Integrable geodesic flows and super polytropic gas equations

The polytropic gas equations are shown to be the geodesic flows with respect to an L² metric on the semidirect product space Diff(S¹)C^∞(S¹), where Diff(S¹) is the group of orientation preserving diffeomorphisms of the circle. We also show that the N=1 supersymmetric polytropic gas equation constitute an integrable geodesic flow on the extended Neveu–Schwarz space. Recently other kinds of supersymmetrizations have been studied vigorously in connection with superstring theory and are called supersymmetric-B (SUSY-B) extension. In this paper we also show that the SUSY-B extension of the polytropic gas equation form a geodesic flow on the extension of the Neveu–Schwarz space.     

The Perturbation Effect of Rotating Solar Polytropic Model on the Variation of Planetary Orbital Elements

In this paper the author examines the perturbation effect of rotating solar polytropic model on the variation of planetary orbital elements by the method of general perturbation in celestial mechanics and the polytropic model ofgaseous star in astrophysics. The perturbation variables of planetary orbital elements caused by the rotation, oblateness and central density of the sun for the polytropic index n = 3 are derived. The result shows clearly that the periodic perturbation effects are the orbital elements of all and the secular perturbation effects are the variation of the longitudes of perihelion, the ascending node and the mean anomaly of epoch. Finally, the author applies the obtained theoretical results to a calculation of the variation of orbital elements of four planets. The numerical results are given in Table 1.     

太阳能强化自然通风理论分析及其在生态建筑中的应用

生态建筑作为建筑节能的一个全新设计理念,旨在最大限度地利用风能、太阳能等自然能源,削减不可再生能源的耗费。将太阳能烟囱、Trombe墙以及太阳能空气集热器等构件与生态建筑一体化设计安装能够取得较好的效果。本文以太阳能烟囱为例对太阳能强化自然通风的原理进行了理论分析与模拟计算。同时,介绍了较为典型的三种太阳能强化自然通风的复合能量系统。     

The solar wind interaction with the Earth's magnetosphere: atutorial

The size of the terrestrial magnetosphere is determined by the balance between the solar wind dynamic pressure and the pressure exerted by the magnetosphere, principally that of its magnetic field. The shape of the magnetosphere is additionally influenced by the drag of the solar wind, or tangential stress, on the magnetosphere. This drag is predominantly caused by the mechanism known as reconnection in which the magnetic field of the solar wind links with the magnetic field of the magnetosphere. The factors that control the rate of reconnection of the two fields are not understood completely, but a southward direction of the interplanetary field is critical to enabling reconnection with the dayside low-latitude magnetosphere, resulting in magnetic flux transfer to the magnetotail. Numerical simulations suggest that the conductivity of the ionosphere controls the rate of reconnection, but this has not been verified observationally. Although solar wind properties ultimately control the interaction, the properties of the plasma that make direct contact with the magnetosphere are different than those of the solar wind, having been altered by a standing bow shock wave. This standing shock is necessitated by the fact that the flow velocity of the solar wind far exceeds the velocity of the compressional wave that diverts the solar wind around the Earth. The upper atmosphere is the final recipient of all the energy and momentum that enters the magnetosphere. Coupling takes place along the magnetic field Lines principally in the polar and auroral region via current systems that close across the magnetic field both at low and high altitudes and flow parallel to the magnetic field between high and low altitudes     

Cosmological Implications of Interacting Polytropic Gas Dark Energy Model in Non-flat Universe

The polytropic gas model is investigated as an interacting dark energy scenario. The cosmological implications of the model including the evolution of EoS parameter w _Λ, energy density Ω_Λ and deceleration parameter q are investigated. We show that, depending on the parameter of model, the interacting polytropic gas can behave as a quintessence or phantom dark energy. In this model, the phantom divide is crossed from below to up. The evolution of q in the context of polytropic gas dark energy model represents the decelerated phase at the early time and accelerated phase later. The singularity of this model is also discussed. Eventually, we establish the correspondence between interacting polytropic gas model with tachyon, K-essence and dilaton scalar fields. The potential and the dynamics of these scalar field models are reconstructed according to the evolution of interacting polytropic gas.     

太阳能制氢腔式吸热器混合对流的数值模拟研究

混合对流热损失是影响太阳能与生物质超临界水气化耦合制氢腔式吸热器热效率的关键因素之一。本文以动力工程多相流实验室建成的生物质超临界水与太阳能聚集供热耦合制氢腔式吸热器为研究对象,对腔式吸热器混合对流换热进行了数值模拟研究。通过使用RNGkε湍流模型,研究了制氢吸热器在外界风吹掠环境下的混合对流热损失,获得了腔式吸热器在不同风速、风向吹掠下的混合对流换热准则Nusselt数。模拟结果表明,侧向风与侧迎向风对腔内对流热损失影响最大,当风速超过某一数值(Richardson数>1),外界风诱发的强制对流会在对流热损失中占主导作用,且随着风速增加,混合对流热损失随Re提高而增大。     

Minimal geometric deformation in asymptotically (A-)dS space-times and the isotropic sector for a polytropic black hole

In the context of the minimal geometric deformation method, in this paper we implement the inverse problem in a black hole scenario. In order to deal with an anisotropic polytropic black hole solution of the Einstein field equations with cosmological constant, the deformation method is slightly extended. After obtaining the isotropic sector and the decoupler for an anisotropic (A-)dS polytropic black hole solution, we emphasize a possible relation between anisotropization/isotropization and the violation of the energy conditions.     

