The heliospheric modulation of cosmic rays: Effects of a latitude dependent solar wind termination shock

Observations made with the two Voyager spacecraft confirmed that the solar wind decelerates to form the heliospheric termination shock and that it has begun its merger with the local interstellar medium. The compression ratio of this shock affects galactic cosmic rays when they enter the heliosphere. Hydrodynamic (HD) models show that the compression ratio can have a significant latitude dependence; with the largest value in the nose direction of the heliosphere, becoming significantly less towards the polar regions. The modulation effects of such large latitude dependence are studied, using a well-established numerical drift and shock modulation model. We focus on computing the modulated spectra for galactic protons with emphasis on the radial and polar gradients in the equatorial plane and at a polar angle of θ = 55°, corresponding to the heliolatitude of Voyager 1. Two sets of solutions are computed and compared each time; with and without a latitude dependence for the compression ratio. All computations are done for the two magnetic field polarity cycles assuming solar minimum conditions. Including the termination shock in the model allows the study of the re-acceleration of galactic protons in the outer heliosphere. We find that for the A < 0 polarity cycle the intensity between ∼200 MeV and ∼1 GeV in the vicinity of the shock in the heliospheric equatorial plane may exceed the local interstellar value specified at the heliopause. Unfortunately, at θ = 55°, the effect is reduced. This seems not possible during an A > 0 cycle because significant modulation is then predicted between the heliopause and the termination shock, depending on how strong global gradient and curvature drifts are in the heliosheath. The overall effect of the shock on galactic protons in the equatorial plane is to reduce the total modulation as a function of radial distance with respect to the interstellar spectrum. Making the compression ratio latitude dependent enhances these effects at energies E < 200 MeV in the equatorial plane. At larger heliolatitudes these effects are even more significant. The differences in the modulation between the two drift cycles are compelling when the compression ratio is made latitude dependent but at Earth this effect is insignificant. A general result is that the computed radial gradient changes for galactic protons at and close to the TS and that these changes are polarity dependent. In line with previous work, large polarity dependent effects are predicted for the inner heliosphere and also close to the shock’s position in the equatorial plane. In contrast, at θ = 55°, the largest polarity effect occurs in the middle heliosphere (50 AU), enhanced by the latitude dependence of the compression ratio. At this latitude, the amount of proton modulation between the heliopause and the termination shock is much reduced. If galactic cosmic rays were to experience some diffusive shock acceleration over the 100–1000 MeV range at the shock, the radial gradient should change its sign in the vicinity of the shock, how large, depends on the compression ratio and the amount of drifts taking place in the outer heliosphere. The effective polar gradient shows a strong polarity dependence at Earth but this dissipates at θ = 55°, especially with increasing radial distance. This tendency is enhanced by making the compression ratio latitude dependent.     

Kinetic theory of sheath formation in solar wind plasma

We present a general self-consistent kinetic theory for plasma sheath formation in solar wind plasma. The theory could be applied to anisotropic, as well as to isotropic collisionless plasma without resorting to any simplifications, limitations, or assumptions, such as the necessary existence of a ‘pre-sheath’ region of ions acceleration to ensure the Bohm criterion. The kinetic framework is first applied to sheath formation around an arbitrary oriented planar absorbing surface, charged by solar wind anisotropic plasma, under the condition of negligible photoelectric effect. We then make use of our kinetic approach for the plane geometry in isotropic collisionless plasma, as a particular case of a planar electrode orientation parallel to plasma streaming velocity, also analyzing the sheath structure around spherical and cylindrical absorbing electrodes submerged in isotropic collisionless plasma. Obtained results demonstrate principal differences in spatial charge distributions in sheath regions between spherical or cylindrical electrodes of large size and an unbound planar surface submerged in isotropic plasma. In the case of a planar electrode, we directly compare results obtained in our kinetic and hydrodynamic theories and conventional hydrodynamic theory of plasma sheath formation. The outcome from the present study have direct implications to the analysis of plasma sheath structure and associated distribution in space of charged dust grains, which is relevant to the moon exploration near the optical terminator region or in shadowed craters in the moon.     

低速风洞绳牵引并联支撑系统的模型气动试验研究(英文)

根据绳牵引并联机构的优点,建造了一种新型的用于低速风洞试验的飞机模型绳牵引并联支撑系统,研究该系统中模型的空气动力参数的测量与计算方法。文中对机构进行了静力学分析,建立了描述实验模型气动载荷的数学模型,提出了通过测量绳系拉力求得模型空气动力参数的解算方法;设计并构建了绳系拉力测量及数据采集系统;将该系统置于开口式回流低速风洞中进行了吹风试验,采集了模型在不同姿态和不同风速下的各牵引绳的拉力数据,并对数据进行了处理分析,通过解算得到了不同吹风条件下模型的气动载荷参数曲线。研究结果表明,绳牵引并联机构用于低速风洞试验的支撑系统是可行的。     

内埋式模型操纵面自动变角度系统研制

针对风洞试验模型操纵面角度的改变,开发了内埋式自动变角机构及控制系统,对控制角度进行了地面校准,并采用三角翼模型进行了风洞常规测力实验、重复性实验和操纵面效率试验。结果表明,采用自动变角机构改变操纵面角度的试验精准度均较高,完全满足国军标的要求,说明本操纵面自动变角系统的研制是成功的,在风洞试验中可以代替人工更换角度片方式,大大提高实验效率。     

