Dynamos in asymptotic-giant-branch stars as the origin of magnetic fields shaping planetary nebulae

Planetary nebulae are thought to be formed when a slow wind from the progenitor giant star is overtaken by a subsequent fast wind generated as the star enters its white dwarf stage. A shock forms near the boundary between the winds, creating the relatively dense shell characteristic of a planetary nebula. A spherically symmetric wind will produce a spherically symmetric shell, yet over half of known planetary nebulae are not spherical; rather, they are elliptical or bipolar in shape. A magnetic field could launch and collimate a bipolar outflow, but the origin of such a field has hitherto been unclear, and some previous work has even suggested that a field could not be generated. Here we show that an asymptotic-giant-branch (AGB) star can indeed generate a strong magnetic field, having as its origin a dynamo at the interface between the rapidly rotating core and the more slowly rotating envelope of the star. The fields are strong enough to shape the bipolar outflows that produce the observed bipolar planetary nebulae. Magnetic braking of the stellar core during this process may also explain the puzzlingly slow rotation of most white dwarf stars.     

热白矮星的质量-半径关系

研究了有限温度条件下分别由Fe核和C核构成的热白矮星.结果表明随着温度升高,对应同一质量的白矮星的半径增加.温度对白矮星质量-半径关系的影响强度随着星体质量的增加而减弱.相比于Fe-白矮星,C-白矮星的质量-半径关系对温度的依赖程度较大.存在一个临界质量,当白矮星的质量小于这个临界值时,温度的影响将不能忽略.C-白矮星...     

小电流环远场分布的一种求法

给出一种简便年出小电流环在空间远点磁场分布的方法.     

Galactic cosmic ray origin of Li, Be and B in stars

A study of the implications of the hypothesis that high energy processes involving cosmic rays acting on the interstellar medium are the sources of the elements Li, Be and B present in stellar atmospheres and in the solar system.     

一种多绕组磁场发生器的设计

文章依据亥姆霍兹线圈原理提出了一种多绕组结构的磁场发生器设计方案,利用Maxwell软件对其进行模拟仿真分析,并制作了一套多绕组磁场发生器。通过对比实际测量数值与模拟仿真数值,证明了该设备能产生0～2T的磁场,在中心区域磁感应强度的不均匀性小于3%,得到了预期效果。     

A deep dynamo generating Mercury's magnetic field

Mercury has a global magnetic field of internal origin and it is thought that a dynamo operating in the fluid part of Mercury's large iron core is the most probable cause. However, the low intensity of Mercury's magnetic field--about 1% the strength of the Earth's field--cannot be reconciled with an Earth-like dynamo. With the common assumption that Coriolis and Lorentz forces balance in planetary dynamos, a field thirty times stronger is expected. Here I present a numerical model of a dynamo driven by thermo-compositional convection associated with inner core solidification. The thermal gradient at the core-mantle boundary is subadiabatic, and hence the outer region of the liquid core is stably stratified with the dynamo operating only at depth, where a strong field is generated. Because of the planet's slow rotation the resulting magnetic field is dominated by small-scale components that fluctuate rapidly with time. The dynamo field diffuses through the stable conducting region, where rapidly varying parts are strongly attenuated by the skin effect, while the slowly varying dipole and quadrupole components pass to some degree. The model explains the observed structure and strength of Mercury's surface magnetic field and makes predictions that are testable with space missions both presently flying and planned.     

Dating the origin of the Orchidaceae from a fossil orchid with its pollinator

Since the time of Darwin, evolutionary biologists have been fascinated by the spectacular adaptations to insect pollination exhibited by orchids. However, despite being the most diverse plant family on Earth, the Orchidaceae lack a definitive fossil record and thus many aspects of their evolutionary history remain obscure. Here we report an exquisitely preserved orchid pollinarium (of Meliorchis caribea gen. et sp. nov.) attached to the mesoscutellum of an extinct stingless bee, Proplebeia dominicana, recovered from Miocene amber in the Dominican Republic, that is 15-20 million years (Myr) old. This discovery constitutes both the first unambiguous fossil of Orchidaceae and an unprecedented direct fossil observation of a plant-pollinator interaction. By applying cladistic methods to a morphological character matrix, we resolve the phylogenetic position of M. caribea within the extant subtribe Goodyerinae (subfamily Orchidoideae). We use the ages of other fossil monocots and M. caribea to calibrate a molecular phylogenetic tree of the Orchidaceae. Our results indicate that the most recent common ancestor of extant orchids lived in the Late Cretaceous (76-84 Myr ago), and also suggest that the dramatic radiation of orchids began shortly after the mass extinctions at the K/T boundary. These results further support the hypothesis of an ancient origin for Orchidaceae.     

