Development of the geometric structure of the thermonuclear-deflagration front in type Ia supernovae

Three-dimensional hydrodynamical simulations of the development of a large-scale instability accompanying deflagration in the degenerate cores of rotating white dwarfs—progenitors of type-Ia supernovae—are presented. The numerical algorithm used is described in detail. An explicit, conservative, Godunov-type TVD difference scheme was employed for the computations. Large-scale convective processes are important as the deflagration front propagates. The supernova explosion is strongly nonspherically symmetric; a large-scale front structure emerges and propagates most rapidly along the rotational axis. The arrival of fresh thermonuclear fuel to the central region of the core can result in flares and the destruction of the core.     

The role of large-scale convection in supernovae explosions

We present the results of simulations of Type Ia and II supernovae explosions taking into account the rotation of the initial configuration. The main idea is development of a large-scale convective instability which affects strongly the geometry of the explosion. For Type Ia supernova a jet-like structure of the ejecta was obtained. An important point here is the possibility of continuing consecutive flares, produced when the fresh thermonuclear fuel is ignited in the central part of the star. This fuel is moved to the center by convective fluxes from the outer stellar layers. For Type II supernova a large-scale convection results in a non-equilibrium neutronization of the matter. Large bubbles, moving to the surface, contain high-energy neutrinos from the central region of the proto-neutron stellar core. The following ejection of these neutrinos to the stellar envelope gives enough energy support to the bounce shock, which finally destroys the envelope producing a non-spherical explosion.     

Supernova explosion mechanism taking into account large-scale convection and neutrino transport

Two types of supernovae are considered: thermonuclear supernovae, whose explosions are due to thermonuclear energy, and core-collapse supernovae, whose explosions are due to the gravitational energy of collapsing stars released in the form of neutrinos. Numerical models of supernovae are discussed. Themain problem in devising supernova explosion mechanisms is producing the energy required to disperse the envelope. In theoretical models, it is necessary to solve multi-dimensional problems involving complex physics (3D gas dynamics, neutrino transport, large-scale convective instability, and other important physical processes). In recent years, the development of large-scale convection during supernova explosions has been reconsidered. Self-consistent problems problems in three-dimensional, gas-dynamical instability have been considered. Two-dimensional gas-dynamical calculations taking into account neutrino absorption in the envelope have been performed. The spherically symmetric collapse and neutrino transport were calculated including all reactions, leading to a new understanding of possible paths for the development of supernova theory. The main emphasis is placed on the neutrino transport and the basis for promising multidimensional models taking into account large-scale convective instability.     

放射性氡气测量动态监测煤炭地下气化燃空区

煤炭地下气化是将地下的煤炭进行有控制的燃烧,为了使煤的燃烧和气化得到有效的控制,了解燃烧的火焰工作面的移动速度以及燃空区的范围是致关重要的。唐山刘庄煤矿地下气化区的试验中,分析了放射性测氡法在进行煤炭地下气化监测中确定燃烧火焰工作面的移动速度及以燃空区范围的可行性和有效性,从而提出一些建议。     

Large-scale Instability during Gravitational Collapse with Neutrino Transport and a Core-Collapse Supernova

Most of the energy released in the gravitational collapse of the cores of massive stars is carried away by neutrinos. Neutrinos play a pivotal role in explaining core-collape supernovae. Currently, mathematical models of the gravitational collapse are based on multi-dimensional gas dynamics and thermonuclear reactions, while neutrino transport is considered in a simplified way. Multidimensional gas dynamics is used with neutrino transport in the flux-limited diffusion approximation to study the role of multi-dimensional effects. The possibility of large-scale convection is discussed, which is interesting both for explaining SN II and for setting up observations to register possible high-energy (?10MeV) neutrinos from the supernova. A new multi-dimensional, multi-temperature gas dynamics method with neutrino transport is presented.     