斜拉索风雨振动及制振措施的风洞试验研究

采用全尺寸节段模型,进行了3种不同直径光面索的风雨振动风洞试验,并在各自雨振发生的临界风速、姿态及雨量条件下,和表面附加螺旋肋条及压花后的模型,进行了对比试验,且考察了不同阻尼条件下模型的振动特性,由此探索出对抑制雨振效果较佳的斜拉索表面形式及合适的阻尼比。     

Global Hybrid Simulation of Magnetic Reconnection in the Magnetosheath

A three-dimensional (3-D) global hybrid simulation is carried out for the generation and structure of magnetic reconnection in the magnetosheath due to interaction of an interplanetary Tangential Discontinuity (TD) with the bow shock and magnetosphere. Runs are performed for solar wind TDs possessing different initial half-widths. As the TD propagates through the bow shock toward the magnetopause, it is greatly narrowed by a two-step compression processes, a "shock compression' followed by a subsequent ``convective compression'. In cases with a relatively thin solar wind TD, 3-D patchy reconnection is initiated in the transmitted TD, forming magnetosheath flux ropes. Multiple components of ion particles are present in the velocity distribution in the magnetosheath merging, accompanied by ion heating. For cases with a relatively wide initial TD, a dominant single X-line appears in the subsolar magnetosheath after the transmitted TD is narrowed. A shock analysis is performed for the detailed structure of magnetic reconnection in the magnetosheath. Rotational Discontinuity (RD)/Time-Dependent Intermediate Shock (TDIS) are found to dominate the reconnection layer, which and some weak slow shocks are responsible for the ion heating and acceleration.      

风洞分布式支撑天平测力试验技术研究

采用双尾支撑测量形式的加工、装配误差会使系统内应力过大,影响测量精度。针对某“双机身”飞机CTS 风洞试验气动力测量需求,发展基于多维力天平内置的风洞分布式支撑天平测力试验技术;研制具有消除系统内应力功能的双支撑系统,提出两种6 分量双支撑天平校准及测力方法,并对数据处理和双支撑系统可靠性进行检验加载、对比分析和验证。结果表明：风洞分布式支撑天平测力试验技术能够有效消除双支撑天平系统由于过约束而导致的固有装配内应力,双支撑天平系统各部分连接、测量可靠;两种校准测力方法测量精度相当,均能达到单台应变天平测量误差水平,可满足风洞试验测量精度需求;综合考虑现有校准设备校准能力,最终采用“合成式校准测力”方法进行的风洞试验,获得了满意的试验测力精度。     

风洞虚拟飞行模型机与原型机动力学特性分析

在低速风洞虚拟飞行试验系统中,采用三自由度（3-DOF）球铰支撑动力学相似缩比飞机模型,在气动力矩作用下试验模型可绕质心自由转动。这种带约束的运动与具有六自由度（6-DOF）的真实大气飞行存在差别,鉴于此,对各影响因素逐个剖离并进行了数值模拟和对比分析。结果表明：位移约束使两者间的动力学特性产生较明显的差异,缩比的影响符合相似准则规律,机构摩擦、模型重心与支撑点不重合影响较小,常值干扰力矩对模型的初始响应有一定影响。对比分析结果可以用于指导风洞虚拟飞行试验的开展,并有助于完善风洞虚拟飞行试验技术及其拓展应用。     

城市风场环境中的无人机快速航迹规划方法

密集的城市障碍环境以及复杂的城市风场干扰对航迹规划的实时性和航迹跟踪的准确性提出了严格要求,为此提出一种城市风场环境中的小型无人机(UAVs)快速航迹规划方法。首先,为了保证航迹规划的高效性,对固定翼无人机运动学方程进行了合理简化。其次,由于障碍环境中的最优航迹难以直接完全塑造,因此根据状态受限的最优控制理论给出了可以使用螺旋线与直线构建近似最优航迹的结论,并据此提出了一种针对城市环境的三维航迹规划方法。然后,通过对无人机运动学模型的分析,从规划角度提出了风场干扰下的航迹设计准则。仿真实验中,首先通过算法对比实验,验证了航迹规划方法的高效性;然后使用六自由度(DOF)飞机模型分别在无风场干扰和有风场干扰的环境下进行了航迹跟踪实验,实验结果证明了风场干扰下航迹设计准则的有效性。     

飞行控制律对体自由度颤振特性影响试验

飞翼飞机易发生刚体短周期模态与机翼低阶弯曲模态耦合所致的体自由度颤振。飞行控制系统对飞机的短周期模态特性影响很大,因此考虑飞行控制系统的闭环体自由度颤振特性值得进一步研究。针对自主设计的颤振模型开发了相应的俯仰姿态保持控制律,综合运用风洞试验和仿真计算开展了相关研究,获得了不同刚体自由边界条件下的开环/闭环体自由度颤振特性,研究了闭环增益对体自由度颤振特性的影响规律,简要分析了影响机理。试验和仿真计算结果共同表明：俯仰姿态保持控制律明显地改变了俯仰模态阻尼的原有走势,闭环后的体自由度颤振特性变化明显。以开环颤振速度为基准,采用较小的比例回路增益K_P或较大的微分回路增益K_D,飞行控制律能增加飞行器俯仰阻尼,提高体自由度颤振速度,反之飞行控制律将导致颤振速度降低。就本文控制律而言,当K_P<0.07或K_D>0.2时俯仰姿态保持控制律能起到抑制体自由度颤振的作用。