A current filamentation mechanism for breaking magnetic field lines during reconnection

During magnetic reconnection, the field lines must break and reconnect to release the energy that drives solar and stellar flares and other explosive events in space and in the laboratory. Exactly how this happens has been unclear, because dissipation is needed to break magnetic field lines and classical collisions are typically weak. Ion-electron drag arising from turbulence, dubbed 'anomalous resistivity', and thermal momentum transport are two mechanisms that have been widely invoked. Measurements of enhanced turbulence near reconnection sites in space and in the laboratory support the anomalous resistivity idea but there has been no demonstration from measurements that this turbulence produces the necessary enhanced drag. Here we report computer simulations that show that neither of the two previously favoured mechanisms controls how magnetic field lines reconnect in the plasmas of greatest interest, those in which the magnetic field dominates the energy budget. Rather, we find that when the current layers that form during magnetic reconnection become too intense, they disintegrate and spread into a complex web of filaments that causes the rate of reconnection to increase abruptly. This filamentary web can be explored in the laboratory or in space with satellites that can measure the resulting electromagnetic turbulence.     

对"磁感应强度和磁场强度"的讨论

从电流观点和磁荷观点两个角度讨论了磁感应强度B 和磁场强度H 两个物理量,旨在加深对两个物理量含义的理解.     

磁性靶丸悬浮磁场的研究

在提高ICF能量增益的研究中,针对靶丸磁悬浮系统的结构,从磁偶板子的磁场分布开始,推导出悬浮磁场中的磁场分布情况,为磁悬浮系统的非线性精确控制提供了磁场分布的修正,提高系统控制的稳定性。     

The origin of the vertebrate jaw:Intersection between developmental biology-based model and fossil evidence

The origin of the vertebrate jaw has been reviewed based on the molecular,developmental and paleontological evidences.Advances in developmental genetics have accumulated to propose the heterotopy theory of jaw evolution,i.e.the jaw evolved as a novelty through a heterotopic shift of mesenchyme-epithelial interaction.According to this theory,the disassociation of the nasohypophyseal complex is a fundamental prerequisite for the origin of the jaw,since the median position of the nasohypophyseal placode in cyclostome head development precludes the forward growth of the neural-crest-derived craniofacial ectomesenchyme.The potential impacts of this disassociation on the origin of the diplorhiny are also discussed from the molecular perspectives.Thus far,our study on the cranial anatomy of galeaspids,a 435-370-million-year-old ’ostracoderm’ group from China and northern Vietnam,has provided the earliest fossil evidence for the disassociation of nasohypophyseal complex in vertebrate phylogeny.Using Synchrotron Radiation X-ray Tomography,we further show some derivative structures of the trabeculae(e.g.orbitonasal lamina,ethmoid plate) in jawless galeaspids,which provide new insights into the reorganization of the vertebrate head before the evolutionary origin of the jaw.These anatomical observations based on new techniques highlight the possibility that galeaspids are,in many respects,a better proxy than osteostracans for reconstructing the pre-gnathostome condition of the rostral part of the braincase.The cranial anatomy of galeaspids reveals a number of derived characters uniquely shared with gnathostomes.This raises the potential possibility that galeaspids might be the closest jawless relatives of jawed vertebrates.Our study provides an intriguing example of intersection between developmental biology-based model and fossil evidence.     

