Alfven波对日冕的随机湍动加热

来自太阳光球层的Ａｌｆｖｅｎ波沿着日冕环的拱形磁感线两足向上传播，在冕环的顶部两反向传播的波相遇，强烈的不稳定性可能激发起等离子体湍动。Ａｌｆｖｅｎ波的能量可能转移给快磁声波并衰减和耗散。在一定条件下可以形成无碰撞波；当粒子的热速度接近于无碰撞波的相速度时，可以通过朗道阻尼引起的无碰撞随机湍动加热，使日冕等离子体湍动区的温度迅速上升，对日冕平均温度的增加有一定的贡献，是日冕快速加热的重要机制。     

束离子与离子声波准线性相互作用的研究

给出了束离子与离子声波准线性相互作用的数值解,由解出的波谱进一步给出湍动加速中的加速系数、脉动加速系数、粒子与湍动场间的等效碰撞频率,通过粒子与湍动场间的等效碰撞频率和粒子间有效碰撞频率的比较,说明在有较强湍动场的情形下采用无碰撞等离子体模型是很合适的。     

低速太阳风中电子的随机湍动加热

在低速太阳风中,在离子声波湍动已经激发的区域,可以产生沿着一定方向运动的逃兔电子束,该电子束可以激发起强烈的纵等离子激元的湍动,朗缪尔波的主要吸收机制是通过等离子体热电子的非线性散射,朗缪尔波受激转换为离子声波,这种转换随着电子的迅速加热,几乎所有有纵等离子激元的能量都转移给散射电子,导致低速太阳风中电子的温度高于质了的温度。     

强朗缪尔湍动与太阳质子电子事件

在空间探测中,太阳质子事件都伴生非相对论性电子,却常有观测到电子流而无质子成分的纯电子事件.纯电子事件中,电子流量比通常电子事件低一个量级左右.荷电粒子会因为与强朗缪尔湍动的相互作用而得到加速,经过理论推导发现电子和质子能否得到加速与朗缪尔湍动强度有关.代入日冕活动区物理量的典型值,计算发现正是由于质子和电子的加速条件对朗缪尔湍动强度的要求不同而产生了上述现象.     

高速太阳风中的α粒子流

利用等离子体湍动理论，研究α粒了在高速太阳风中，被阿尔文波湍动随机加速的机制，定量地解释了α粒子的速度大于质子的速度，α粒子的温度高于质了的温度的原因。     

太阳活动区漂移电场引起的日冕瞬变

在太阳活动区，当离子声波湍动充分发展后库仑碰撞阻尼和朗道无碰撞阻尼全部可以被忽略，在电场力大于阻尼力的瞬间，电子和离子将突然逃逸，在一定条件下，将产生爆发日珥和日冕物质抛射。     

脉冲星相对论风流的湍动波加速机制

考虑由脉冲星磁偶极辐射产生的低应电磁波，它构成的湍动波压将加速等离子体，并通过磁极的磁力线散发到空间，形成脉冲星风。计算表明：当找到一个能与粒子产生共振的初始波能时，电子可被加速到γ≥１２，而构成相对论性风流。     

三维强朗缪尔湍动对电子的加速

从等离子体动力学理论出发，研究了三维强朗缪尔湍动对电子的加速，得出了高能电子的能量谱，理论得出的这种能量谱能够跟实验观测结果很好的吻合。     

喷动床导向管内粗颗粒的动特性

喷动床是处理粗颗粒物料的高效反应器．应用粒子图像测速仪（PIV）研究了喷动床导向管内粗颗粒物料的运动规律，测量了粗颗粒物料的瞬态流场及湍流度分布．粒子运动速度基本是轴对称的，轴心处速度最高；而在近壁处低，当喷动气流速度增加时粒子湍流度也增加，轴心处湍流度高于近壁处的湍流度．管中的流动湍动十分剧烈，湍流度始终很大，这加强了气流和物料间的热量和质量的传递．     

高速太阳风中质子的随机湍动加热

在高速太阳风中，Ａｌｆｖｅｎ波在传播过程中其能量可能转移给快磁声波，当磁场强度和Ａｌｆｖｅｎ波速度趋于零时，快磁声波将转变为离子声波。通过对质子的随机湍动加热，而导致高速太阳风中质子平均温度高于电子的平均温度。     

Electron dynamics in collisionless magnetic reconnection

Magnetic reconnection provides a physical mechanism for fast energy conversion from magnetic energy to plasma kinetic energy. It is closely associated with many explosive phenomena in space plasma, usually collisionless in character. For this reason, researchers have become more interested in collisionless magnetic reconnection. In this paper, the various roles of electron dynamics in collisionless magnetic reconnection are reviewed. First, at the ion inertial length scale, ions and electrons are decoupled. The resulting Hall effect determines the reconnection electric field. Moreover, electron motions determine the current system inside the reconnection plane and the electron density cavity along the separatrices. The current system in this plane produces an out-of-plane magnetic field. Second, at the electron inertial length scale, the anisotropy of electron pressure determines the magnitude of the reconnection electric field in this region. The production of energetic electrons, which is an important characteristic during magnetic reconnection, is accelerated by the reconnection electric field. In addition, the different topologies, temporal evolution and spatial distribution of the magnetic field affect the accelerating process of electrons and determine the final energy of the accelerated electrons. Third, we discuss results from simulations and spacecraft observations on the secondary magnetic islands produced due to secondary instabilities around the X point, and the associated energetic electrons. Furthermore, progress in laboratory plasma studies is also discussed in regard to electron dynamics during magnetic reconnection. Finally, some unresolved problems are presented.     