Features of the matter flows in the peculiar cataclysmic variable AE Aquarii

The structure ofmatter flows in close binary systems in which one of the components is a rapidly rotating magnetic white dwarf is studied. Themain example considered is the AEAquarii system; the period of the white dwarf’s rotation is about a factor of 1000 shorter than the orbital period, and the magnetic field on the white-dwarf surface is of order 50MG. The matter flows in this system were analyzed via numerical solution of a systemofmagnetohydrodynamical equatons. These computations show that the white dwarf’s magnetic field does not significantly influence the velocity field of the matter in its Roche lobe in the case of a laminar flow regime, so that the field does not hinder the formation of a transient disk (ring) surrounding the magnetosphere. However, the efficiency of the energy and angular-momentum exchange between the white dwarf and the surrounding matter increases considerably with the development of turbulent motions in the matter, accelerating the matter at the magnetosphere boundary and leading to a high escape rate from the system. The time scales for the system’s transition between the laminar and turbulent modes are close to those for the transition of AE Aquarii between its quiet and active phases.     

Collective supernova outbursts and the growth of supershells: Observational manifestations

Numerous supernova outbursts that are correlated in time and space are the main mechanism for the formation of powerful galactic winds and supershells of ionized hydrogen. Information about the dynamics and thermal properties of the gas in shells (bubbles) can be obtained from spectral observations, including those of optical recombination lines. The emission properties of the Hα and Hβ recombination lines and the velocity dispersion of the gas in bubbles formed by numerous supernova outbursts are studied. The appearance of the intensity vs. velocity dispersion (I(H _α)_?σ) diagram depends on the supernova rate and the age of the bubble. The temperature dependence of the I(H_α)/I(H _β) line-intensity ratio (the Balmer decrement) can be used to obtain additional constraints on the evolutionary status of a collective remnant formed by numerous supernova outbursts.     

Observations of five supernovae in 1995–1997

We present the results of photometric observations of the type Ia supernovae SN 1995al, 1996bo, 1996bk, the type Ib/c supernova SN 1997X, and the type II supernova SN 1996an. The photometric characteristics of SN 1995al are close to the average for type Ia supernovae. Our analysis has revealed possible peculiarities in the light-curve shape and deviations from the average photometric parameters for SN 1996bk and 1996bo. Sn 1996an probably belongs to type IIP. The light curve of SN 1997X resembles that of the type Ic supernova SN 1994I. Light-curve parameters and absolute magnitude estimates are presented.     

Late stages of the evolution of close compact binaries: Type I supernovae,gamma-ray bursts,and supersoft X-ray sources

We consider the evolution of close binaries resulting in the most intensive explosive phenomena in the stellar Universe—Type Ia supernovae and gamma-ray bursts. For Type Ia supernovae, which represent thermonuclear explosions of carbon-oxygen dwarfs whose masses reach the Chandrasekhar limit during the accretion of matter from the donor star, we derive the conditions for the accumulation of the limiting mass by the degenerate dwarf in the close binary. Accretion onto the degenerate dwarf can be accompanied by supersoft X-ray radiation with luminosity 1–10⁴ L _⊙. Gamma-ray bursts are believe to accompany the formation and rapid evolution of compact accretion-decretion disks during the formation of relativistic objects—black holes and neutron stars. The rapid (～1 M _⊙/s) accretion of matter from these disks onto the central compact relativistic star results in an energy release of ～0.1 M _⊙ c ² ～ 10⁵³ erg in the form of gamma-rays and neutrinos over a time of 0.1–1000 s. Such disks can form via the collapse of the rapidly rotating cores of Type Ib, Ic supernovae, which are components in extremely close binaries, or alternately due to the collapse of accreting oxygen-neon degenerate dwarfs with the Chandrasekhar mass into neutron stars, or the merging of neutron stars with neutron stars or black holes in close binaries. We present numerical models of the evolution of some close binaries that result in Type Ia supernovae, and also estimate the rates of these supernovae (～0.003/year) and of gamma-ray bursts (～10^?4/year) in our Galaxy for various evolutionary scenarios. The collimation of the gamma-ray burst radiation within an opening angle of several degrees “matches” the latter estimate with the observed rate of these events, ～10^?7–10^?8/year calculated for a galaxy with the mass of our Galaxy.     

