black holes in a binary system by LIGO marks the beginning of a new stage in black-hole research. It is quite possible that gravitational-wave studies will provide definitive evidence for the existence of event horizons in black holes in the near future. On the other hand, the development of methods for space and ground-based radio-interferometry observations provides hope that it will be possible to obtain images of “shadows” of supermassive black holes in galactic nuclei, and to observe directly processes occurring in the vicinities of the event horizons of supermassive black holes. This is important for tests of general relativity in extremely strong gravitational fields.     

Merging of components in close binaries: Type Ia supernovae,massive white dwarfs,and Ap stars

The “Scenario Machine” (a computer code designed for studies of the evolution of close binaries) was used to carry out a population synthesis for a wide range of merging astrophysical objects: main-sequence stars with main-sequence stars; white dwarfs with white dwarfs, neutron stars, and black holes; neutron stars with neutron stars and black holes; and black holes with black holes. We calculate the rates of such events, and plot the mass distributions for merging white dwarfs and main-sequence stars. It is shown that Type Ia supernovae can be used as standard candles only after approximately one billion years of evolution of galaxies. In the course of this evolution, the average energy of Type Ia supernovae should decrease by roughly 10%; the maximum and minimum energies of Type Ia supernovae may differ by no less than by a factor of 1.5. This circumstance must be taken into account at estimating the parameters of the Universe expansion acceleration. According to theoretical estimates, the most massive—as a rule, magnetic—white dwarfs probably originate from mergers of white dwarfs of lower mass. At least some magnetic Ap and Bp stars may form in mergers of low-mass main-sequence stars (M ? 1.5 M _⊙) with convective envelopes.     

湘西北黑色岩系中的镍钼矿床及其贵金属矿化特征

湖南西北部下寒武统黑色岩系蕴藏着丰富的镍钼钒多金属矿床及其伴生的Au,Ag,Pt,Pd等贵金属矿化。它是我国新类型的镍钼矿床及贵金属矿化极具找矿潜力的地区。富含有机质和黄铁矿的黑色岩系既是镍钼矿的富集层,也是贵金属矿化的主要富集层。矿床的成矿作用是伴随热水的加入而开始,热水沉积与正常沉积交替期是成矿的高峰期,至正常沉积期结束。生物及生物地球化学作用在黑色岩系的成岩成矿过程中起了重要作用。矿床以同生沉积为主,兼有热水性质沉积特点。其成因应归属于生物地球化学沉积矿床范畴。     

Supermassive black holes in interacting galaxies

The possible influence of galactic interaction on the formation and growth of supermassive black holes in their nuclei and the dynamics of their circumnuclear regions are considered, based on new data from the updated Vorontsov-Velyaminov catalog of interacting galaxies and modern estimates of the masses of supermassive black holes. A sample of interacting galaxies with known black-hole masses is created, and the dependence of the masses of the central black holes on the absolute B magnitudes and central stellar velocity dispersions in the host galaxy derived for this sample. A statistical analysis of the sample shows that the black-hole masses in interacting galaxies satisfy the same mass-velocity dispersion relation as non-interacting galaxies. A higher mass dispersion is characteristic of merging pairs than for galaxies that interact in other ways. The maximum masses of the central black holes are observed in radio galaxies.     

Formation of close binary black holes merging due to gravitational-wave radiation

The conditions for the formation of close-binary black-hole systems merging over the Hubble time due to gravitational-wave radiation are considered in the framework of current ideas about the evolution of massive close-binary systems. The original systems whose mergers were detected by LIGO consisted of main-sequence stars with masses of 30–100M _⊙. The preservation of the compactness of a binary black hole during the evolution of its components requires either the formation of a common envelope, probably also with a low initial abundance of metals, or the presence of a “kick”—a velocity obtained during a supernova explosion accompanied by the formation of a black hole. In principle, such a kick can explain the relatively low frequency of mergers of the components of close-binary stellar black holes, if the characteristic speed of the kick exceeds the orbital velocities of the system components during the supernova explosion. Another opportunity for the components of close-binary systems to approach each other is related to their possible motion in a dense molecular cloud.     