Clustering of the collisionless particles in a gravitational field and rotation curve

The problem of dark matter in present astrophysics has been disputed for a long time and has not been solved yet. More and more evidence shoves that mostly the dark matter is probably not baryonic, but the collisionless particles which only participate in the gravitational interaction. These collisionless particles can condense in any potential well and provide the "missing mass".     

Recent progresses in theoretical studies and satellite observations for collisionless magnetic reconnection

As an essential mechanism in large scale fast magnetic energy releases and field reconfigurations processes in space,astrophysical, and laboratory plasmas,magnetic reconnection,particularly collisionless magnetic reconnection,has been studied for more than 65 years.Many progresses have been achieved in recent years and basic features of the process have been well understood,largely due to more and more satellite observation data available in the last decade.However,a few outstanding issues are still remained unresolved.We in the paper review the development of collisionless magnetic reconnection studies and major achievements in recent years,and also briefly discuss the open questions remained to be answered in studies of collisionless magnetic reconnection.     

基于不同动态负荷的太阳能辅助地源热泵系统供暖特性研究

建立了太阳能辅助地源热泵系统(SAGSHPS)动态仿真模型,基于间歇负荷1(8:00-20:00末端开启)、间歇负荷2(18:00-次日7:00末端开启)和连续负荷(末端全天24h开启)条件,对大连地区SAGSHPS在整个供暖期内的运行过程分别进行逐时动态仿真,分析了3种典型动态负荷下SAGSHPS的运行特性.结果表明:冬季最冷日内不同负荷下,系统供暖运行方式不同.间歇负荷1下系统以地源热泵(GSHP)和太阳能热泵(SHP)交替供暖;间歇负荷2下系统以地源热泵供暖为主,只在入夜初期辅以太阳能热泵供暖;连续负荷下系统白天以太阳能热泵供暖,夜间以地源热泵供暖.整个供暖期内,蒸发器入口温度对热泵机组性能系数的影响高于对系统性能系数的影响;对于太阳能、地热能和电能对热负荷的贡献比例而言,蒸发器入口温度越高,太阳能对热负荷的贡献比例越大,地热能的贡献比例越小,而电能的贡献比例变化不明显.     

In situ detection of collisionless reconnection in the Earth's magnetotail

Magnetic reconnection is the process by which magnetic field lines of opposite polarity reconfigure to a lower-energy state, with the release of magnetic energy to the surroundings. Reconnection at the Earth's dayside magnetopause and in the magnetotail allows the solar wind into the magnetosphere. It begins in a small 'diffusion region', where a kink in the newly reconnected lines produces jets of plasma away from the region. Although plasma jets from reconnection have previously been reported, the physical processes that underlie jet formation have remained poorly understood because of the scarcity of in situ observations of the minuscule diffusion region. Theoretically, both resistive and collisionless processes can initiate reconnection, but which process dominates in the magnetosphere is still debated. Here we report the serendipitous encounter of the Wind spacecraft with an active reconnection diffusion region, in which are detected key processes predicted by models of collisionless reconnection. The data therefore demonstrate that collisionless reconnection occurs in the magnetotail.     

一维线性Vlasov-Poisson方程组的衰减估计

研究了一类带异种电荷无碰撞的等离子体运动模型(Vlasov-Poisson方程组),在一维情况下得到了线性Vlasov-Poisson方程组的一个重要不等式,同时利用此不等式研究其解的长时间行为,并给出了相应的衰减估计.     

微细菱镁矿热分解过程及动力学

采用TG-DSC热分析技术,在不同升温速率下对高纯微细菱镁矿进行热分解动力学研究.结果表明:随着升温速率的增大,菱镁矿分解速率不断增大且最大分解速率也向高温区偏移.首先使用Hu-Gao-Zhang方程对不同升温速率的TG数据进行计算,确定了热分解机理函数的唯一性和活化能.进而采用双等双步法和产品形貌分析,确定其最概然机理函数为f(α)=2(1-α)^1/2,热分解沿解理面向内进行,属于典型的相边界反应.最后利用Flynn-Wall-Ozawa方程求得指前因子,建立了微细菱镁矿的热分解动力学方程.用两组不同升温速率的TG数据对所建立方程进行验证,方程合理.