煤层气排采非饱和流阶段煤粉–气泡耦合作用机理

揭示煤层气排采储层非饱和流阶段煤粉与气体相互作用机理,对制定排采制度和提高产气量具有重要意义。通过气泡–煤粉微观作用实验装置,系统开展了不同直径大小的气泡对不同粒度和密度煤粉的作用实验,分析了气泡对煤粉运移轨迹和速度的影响及捕获煤粉特征。结果表明,气泡产出能够影响煤粉的运移轨迹,甚至能够捕获煤粉;煤粉通过气泡时会产生3种运动类型：沿着气泡表面运移到气泡底部最后被捕获、沿着气泡表面运移到气泡底部最后脱落及接近气泡时被排斥而轨迹发生偏转。煤粉若被气泡捕捉,则运动速度呈现出减小–增大–减小的变化特征;若未被气泡捕获,速度呈现出减小–增大–减小–增大的变化特征。不同条件下气泡对煤粉的捕获效率高达64.38%～86.64%;在气泡表面最高点附近发生碰撞煤粉被捕获的概率最大,并且随着偏离角度的增大,气泡捕获效率均呈现出逐渐减小的趋势;在相同的碰撞位置下,气泡对煤粉的捕获效率随着煤粉密度、煤粉粒径的增大而减小,随着气泡直径的增大而增大。煤层气产气初期应根据储层的实际导流能力合理控制降压速率,若储层导流能力较强,应加大排采速率,增大气体解吸对煤粉的扰动和捕获作用,促使大量煤粉随地下水或气泡产出;若储层...     

明渠湍流涡运动尺度分布特性

为了解明渠湍流涡运动尺度沿水深的分布特征,使用高精度粒子图像测速法水槽试验系统测量充分发展的明渠湍流,利用改进后的功率谱分析方法,对明渠湍流涡运动尺度沿水深分布、上升流、下扫流和平均涡量等进行了分析。结果表明:明渠湍流涡运动尺度大小沿水深增加呈先增大后减小;沿水深增加下扫流比上升流更容易发生;各自水深的顺向涡涡量大于逆向涡涡量,在近壁区平均涡量最大;明渠湍流近壁区产生涡量大、尺度小的涡结构,沿水深增加,涡尺度发展变大,但受水面区下扫流抑制,涡尺度又变小。     

煤火区浅部松散煤体及采空区的探地雷达响应特征

探地雷达对浅层勘探具有较高分辨率,为煤田火区浅部松散煤体或采空区等典型火源地质结构探测提供了重要手段。然而如何识别各种火源地质结构体,确定火区重点范围还存在一定的理论不足。基于电磁波理论,采用时域有限差分法正演模拟了火区典型地质体地电模型雷达响应,其特征表现为：松散跨塌煤体对应雷达响应绕射波严重,其内部波形紊乱;空洞区顶界面回波能量强,较为连续,其内部无绕射。正演模拟和现场测试研究表明：探地雷达对识别浅埋火区煤层松散跨落程度,圈定火烧重点区域,减少灭火成本和火区开采安全事故具有重要的现实意义。     

Thermal radio emission and absorption in HII regions in the vicinity of remnants of type II supernovae

Data on thermal radio emission and absorption in and near the directions towards supernova remnants are used to estimate the distribution of ionized gas surrounding remnants of type II supernovae. The amount of absorption and emission toward the supernova remnants are determined by two types of HII regions. The first are extended HII regions around the supernova remnants (Strömgren spheres), while the second are more compact and bright HII regions surrounding early-type stars. In the early stages of evolution of the supernova remnants (1000–3000 yrs), the amount of thermal absorption and emission is minimum, apparently indicating that only the supernova Strömgren zones contribute in these stages, while there is an absence of absorption or emission from the compact HII regions. Possible mechanisms for this scenario are discussed.     