Acceleration of spatial motions of stars by close-binary supermassive black holes in galactic nuclei

The conditions for the acceleration of the spatial motions of stars by close-binary supermassive black holes (SMBHs) in galactic nuclei are analyzed in order to derive the velocity distribution for stars ejected from galaxies by such black holes. A close binary system consisting of two SMBHs in circular orbits was subject to a spherically symmetrical “barrage” of solar-mass stars with various initial velocities. The SMBHs were treated as point objects with Newtonian gravitational fields. Models with binary component-mass ratios of 1, 0.1, 0.01, and 0.001 were studied. The results demonstrate the possibility of accelerating neutron stars, stellar-mass black holes, and degenerate dwarfs to velocities comparable to the relative orbital velocities of the binary-SMBH components. In the stage when the binary components are merging due to the action of gravitational-wave radiation, this velocity can approach the speed of light. The most massive binary black-holes (M ? 10⁹M_⊙) can also accelerate main-sequence stars with solar or subsolar masses to such velocities.     

Statistics of Stars with Relativistic Velocities

The scenario for the dynamical capture of a binary system in the neighborhood of a supermassive black hole used byHills in 1988 to predict the existence of hypervelocity stars (~1000 km/s) allows the existence of stars with relativistic velocities attaining (1/3?2/3)c, where c is the speed of light. The increase of the kinetic energy of these stars by more than a factor of 100 is due to the replacement of one component of the binary with a supermassive black hole. This scenario takes candidate of relativisti©velocity stars outside our Galaxy, into intergalactic space, where they could be ejected from merging galaxies populated by supermassive black holes. At present, this is a hypothetical class of stars with anomalous kinematics, but it is already posing a serious challenge for modern astrometry, which, like 300 years ago, is still concerned with the detection of proper motions. While this was related to stars in the solar neighborhood at the time of Halley, is now a problem for studies of the most remote and weakest stars in intergalactic space. Possibilities for detecting such stars must be based on estimates of their abundances, that is, on their statistics. This paper is based on a presentation made at the conference “Modern Astrometry 2017,” dedicated to the memory of K.V. Kuimov (Sternberg Astronomical Institute, Moscow State University, October 23–25, 2017).

     

考虑有雨无雨辨识的多源降水融合方法

多源降水融合是精准估计降水时空分布的重要途径,多聚焦降水量或降水强度的误差订正,对短历时降水雨区辨识的重视不足。提出考虑有雨无雨辨识的多源降水融合框架,耦合地理加权逻辑回归与地理加权回归模型,构建兼顾雨区辨识及雨量估计的降水融合方法,并应用于汉江流域MSWEP V2.1与地面站网观测日降水融合。结果表明：所提方法成功再现有雨无雨空间格局并刻画了降水中心,整体强化了MSWEP V2.1对地面降水的表征能力,降低误报率和误报降水量的幅度超过了60%,提高临界成功指数和Kling-Gupta效率系数达40%以上;较降水空间插值数据,削减误报降水量并提升Kling-Gupta效率系数高于10%;另外,较参考数据,降水融合改善强降水事件(雨强≥50 mm/d)分辨精度的增益不低于60%。所提方法有效改善了降水估计效果,为多源降水融合提供了新思路。     

地质约束条件下的地质体智能综合方法研究

地质体综合是地质图编制工作的重中之重,因其处理涉及内容多、 业务逻辑复杂、 重复工作量大,是影响编图工作推进的主要因素.为了能够实现地质体的高效综合,文章提出了一种以地质约束条件(专家知识)为核心、 以制图综合为空间图形合并手段的新型地质体智能综合方法,设计并实现了围绕地质专家知识(如地质年代、 地层名称等)规则映射开...     

