Shock surfing acceleration   总被引：1，自引：0，他引：1  

Vitali D Shapiro  Defne Üçer 《Planetary and Space Science》2003,51(11):665-680

Analytical and numerical analysis identify shock surfing acceleration as an ideal pre-energization mechanism for the slow pick-up ions at quasiperpendicular shocks. After gaining sufficient energy by shock surfing, pick-up ions undergo diffusive acceleration to reach their observed energies. Energetic ions upstream of the cometary bow shock, acceleration of solar energetic particles by magnetosonic waves in corona, ion enhancement in interplanetary shocks, generation of anomalous cosmic rays from interstellar pick-up ions at the termination shock are some of the cases where shock surfing acceleration apply. Inclusion of the lower-hybrid wave turbulence into the laminar model of shock surfing can explain the preferential acceleration of heavier particles as observed by Voyager at the termination shock. At relativistic energies, unlimited acceleration of ions is theoretically possible; because for sufficiently strong shocks main limitation of the mechanism, caused by the escape of accelerated particles downstream of the shock during acceleration no longer exists.  相似文献   

Dynamo saturation in direct simulations of the multi‐phase turbulent interstellar medium     

A. Bendre  O. Gressel  D. Elstner 《Astronomische Nachrichten》2015,336(10):991-1004

The ordered magnetic field observed via polarised synchrotron emission in nearby disc galaxies can be explained by a mean‐field dynamo operating in the diffuse interstellar medium (ISM). Additionally, vertical‐flux initial conditions are potentially able to influence this dynamo via the occurrence of the magnetorotational instability (MRI). We aim to study the influence of various initial field configurations on the saturated state of the mean‐field dynamo. This is motivated by the observation that different saturation behaviour was previously obtained for different supernova rates. We perform direct numerical simulations (DNS) of three‐dimensional local boxes of the vertically stratified, turbulent interstellar medium, employing shearing‐periodic boundary conditions horizontally. Unlike in our previous work, we also impose a vertical seed magnetic field. We run the simulations until the growth of the magnetic energy becomes negligible. We furthermore perform simulations of equivalent 1D dynamo models, with an algebraic quenching mechanism for the dynamo coefficients. We compare the saturation of the magnetic field in the DNS with the algebraic quenching of a mean‐field dynamo. The final magnetic field strength found in the direct simulation is in excellent agreement with a quenched α) dynamo. For supernova rates representative of the Milky Way, field losses via a Galactic wind are likely responsible for saturation. We conclude that the relative strength of the turbulent and regular magnetic fields in spiral galaxies may depend on the galaxy's star formation rate. We propose that a mean field approach with algebraic quenching may serve as a simple sub‐grid scale model for galaxy evolution simulations including a prescribed feedback from magnetic fields. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

北京一次罕见夜间突发性强增温事件成因分析   总被引：4，自引：0，他引：4  

罗然  郑永光  陈敏 《气象》2020,46(4):478-489

夜间降温是正常的地表气温日变化,但统计表明北京及周边地区冬半年时常出现入夜后气温不降反升的现象,甚至出现了小时升温超过10℃的剧烈增温事件。这种增温具有明显的突发性,且很快转为降温,常对业务预报造成困扰。2010年11月26日夜间冷锋过境该区域造成了最强达12℃·h^-1的夜间急剧增温事件,与气候统计结果相比,该次增温幅度和影响区域范围非常罕见且极端。文章对其进行了详细诊断分析,使用的资料包括自动气象站、常规地面和探空、铁塔、卫星、风廓线雷达等观测资料和美国环境预报中心(NCEP)最终分析资料。分析结果表明:该次过程对流层低层有非常显著的冷平流;垂直速度诊断、卫星和风廓线雷达观测都表明,对流层中低层都存在显著的强下沉运动;铁塔观测和北京探空观测演变都表明增温过程中近地面大气有显著的湍流运动。分析此次罕见过程的机理包括三个方面:高原地区地面位温显著高于平原地区(二者最大可差10 K),是该次罕见增温事件形成的首要条件;强下沉运动使得低密度高位温空气强迫下沉到边界层,是增温必要条件;强湍流混合作用则是地面空气增温的必要机制。估算结果表明,边界层急流伴随的强湍流混合可引起约8℃的罕见地面空气增温。最后,给出了该次事件的机理概念模型。  相似文献   

