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

Wang Jianli 《中国地理科学(英文版)》1997,8(1):85-90

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.  相似文献   

The angular momentum content of dwarf galaxies: new challenges for the theory of galaxy formation     

Frank C. van den Bosch  reas Burkert  Rob A. Swaters 《Monthly notices of the Royal Astronomical Society》2001,326(3):1205-1215

We compute the specific angular momentum distributions for a sample of low-mass disc galaxies observed by Swaters. We compare these distributions to those of dark matter haloes obtained by Bullock et al. from high-resolution N -body simulations of structure formation in a ΛCDM universe. We find that although the disc mass fractions are significantly smaller than the universal baryon fraction, the total specific angular momenta of the discs are in good agreement with those of dark matter haloes. This suggests that discs form out of only a small fraction of the available baryons, but yet manage to draw most of the available angular momentum. In addition we find that the angular momentum distributions of discs are clearly distinct from those of the dark matter; discs lack predominantly both low and high specific angular momenta. Understanding these findings in terms of a coherent picture for disc formation is challenging. Cooling, feedback and stripping, which are the main mechanisms to explain the small disc mass fractions found, seem unable to simultaneously explain the angular momentum distributions of the discs. In fact, it seems that the baryons that make up the discs must have been born out of angular momentum distributions that are clearly distinct from those of ΛCDM haloes. However, the dark and baryonic mass components experience the same tidal forces, and it is therefore expected that they should have similar angular momentum distributions. Therefore, understanding the angular momentum content of disc galaxies remains an important challenge for our picture of galaxy formation.  相似文献   

Asteroseismic theory of rapidly oscillating Ap stars     

Margarida S. Cunha 《Journal of Astrophysics and Astronomy》2005,26(2-3):213-221

This paper reviews some of the important advances made over the last decade concerning theory of roAp stars.  相似文献   

CCD photometry of variable stars in the Magellanic Clouds – VII. The eclipsing binaries MACHO*05:36:48.7−69:17:00 in the LMC, and MOA J005018.4−723855 and J005623.5−722123 in the SMC     

G. P. Bayne  W. Tobin  J. D. Pritchard  K. R. Pollard  M. D. Albrow 《Monthly notices of the Royal Astronomical Society》2004,349(3):833-840

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Observations of the Blandford–Znajek process and the magnetohydrodynamic Penrose process in computer simulations of black hole magnetospheres     

S. S. Komissarov 《Monthly notices of the Royal Astronomical Society》2005,359(3):801-808

In this paper we report the results of axisymmetric relativistic magnetohydrodynamic (MHD) simulations for the problem of a Kerr black hole immersed in a rarefied plasma with 'uniform' magnetic field. The long-term solution shows properties that are significantly different from those of the initial transient phase studied recently by Koide. The topology of magnetic field lines within the ergosphere is similar to that of the split-monopole model with a strong current sheet in the equatorial plane. Closer inspection reveals a system of isolated magnetic islands inside the sheet and ongoing magnetic reconnection. No regions of negative hydrodynamic 'energy at infinity' are seen inside the ergosphere and the so-called MHD Penrose process does not operate. However, the rotational energy of the black hole continues to be extracted via the purely electromagnetic Blandford–Znajek mechanism. In spite of this, no strong relativistic outflows from the black hole are seen to be developing. Combined with results of other recent simulations, our results signal a potential problem for the standard MHD model of relativistic astrophysical jets should they be found at distances as small as a few tens of gravitational radii from the central black hole.  相似文献   

Smoothed Particle Magnetohydrodynamics – III. Multidimensional tests and the  ∇·B= 0  constraint     

D. J. Price  J. J. Monaghan 《Monthly notices of the Royal Astronomical Society》2005,364(2):384-406

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A new numerical scheme for structures of rotating magnetic stars     