Strmömgren zones of type II supernovae

The emission measures EM in the directions of supernova remnants and pulsars are considered as functions of their ages t. The resulting plot has a well-defined lower boundary, which can be approximated by the expression EM_min∝1/t. The quantity EM_min increases with decreasing age t and does not level off or reach a maximum until t?500 yr. It is concluded that the bulk of the radiative energy that goes into ionizing and heating the interstellar gas is released at early stages of the supernova remnant’s evolution. We suggest that most of the kinetic energy of the supernova shell is converted into thermal energy and radiated at remnant ages t<100 yr, when the supernova shell, which is expanding at an enormous speed (about 10⁴ km/s), overtakes the shell produced by the presupernova in the supergiant stage. We have estimated the ionization energy E?10⁵¹ erg, diameter L?60 pc, and electron density N_e?7 cm^?3 of the HII regions around the supernovae (the supernova Strömgren zones). A list of objects that can be reliably identified as Strömgren zones of type II supernovae is presented. The plot of pulsar pulse broadening τ as a function of the pulsar age t also has a well-defined lower boundary, for which τ∝t^?2 when t≥1000 yr. This suggests that turbulence develops during the first thousand years after the supernova outburst. It is also concluded that turbulence plays an important role in the formation and evolution of the Strömgren zones of type II supernovae.     

Axially symmetrical models of the products of a conservative merger of a binary white dwarf with similar-mass components

The possibility of a conservative merger of a binary white dwarf whose components have similar masses is studied. Axially symmetrical models for single, rapidly rotating white dwarfs that are possible products of such mergers are constructed and their physical characteristics investigated. The merger products must be turbulent, and the viscosity of the electron gas is not sufficient to support the observed luminosities of massive, bright white dwarfs. The amount of dissipative energy and the timescale for its release are estimated.     

Supersoft X-ray sources: Basic parameters

The parameters of ten supersoft X-ray sources observed by ROSAT obtained using blanketing approximations and LTE model atmospheres are analyzed. The consistency of the resulting parameters with a model with stable/recurrent burning on the surface of the white dwarf is studied. The luminosity and sizes of seven of the sources are in good agreement with this model. The masses of the white dwarfs in these sources are estimated. A formula that can be used to estimate the masses of white dwarfs in classical supersoft sources based on their effective temperatures is presented.     

Radiation of a neutrino mechanism for type II supernovae

We propose a new mechanism for type II supernova explosions. An important element of the model is large-scale convection that arises due to non-equilibrium neutronization of the matter in the central region of the proto-neutron star. Our analytical estimates and numerical simulations of the convection rate are in good mutual agreement. Large-scale convection leads to the rapid transport of neutrinos from the center of the star to the bounce shock formed during the pause in the collapse of the stellar matter in the proto-neutron star. The mean neutrino energy is 30–50 MeV. We analyze the dependence of the mean neutrino energy on the size of the convection cells—“bubbles.” Our computations of the interaction between the neutrinos and the shock show that the velocity of the shock along the rotational axis of the star exceeds the escape velocity. Thus, explosion of the envelope and a supernova with a very asymmetrical envelope structure become possible, leading to the formation of a neutron star.     