Compressibility in solar wind plasma turbulence

Incompressible magnetohydrodynamics is often assumed to describe solar wind turbulence. We use extended self-similarity to reveal scaling in the structure functions of density fluctuations in the solar wind. The obtained scaling is then compared with that found in the inertial range of quantities identified as passive scalars in other turbulent systems. We find that these are not coincident. This implies that either solar wind turbulence is compressible or that straightforward comparison of structure functions does not adequately capture its inertial range properties.     

Chaos in the solar wind flow near Earth

We have done a time series analysis of daily average data of solar wind velocity, density and temperature at 1 AU measured by ACE spacecraft for a period of nine years. We have used the raw data without filtering to give a faithful representation of the nonlinear behaviour of the solar wind flow which is a novel one. The sensitivity of the results on filtering is highlighted. The attractor dimension is estimated for every parameter of the solar wind and it is found that they differ substantially. Hence a chaotic picture for the problem from different angles have been obtained. The calculated Kolmogorov entropies and Lyapunov exponents are positive showing evidences that the complex solar wind near the Earth is most likely a deterministic chaotic system.      

An observational picture of solar-wind MHD turbulence

Summary A review of the available information on the MHD fluctuations in the solar wind is given. The most general properties of the picture which derives from the satellite measurements are discussed. The very important result which seems to appear is the fact that the low-frequency MHD fluctuations are characteristic of a turbulent state. Clearly this state cannot be represented by the usual models based on the hypothesis of the presence of simple waves in the solar wind. It is then rather natural to suppose that these observational data should be usefully analysed only through the theoretical methods developed to study the strong MHD turbulence. Moreover, this analysis is rather stimulating since the solar wind offers us one of the rare possibilities to have observational tests of the theoretical models of strong MHD turbulence.     

Anisotropic third-moment estimates of the energy cascade in solar wind turbulence using multispacecraft data

The first direct determination of the inertial range energy cascade rate, using an anisotropic form of Yaglom's law for magnetohydrodynamic turbulence, is obtained in the solar wind with multispacecraft measurements. The two-point mixed third-order structure functions of Els?sser fluctuations are integrated over a sphere in magnetic field-aligned coordinates, and the result is consistent with a linear scaling. Therefore, volume integrated heating and cascade rates are obtained that, unlike previous studies, make only limited assumptions about the underlying spectral geometry of solar wind turbulence. These results confirm the turbulent nature of magnetic and velocity field fluctuations in the low frequency limit, and could supply the energy necessary to account for the nonadiabatic heating of the solar wind.     

30m~2槽式太阳能集热器性能模拟研究

本文针对30 m~2槽式太阳能集热试验装置,对太阳能集热器的性能进行了模拟。分析了太阳能集热器光热转化过程,建立了太阳能能量转换与传递模型,并开发了模拟计算程序,研究了集热器关键结构参数和运行参数对集热性能的影响规律。具体考察了太阳辐照强度、工质流量、环境风速、吸热管管径等对集热效率的影响。结果表明:太阳能集热器的集热效率随太阳辐照强度的增加而增大,随工质流量的增加而增大,存在最佳的吸热管管径使得集热效率最大。研究结果将为太阳能集热器的设计提供参考依据。     

微型风力发电演示仪

设计制作了一种基于风光互补原理的微型风力发电演示仪.该仪器由风力发电机、光伏太阳能电池板、控制器、蓄电池、负载等各部分组成.整个系统以控制器为核心,由风力发电机、光伏太阳能电池板把风能和光能转变为电能并储存于蓄电池中供负载使用.该仪器作为演示实验仪不仅小型、直观、模块化和操作简便,而且演示内容突显物理与工程相结合的知识...     

On Yaglom’s Law for the Interplanetary Proton Density and Temperature Fluctuations in Solar Wind Turbulence

In the past decades, there has been an increasing literature on the presence of an inertial energy cascade in interplanetary space plasma, being interpreted as the signature of Magnetohydrodynamic turbulence (MHD) for both fields and passive scalars. Here, we investigate the passive scalar nature of the solar wind proton density and temperature by looking for scaling features in the mixed-scalar third-order structure functions using measurements on-board the Ulysses spacecraft during two different periods, i.e., an equatorial slow solar wind and a high-latitude fast solar wind, respectively. We find a linear scaling of the mixed third-order structure function as predicted by Yaglom’s law for passive scalars in the case of slow solar wind, while the results for fast solar wind suggest that the mixed fourth-order structure function displays a linear scaling. A simple empirical explanation of the observed difference is proposed and discussed.     