四川盆地下古生界黑色页岩纳米孔隙形态的影响因素及其地质意义

以场发射扫描电镜与Pores and Cracks Analysis System （PCAS） 图像处理软件为主要研究手段,以形状系数为孔隙形态表征参数,并选取低压N2吸附等为辅助研究手段,对四川盆地及周缘地区的典型钻井A-D 井龙马溪组及筇竹寺组黑色页岩中纳米孔隙的形态特征进行定量研究。研究发现黑色页岩纳米孔隙形态受孔隙类型（赋存位置）、有机质显微组分、地层埋藏深度、热成熟度及孔隙尺寸等因素综合控制。具体体现在：（1） 有机质孔、粒间孔和粒内孔所占比例、孔径分布与孔隙形态具有明显差异,反映这三类孔隙的演化受成岩作用的影响不同。（2） 固体沥青纳米孔隙比其他显微组分中的纳米孔隙更加规则。（3） 与埋藏深度密切相关的压实作用很可能会在垂向上压缩孔隙,一方面令孔径缩小,另一方面让孔隙形态往狭长–裂缝形发展。（4） 有机质孔形态随热成熟度升高总体上会变得更加规则,但这种趋势可能会被孔隙间的合并及压实作用等破坏。（5） 面积更小的孔隙形态往往比面积更大的孔隙更规则。初步研究显示固体沥青纳米孔隙形态代表着高过成熟页岩气储层中主体储集空间所处压力环境,但固体沥青纳米孔隙形态随孔隙压力的演化模式及利用固体沥青纳米孔隙形态表征其所在层系异常高压维持状况及页岩气保存状况的可能性尚需进一步研究。     

四川盆地下古生界黑色页岩纳米孔隙形态的影响因素及其地质意义

以场发射扫描电镜与Pores and Cracks Analysis System （PCAS） 图像处理软件为主要研究手段，以形状系数为孔隙形态表征参数，并选取低压N2吸附等为辅助研究手段，对四川盆地及周缘地区的典型钻井A-D 井龙马溪组及筇竹寺组黑色页岩中纳米孔隙的形态特征进行定量研究。研究发现黑色页岩纳米孔隙形态受孔隙类型（赋存位置）、有机质显微组分、地层埋藏深度、热成熟度及孔隙尺寸等因素综合控制。具体体现在：（1） 有机质孔、粒间孔和粒内孔所占比例、孔径分布与孔隙形态具有明显差异，反映这三类孔隙的演化受成岩作用的影响不同。（2） 固体沥青纳米孔隙比其他显微组分中的纳米孔隙更加规则。（3） 与埋藏深度密切相关的压实作用很可能会在垂向上压缩孔隙，一方面令孔径缩小，另一方面让孔隙形态往狭长–裂缝形发展。（4） 有机质孔形态随热成熟度升高总体上会变得更加规则，但这种趋势可能会被孔隙间的合并及压实作用等破坏。（5） 面积更小的孔隙形态往往比面积更大的孔隙更规则。初步研究显示固体沥青纳米孔隙形态代表着高过成熟页岩气储层中主体储集空间所处压力环境，但固体沥青纳米孔隙形态随孔隙压力的演化模式及利用固体沥青纳米孔隙形态表征其所在层系异常高压维持状况及页岩气保存状况的可能性尚需进一步研究。     

Pulse propagation in turbidity currents

Submarine turbidity currents are a key mechanism in the transportation of clastic sediments to deep seas. Such currents may initiate with a complex longitudinal flow structure comprising flow pulses (for example, by being sourced from retrogressive sea floor slope failures) or acquire such structure during run‐out (for example, following flow combination downstream of confluences). A key question is how far along channel pathway complex flow structure is preserved within turbidity currents as they run out and thus if flow initiation mechanism and proximity to source may be inferred from the vertical structure of their deposits. To address this question, physical modelling of saline flows has been conducted to investigate the dynamics of single‐pulsed versus multi‐pulsed density driven currents. The data suggest that, under most circumstances, individual pulses within a multi‐pulsed flow must merge. Therefore, initiation signatures will only be preserved in deposits upstream of the merging point and may be distorted approaching it; downstream of the merging point, all initiation signals will be lost. This new understanding of merging phenomenon within multi‐pulsed gravity currents broadens our ability to interpret multi‐pulsed turbidites.     

Type Ia supernovae: Non-standard candles of the universe

We analyze the influence of the evolution of light absorption by gray dust in the host galaxies of type Ia supernovae (SN Ia) and the evolution of the mean combined mass of close-binary carbon-oxygen white dwarfs merging due to gravitational waves (SN Ia precursors) on the interpretation of Hubble diagrams for SN Ia. A significant increase in the mean SN Ia energy due to the higher combined masses of merging dwarfs should be observable at redshifts z > 2. The observed relation between the distance moduli and redshifts of SN Ia can be interpreted not only as evidence for accelerated expansion of the Universe, but also as indicating time variations of the gray-dust absorption of light from these supernovae in various types of host galaxies, observational selection effects, and the decreasing mean combined masses of merging degenerate dwarfs.     