氧弹燃烧-电位滴定法测定煤中氯

介绍了氧弹燃烧-电位滴定法测定煤中氯离子含量的方法：将样品于加入已知量的碳酸铵溶液的氧弹内燃烧，释放出的氯被碳酸铵溶液吸收后用0．01mol／L的硝酸银标准溶液进行电位滴定。方法的检出限为0．007mg，回收率为96．4％-101．4％。用于实际样品的测定，准确度和精密度与ISO和国标方法相当，但操作简便、快捷。     

Magnetite scavenging and the buoyancy of bubbles in magmas. Part 2: Energetics of crystal-bubble attachment in magmas

The fate of pre-eruptive bubbles depends largely on their buoyancy, which can be strongly modified by the presence of crystals attached to the bubble–melt interface. We define the attachment energy and attachment force as those resulting from the attachment of a crystal to a bubble. The attachment energy is such that (1) attachment of crystals to bubbles is always favored energetically, and (2) oxide minerals attach to bubbles much more strongly than silicates, because the attachment energy is a strong function of the wetting angle. Attaching crystals to bubbles can cause bubble–crystal pairs to become neutrally buoyant. There is a critical bubble radius below which the attachment force will be strong enough to keep the pair together; we show that crystals as large as 1 mm in diameter can form neutrally buoyant pairs. For early erupted Bishop magma, if all magnetite forms neutrally buoyant pairs with gas bubbles, ca. 0.1–0.2 vol% gas can be stored in the magma; 2–3 vol% of gas can be accounted for if all minerals form neutrally buoyant aggregates. These values are an order of magnitude lower than what is inferred from melt inclusions. Hence, both magnetite-free and magnetite-rich bubbles might have existed, but only a very small fraction of them could have been neutrally buoyant. Importantly, an intrinsic association between magnetite crystals and bubbles is expected. However, most magnetite crystals in the early erupted Bishop are free of bubbles; the puzzling conclusion is that nucleation away from crystals is favored over heterogeneous nucleation on crystal substrates. Electronic Supplementary Material The online version of this article (doi:) contains supplementary material, which is available to authorized users.     

Evolution of the first supernovae in protogalaxies: Dynamics of mixing of heavy elements

The paper considers the evolution of the supernova envelopes produced by Population III stars with masses ofM _* ?? 25?C200M _?? located in non-rotating protogalaxies with masses of M ?? 10⁷ M _?? at redshifts z = 12, with dark-matter density profiles in the form of modified isothermal spheres. The supernova explosion occurs in the ionization zone formed by a single parent star. The properties of the distribution of heavy elements (metals) produced by the parent star are investigated, as well as the efficiency with which they are mixed with the primordial gas in the supernova envelope. In supernovae with high energies (E ? 5 × 10⁵² erg), an appreciable fraction of the gas can be ejected from the protogalaxy, but nearly all the heavy elements remain in the protogalaxy. In explosions with lower energies (E ? 3 × 10⁵² erg), essentially no gas and heavy elements are lost from the protogalaxy: during the first one to threemillion years, the gas and heavy elements are actively carried from the central region of the protogalaxy (r ?? 0.1r _v , where r _v is the virial radius of the protogalaxy), but an appreciable fraction of the mass of metals subsequently returns when the hot cavity cools and the envelope collapses. Supernovae with high energies (E ? 5 × 10⁵² erg) are characterized by a very low efficiency of mixing of metals; their heavy elements are located in the small volume occupied by the disrupted envelope (in a volume comparable with that of the entire envelope), with most of the metals remaining inside the hot, rarified cavity of the envelope. At the same time, the efficiency of mixing of heavy elements in less energetic supernovae (E ? 3 × 10⁵² erg) is appreciably higher. This comes about due to the disruption of the hot cavity during the collapse of the supernova envelope. However, even in this case, a clear spatial separation of regions enriched and not enriched in metals is visible. During the collapse of the supernova envelope, the metallicity of the gas is appreciably higher in the central region ([Z] ?? ?1 to 0) than at the periphery ([Z] ?? ?2 to ?4) of the protogalaxy; most of the enriched gas has metallicities [Z] ?? ?3.5 to ?2.5. The masses of enriched fragments of the supernova envelope remain appreciably lower than the Jeans mass, except in regions at the center of the protogalaxy upon which the surrounding enriched gas is efficiently accreted. Consequently, the birth of stars with metallicities close to those characteristic of present-day Galactic stars is very probable in the central region of the protogalaxy.