A two-layer αω-dynamo model with dynamic feedback on the ω-effect

In an attempt to produce a simple representation of an interface dynamo, I examine a dynamo model composed of two one-dimensional (radially averaged) pseudo-spherical layers, one in the convection zone and possessing an α-effect, and the other in the tachocline and possessing an ω-effect. The two layers communicate by means of an analogue of Newton's law of cooling, and a dynamical back-reaction of the magnetic field on ω is provided. Extensive bifurcation diagrams are calculated for three separate values of η, the ratio of magnetic diffusivities of the two layers. I find recognizable similarities to, but also dramatic differences from, the comparable one-layer model examined by Roald &38; Thomas. In particular, the solar-like dynamo mode found previously is no longer stable in the two-layer version; in its place there is a sequence of periodic, quasi-periodic and chaotic modes probably created in a homoclinic bifurcation. These differences are important enough to provide support for the view that the solar dynamo cannot be meaningfully modelled in one dimension.     

Disc structure around strongly magnetic accretors: a full disc solution with buoyancy diffusivity

A full numerical solution is found for the effect of a strongly magnetic star on its accretion disc, for the case of magnetic buoyancy diffusion. As in the previously considered case of turbulent diffusion, the disc becomes disrupted when magnetic and viscous stresses become comparable. A magnetically induced temperature elevation leads to electron scattering opacity and radiation pressure becoming significant far from the stellar surface, with consequent viscous instability and vertical disruption of the disc. This, together with the previous turbulent case, suggests that such a disruption mechanism owing to strongly magnetic accretors is generally operable.     

PSR J1012+5307: younger than it looks?

Lorimer et al. have recently reported that the spin-down age (∼7 × 10⁹ yr) of the low-mass binary pulsar PSR J1012+5307 is much higher than the cooling age (3 × 10⁸ yr) of its white dwarf companion. The proposed solutions for this discrepancy are outlined and discussed. In particular, the revised cooling age estimate proposed by Alberts et al. agrees with data from other low-mass binary pulsar systems if a transition to the 'classical' cooling regime occurs between ∼0.14 and ∼0.28 M_⊙. If this transition is excluded, PSR J1012+5307 seems to have finished its accretion phase far from the spin-up line.     

The anisotropy of loess magnetic susceptibility in the northeastern fringe of Qinghai-Xizang Plateau as an indicator of palaeowind direction

Estimates of the palaeo-subaerial wind direction were studied systematically for the first time by using the anisotropy of loess magnetic susceptibility (AMS) measurements in the northwestern China. One hundred and forty undisturbed oriented aeolian loess samples were collected from Lanzhou, Linxia and Wudu areas for AMS measurements, which indicated the subaerial wind directions were not the same while the loess deposited. From the Early Pleistocene to Middle Pleistocene till Late Pleistocene, the wind direction experienced an anticlockwise rotation in the studied area. We suggested this change was related to the uplift of the Qinghai-Xizang Plateau and the adjustment of current and landform effects.     

山东省区域地球物理场

山东省各岩石磁性及密度参数基本可分为高、中、低 3类。山东省磁性结晶基底为泰山岩群、荆山群、胶东岩群、胶南岩群。以沂沭断裂带为界 ,山东省区域地球物理场分为鲁东区和鲁西区。鲁东区进一步划分为 3个次级区 ,即北部区、中部区和南部区。鲁西区进一步划分为 5个次级区 ,即鲁北重磁缓变区、鲁西南重高磁高区、中部弧形重磁场区、鲁西中部重低磁高区、鲁中南条带状重磁场区。各区地球物理场由于地质原因各具特点。山东省莫氏面总体呈东浅西深的缓变带 ,在该缓变带的背景上 ,呈周边地区条带状幔隆、中部幔坳的特征。山东省居里面呈近南北向带状分布 ,有德州聊城菏泽隆起带、滨州淄博滕州深坳带、蓬莱海阳千里岩响水隆起带。鲁中隆起北部碰撞带为山东省特殊的构造地带 ,其特征为侵入岩体沿该带断续出现、岩体围岩或岩体内铜及多金属矿化较为普遍、地热田沿该带时有分布、地形上为南部山区和北部平原的分界地带。胶莱盆地内 ,蓼兰—高密缺失莱阳群层位 ;中生代早期 ,盆地东北部与西南部是盆地的沉积中心 ,至晚期盆地中心北移 ,第三纪沉积中心则为平度蓼兰附近 ;盆地较深部位位于诸城凹陷、平度凹陷。胶莱盆地的次级构造单元可划分为 11个 ,七级镇构造带控制了胶莱盆地的成生和发展。山东省岩浆岩通常表