Polytropes in plasmas described by kappa distributions – Application in atmospheric modelling

The paper derives the complete formulations of polytropic behaviour for plasmas described by kappa distributions. This is achieved by employing both positive and negative types of phase-space kappa distributions of a Hamiltonian for a nonzero potential energy, while the cases of positive and negative potential energies are analysed separately. Then, we develop the general polytropic-barometric formula that describes the profiles of density, temperature, and thermal pressure. Furthermore, it is shown how the kappa and polytropic indices can be derived from observational measurements of the temperature altitude gradient. As an example, we calculated the kappa κ ≈ 3.35 and polytropic γ ≈ 0.74 indices of the terrestrial atmosphere at ∼100 km, revealing the existence of heating processes that add thermal energy to atmospheric particles.     

Self-similar signature of the active solar corona within the inertial range of solar-wind turbulence

We quantify the scaling of magnetic energy density in the inertial range of solar-wind turbulence seen in situ at 1 AU with respect to solar activity. At solar maximum, when the coronal magnetic field is dynamic and topologically complex, we find self-similar scaling in the solar wind, whereas at solar minimum, when the coronal fields are more ordered, we find multifractality. This quantifies the solar-wind signature that is of direct coronal origin and distinguishes it from that of local MHD turbulence, with quantitative implications for coronal heating of the solar wind.     

On nonlinear cascades and resonances in the outer magnetosphere

The paper addresses nonlinear phenomena that control the interaction between plasma flow (solar wind) and magnetic barrier (magnetosphere). For the first time we demonstrate that the dominant solar wind kinetic energy: (i) excites boundary resonances and their harmonics which modulate plasma jets under the bow shock; (ii) produces discrete three-wave cascades, which could merge into a turbulent-like one; (iii) jet produced cascades provide the effective anomalous plasma transport inside and out of the magnetosphere; (iv) intermittency and multifractality characteristics for the statistic properties of jets result in a super-ballistic turbulent transport regime. Our results could be considered as suggestive for the space weather predictions, for turbulent cascades in different media and for the laboratory plasma confinement (e.g., for fusion devices).     

Swimming of micro-organism over an oscillatory stretched surface filled with a magnetic third-grade nanofluid: An application of activation energy

During the past few years, abundant involvement of nanoparticles in improving the thermal extrusion systems and energy resources attracted the attention of numerous scientists recently. The significance of nanofluid in terms of working liquid directed for the enhancement of solar energy and thermal extrusion performances. Therefore, the present analysis deals with the thermal performances of bioconvection flow with nanoparticles suspended in a non-Newtonian fluid. Considering that the flow has been induced due to periodically accelerated surface. The activation energy consequences are also employed in the concentration equation. The flow problem is initially formulated in the form of partial differential equations. The dimensionless variables are reported to renovate such equations in the dimensionless style, which are tackled analytically by employing the homotopy analysis method. The significance of various physical parameters is estimated for the relevant distribution of velocity, temperature, concentration, and motile micro-organisms. The dimensionless local Nusselt number, local Sherwood number, and motile density number are numerically iterated via flow parameters. A convergence analysis is also presented. The detected observation can involve theoretical significance in various engineering processes, bio-fuel cells, solar energy systems, and enhancement of extrusion systems.     

Gravitational perturbations of spherically symmetric systems. II. Perfect fluid interiors

Methods developed in a previous paper on perturbations of the Schwarzschild metric are here extended to the treatment of perturbations of perfect fluid stellar models. The perturbations of a perfect fluid sphere are explicitly decomposed into their gauge invariant and gauge dependent parts and a variational principle for the perturbation equations is derived. The Hamiltonian for the perturbations is constructed and a sufficient condition for stability against nonradial, radiative perturbations is derived from it. The stability criterion is applied to two interesting classes of stellar models, polytropic white dwarf models and high-density neutron star cores with pressure proportional to energy density.     

嫦娥一号卫星太阳风离子探测器数据分析

探月航天器与月球周围等离子体环境相互作用,表面将出现充放电效应,给航天器带来很多不利影响.表面充电电位对充放电的影响至关重要.评估探月航天器的充放电效应,首先需获得月球周围等离子体环境数据.嫦娥一号上搭载的两台太阳风离子探测器SWIDA/B是用来观测月球200 km轨道附近等离子体环境的探测仪器,获得了月球附近的太阳风速度、密度和温度.本文对2008年6月一个月内太阳风离子探测器SWIDA机获得的离子微分通量进行统计平均,得到太阳风离子微分通量能谱,并计算得到了月球200 km附近的太阳风速度(300.00—600.00 km·s-1)、密度(1—10 cm-3)和温度(1—20 eV).最后采用等效电路模型的方法计算得到了探月航天器表面充电电位范围为-7—-70 V.