磁荷的多极辐射场强和能流密度

在Dirac磁单极存在的情况下,考虑保持Maxwell方程双矢势下的电磁对偶性。利用有磁荷存在的d′Alembert方程推迟解,求出了带磁荷粒子的电磁辐射的表达式。最后得到磁多极辐射表达式。     

面场强计算中的一个问题

面场强的计算是电磁学中一类常见问题。然而目前的文献在研究此类问题时都忽略了一个问题,即没有解释位于场点所在处的面元的场强为什么是0。本文指出了这一问题并给出了解决方案,所得结论对面场强计算的教学具有较大的参考价值。     

外磁场和电流共同驱动的磁纳米柱中磁矩动力学

针对自由层与自旋极化层均为垂直磁各向异性材料的磁纳米柱结构,基于Landau-Lifshitz-Gilbert-Slonczewski(LLGS)方程,利用微磁学模拟方法,研究了外磁场和电流导致的自旋转矩效应所驱动的自由层磁矩翻转特性.模拟结果显示磁矩翻转曲线中出现了多个凸起的非正常翻转状态;且凸起区域出现的位置与外加磁场大小、纳米柱尺寸和垂直磁各向异性相关,而与极化层磁矩的倾角大小无关.在自旋极化层的磁矩倾角给定时,凸起区域出现的磁矩状态有亚稳态、振荡态、稳定态3种.给出建立了它们随磁场和极化层倾角变化的参数相图.     

永磁非金属液体电磁泵磁场数值分析

将电磁泵体求解场域按二维平面场处理,考虑了外磁场对永磁体的磁化效应,用有限元法对永磁非金属液体电磁泵的磁场进行了数值分析,得到了该电磁泵气隙中的磁密曲线以及载流海水在气隙中流动所受到的电磁力.实验证明该数值分析的结果是准确的,这些数据为永磁非金属液体电磁泵的设计和应用提供了可靠依据,同时也说明了可用永磁体代替价格昂贵的超导磁体应用于非金属液体电磁泵的磁极设计.图7,参7.     

外磁场驱动的无线内窥镜磁场线圈的设计方法研究

为实现外磁场驱动的无线内窥镜所需的外部磁场,提出了外部磁场线圈的设计方法．针对人体呈圆柱状外形对目标磁场在柱坐标系中进行分解,通过目标场法（target field,TF）反解出电流密度分布,并通过离散得到实际线圈的位置和电流大小．用此方法设计了一个方案,并用有限元软件进行建模仿真,计算磁体转矩的大小,与预计的理想转矩进行了对比;同时分析了均匀磁场的范围．仿真结果表明,这样的线圈和电流分布方式可以使无线内窥镜所带的永磁体在任意平面产生均匀转矩．     

A regular period for Saturn's magnetic field that may track its internal rotation

The rotation rate of a planet is one of its fundamental properties. Saturn's rotation, however, is difficult to determine because there is no solid surface from which to time it, and the alternative 'clock'--the magnetic field--is nearly symmetrically aligned with the rotation axis. Radio emissions, thought to provide a proxy measure of the rotation of the magnetic field, have yielded estimates of the rotation period between 10 h 39 min 22 s and 10 h 45 min 45 s (refs 8-10). Because the period determined from radio measurements exhibits large time variations, even on timescales of months, it has been uncertain whether the radio-emission periodicity coincides with the inner rotation rate of the planet. Here we report magnetic field measurements that revealed a time-stationary magnetic signal with a period of 10 h 47 min 6 s +/- 40 s. The signal appears to be stable in period, amplitude and phase over 14 months of observations, pointing to a close connection with the conductive region inside the planet, although its interpretation as the 'true' inner rotation period is still uncertain.     

强磁场中氢原子波函数的研究

通过采用绝热近似和绝热交分近似方法,用柱坐标,画出z和ρ两个方向的波函数,结果表明：变化较小．计算出强磁场（10≤β≤1000）中氢原子的部分能级,采z方向波函数随磁场变化较剧烈,ρ方向波函数随磁场     

电缆三维磁场分析与自感计算

文章采用三维有限元方法分析计算了几类同轴电缆、多股导线同轴电缆以及偏心电缆的三维磁场和电感参数;采用有限元商用软件包ANSYS,基于磁场能量法计算得到几种不同形状的同轴电缆、多股导线同轴电缆以及偏心电缆在不同参数下的单位长度自感参数;基于能量摄动法计算得到同轴电缆在不同参数下的单位长度自感参数和单位长度互感参数,并进一步分析得出电感参数变化规律.有限元法与解析方法计算结果的一致性验证了有限元法计算的正确性.该方法简单易行,且计算精度很高,可用于计算规则或不规则形状的同轴电缆以及偏心电缆等各类电缆的电感参数.