Seismic events discrimination by neuro-fuzzy merging of signal and catalogue features

This article presents an original method for the classification of low magnitude seismic events recorded in France by a network of seismometers. Three types of events are discriminated: earthquakes, mining blasts and rock bursts. This method is based on a merging of catalogue measurements and possibly incomplete measurements deduced from several seismic signals related to the event. The merging is performed by a multi-layer neural network. A fuzzy coding is applied to the input characteristics of the neural network. It allows the network to integrate data imperfections during the learning phase. Then, it is possible to process efficiently incomplete data. The results are obtained on a database composed of all the 1,402 seismic events recorded between August 23^rd 1993 and May 30^th 1994. They show that the fuzzy coding and the merging of catalogue features and signal features extracted from several seismometers for each event increase the performance of correct classification to more than 90% even when the database contains missing values. The confusion rate between earthquakes and mining blasts is simultaneously reduced.     

基于遥感图像分割和形态学的黄土滑坡后壁自动提取方法

基于黄土滑坡后壁的光谱和形状特征,提出了利用区域生长合并方法分割高分辨率遥感影像,提取滑坡后壁区域,经过二值化构图处理后,获得滑坡后壁主要格架,以表征黄土滑坡的方法。首先充分考虑黄土滑坡后壁在遥感影像中所呈现出的独特光谱特征和半圆状或圈椅状的形状特征,利用区域生长合并的方法,在生长参数为47.5,合并参数49的状态下进行影像分割,获得初步的黄土滑坡后壁形状;其次,填充分割过程中产生的孔洞,对获得的滑坡后壁进行细部构图;最后,采用二值化骨骼提取算法,提取滑坡后壁的主要格架,作为黄土滑坡的标志。该方法是对黄土滑坡遥感解译工作中,滑坡表达方法的改进和提高。     

基于专家知识的地质体制图综合方法研究

传统数字地质编图的地质体处理过程中存在重复操作多、制图周期长等缺点,极大地限制了地质编图的工作效率.为提高工作效率,笔者提出以地质专家知识驱动的地质体制图综合方法,主要包括地质体合并(自动同属性合并、交互式合并)、消除微小地质体、地质体夸大、地质体圆滑等.该方法以地质专家总结的地质演化关系知识为主线,采用GI S组件、...     

A new phase field model for mixed-mode brittle fractures in rocks modified from triple shear energy criterion

Acta Geotechnica - Fracture initiation, propagation, merging and branching in rocks are considerably complicated and commonly exhibit a great variety of patterns. How to characterize and capture...     

Analysis of the 1 November 2015 heavy rainfall episode in Algarve by using weather radar and rain gauge data

The trigger for the study presented in this paper was the extreme rain event of 1 November 2015 in Algarve region. The main objective was the analysis and improvement of the precipitation field using a radar–rain gauge merging method. Ordinary kriging with radar-based error correction has been applied to hourly values of precipitation from both sensors. The merging technique allowed keeping the better radar spatial pattern, being the respective estimates corrected by the rain gauges observations. The procedure led to a reduction in the errors of the precipitation estimates, evaluated by cross-validation, when compared to univariate interpolation of rain gauge observation or radar rain product. Finally, some discussion is also added on the problematic of flooding in urban areas, especially those with absent or deficient urban planning.     

Analysis of the 1 November 2015 heavy rainfall episode in Algarve by using weather radar and rain gauge data

The trigger for the study presented in this paper was the extreme rain event of 1 November 2015 in Algarve region. The main objective was the analysis and improvement of the precipitation field using a radar–rain gauge merging method. Ordinary kriging with radar-based error correction has been applied to hourly values of precipitation from both sensors. The merging technique allowed keeping the better radar spatial pattern, being the respective estimates corrected by the rain gauges observations. The procedure led to a reduction in the errors of the precipitation estimates, evaluated by cross-validation, when compared to univariate interpolation of rain gauge observation or radar rain product. Finally, some discussion is also added on the problematic of flooding in urban areas, especially those with absent or deficient urban planning.