Cloud dispersal in turbulent flows     

F. Heitsch  A. D. Slyz  J. E. G. Devriendt  A. Burkert 《Monthly notices of the Royal Astronomical Society》2006,373(4):1379-1388

  相似文献   

Cosmic ray scattering in compressible turbulence     

A. Lazarian  A. Beresnyak 《Monthly notices of the Royal Astronomical Society》2006,373(3):1195-1202

We study the scattering of low-energy cosmic rays (CRs) in a turbulent, compressive magnetohydrodynamic (MHD) fluid. We show that compressible MHD modes – fast or slow waves with wavelengths smaller than CR mean free paths induce cyclotron instability in CRs. The instability feeds the new small-scale Alfvénic wave component with wavevectors mostly along magnetic field, which is not a part of the MHD turbulence cascade. This new component gives feedback on the instability through decreasing the CR mean free path. We show that the ambient turbulence fully suppresses the instability at large scales, while wave steepening constrains the amplitude of the waves at small scales. We provide the energy spectrum of the plane-parallel Alfvénic component and calculate mean free paths of CRs as a function of their energy. We find that for the typical parameters of turbulence in the interstellar medium and in the intercluster medium the new Alfvénic component provides the scattering of the low-energy CRs that exceeds the direct resonance scattering by MHD modes. This solves the problem of insufficient scattering of low-energy CRs in the turbulent interstellar or intracluster medium that was reported in the literature.  相似文献   

Electric field representation of pulsar intensity spectra     

M. A. Walker  D. R. Stinebring 《Monthly notices of the Royal Astronomical Society》2005,362(4):1279-1285

  相似文献   

The interaction of cosmic rays and magnetized plasma     

A. R. Bell 《Monthly notices of the Royal Astronomical Society》2005,358(1):181-187

A large flux of cosmic rays streaming through a magnetized plasma creates cavities of low plasma density and low magnetic field. The magnetic field focuses the cosmic ray trajectories into the cavities with the possible formation of filaments or beams of high-energy cosmic rays.  相似文献   

Supersonic turbulence, filamentary accretion and the rapid assembly of massive stars and discs     

Robi Banerjee  Ralph E. Pudritz  Dave W. Anderson 《Monthly notices of the Royal Astronomical Society》2006,373(3):1091-1106

  相似文献   

高空急流区飞机颠簸的一种形成机制的探讨     

朱志愚 《成都信息工程学院学报》1997,(4)

作者应用动力学分析方法，结合观测飞机颠簸的事实，对高空急流区飞机颠簸的一种形成机理进行了理论探讨。结果表明，高空急流区温度平流分布的不均匀性，会在急流附近等温线密集区边缘激发出空气垂直运动和湍流，引起飞机颠簸。  相似文献   

Analysis of the effect of a mean velocity field on a mean field dynamo     

Alejandra Kandus 《Monthly notices of the Royal Astronomical Society》2007,378(4):1356-1364

We study semi-analytically and in a consistent manner the generation of a mean velocity field     by helical magnetohydrodynamical (MHD) turbulence, and the effect that this field can have on a mean field dynamo. Assuming a prescribed, maximally helical small-scale velocity field, we show that large-scale flows can be generated in MHD turbulent flows via small-scale Lorentz force. These flows back-react on the mean electromotive force of a mean field dynamo through new terms, leaving the original α and β terms explicitly unmodified. Cross-helicity plays the key role in interconnecting all the effects. In the minimal τ closure that we chose to work with, the effects are stronger for large relaxation times.  相似文献