Y. Tomimura  Y. Eriguchi 《Monthly notices of the Royal Astronomical Society》2005,359(3):1117-1130

We have developed a new numerical scheme for obtaining structures of rapidly rotating stars with strong magnetic fields. In our scheme, both poloidal and toroidal magnetic fields can be treated for stars with compressibility and infinite conductivity. By introducing the vector potential and its integral representation, we can treat the boundary condition for the magnetic fields across the surface properly. We show structures and distributions of magnetic fields as well as the distributions of the currents of rotating magnetic polytropic stars with polytropic index   N = 1.5  . The shapes of magnetic stars are oblate as long as the magnetic vector potential decreases as 1/ r when   r →∞  . For extremely strong magnetic fields, equilibrium configurations can be of toroidal shapes.  相似文献   

日冕磁场和重联的射电信号     

黄光力 《天文研究与技术》2006,3(2):99-112

总结了近期用射电频谱仪（高时间和高频谱分辨）和野边山射电日像仪（高空间分辨）以及国内外其它空间和地面设备分析日冕磁场和重联的系列工作。主要结论可归纳为：1）在Dulk等人（1982）的近似下自恰计算射电爆发源区磁场的平行和垂直分量，并首次得到该磁场在日面的两雏分布。2）为了考虑非热电子低能截止的影响，必须采用更严格的回旋同步辐射理论来计算。结果表明：低能截止和日冕磁场对计算有明显的影响，而其它参数（包括背景温度、密度、高能截止和辐射方向）的影响均可忽略。因此，对低能截止和日冕磁场必须联立求解。3）射电爆发中的精细结构可能反映了射电爆发源比较靠近粒子加速（磁场重联）的区域，利用高时间和高频率分辨的频谱仪和高空间分辨的日像仪联合分析，可以确定精细结构的源区位置，从而确定粒子加速（磁场重联）的准确时间和地点。  相似文献   

电力系统潮流量的微机快速跟踪测量     

王筱珍 《广东海洋大学学报》1995,(2)

提出了一种电力系统潮流量的快速跟踪测量方法，其响应时间只有一个采样时间间隔。实验表明，其准确度可满足实用要求。  相似文献   

On the origin of warps and the role of the intergalactic medium     

F. J. Sánchez-Salcedo 《Monthly notices of the Royal Astronomical Society》2006,365(2):555-571

There is still no consensus as to what causes galactic discs to become warped. Successful models should account for the frequent occurrence of warps in quite isolated galaxies, their amplitude as well as the observed azimuthal and vertical distributions of the H  i layer. Intergalactic accretion flows and intergalactic magnetic fields may bend the outer parts of spiral galaxies. In this paper we consider the viability of these non-gravitational torques to take the gas off the plane. We show that magnetically generated warps are clearly flawed because they would wrap up into a spiral in less than two or three galactic rotations. The inclusion of any magnetic diffusivity to dilute the wrapping effect causes the amplitude of the warp to damp. We also consider the observational consequences of the accretion of an intergalactic plane-parallel flow at infinity. We have computed the amplitude and warp asymmetry in the accretion model, for a disc embedded in a flattened dark matter halo, including self-consistently the contribution of the modes with azimuthal wavenumbers   m = 0  and   m = 1  . Since the m = 0 component, giving a U-shaped profile, is not negligible compared to the m = 1 component, this model predicts quite asymmetric warps, maximum gas displacements on the two sides in the ratio 3 : 2 for the preferred Galactic parameters, and the presence of a fraction ∼3.5 per cent of U-shaped warps, at least. The azimuthal dependence of the moment transfer by the ram pressure would produce a strong asymmetry in the thickness of the H  i layer and asymmetric density distributions in z , in conflict with observational data for the warp in our Galaxy and in external galaxies. The amount of accretion that is required to explain the Galactic warp would give gas scaleheights in the far outer disc that are too small. We conclude that accretion of a flow with no net angular momentum cannot be the main and only cause of warps.  相似文献