Broadband electrostatic noise and low-frequency waves in the Earth’s magnetosphere

Broadband electrostatic noise (BEN) is commonly observed in different regions of the Earth’s magnetosphere, eg., auroral region, plasma sheet boundary layer, etc. The frequency of these BENs lies in the range from lower hybrid to the local electron plasma frequency and sometimes even higher. Spacecraft observations suggest that the high and low-frequency parts of BEN appear to be two different wave modes. There is a well established theory for the high-frequency part which can be explained by electrostatic solitary waves, however, low-frequency part is yet to be fully understood. The linear theory of low-frequency waves is developed in a four-component magnetized plasma consisting of three types of electrons, namely cold background electron, warm electrons, warm electron beam and ions. The electrostatic dispersion relation is solved, both analytically and numerically. For the parameters relevant to the auroral region, our analysis predict excitation of electron acoustic waves in the frequency range of 17 Hz to 2.6 kHz with transverse wavelengths in range of (1–70) km. The results from this model may be applied to explain some features of the low-frequency part of the broadband electrostatic noise observed in other regions of the magnetosphere.     

A gravity wave analysis near to the Andes Range from GPS radio occultation data and mesoscale numerical simulations: Two case studies

Global maps of potential wave energy per unit mass, recently performed with the Global Positioning System (GPS) Radio Occultation (RO) technique and different satellite missions (CHAMP and SAC-C since 2001, GRACE and COSMIC since 2006) revealed in Argentina, at the eastern side of the highest Andes Mountains, a considerable wave activity (WA) in comparison with other extra-tropical regions. The main gravity wave (GW) sources in this natural laboratory are deep convection (mainly during late Spring and Summer), topographic forcing and geostrophic adjustment.     

Detecting gravitational waves from accreting neutron stars

The gravitational waves emitted by neutron stars carry unique information about their structure and composition. Direct detection of these gravitational waves, however, is a formidable technical challenge. In a recent study we quantified the hurdles facing searches for gravitational waves from the known accreting neutron stars, given the level of uncertainty that exists regarding spin and orbital parameters. In this paper we reflect on our conclusions, and issue an open challenge to the theoretical community to consider how searches should be designed to yield the most astrophysically interesting upper limits. With this in mind we examine some more optimistic emission scenarios involving spin-down, and show that there are technically feasible searches, particularly for the accreting millisecond pulsars, that might place meaningful constraints on torque mechanisms. We finish with a brief discussion of prospects for indirect detection.     

Moderate geomagnetic storms of January 22–25, 2012 and their influences on the wave components in ionosphere and upper stratosphere-mesosphere regions

Moderate geomagnetic storms occurred during January 22–25, 2012 period. The geomagnetic storms are characterized by different indices and parameters. The SYM-H value on January 22 increased abruptly to 67 nT at sudden storm commencement (SSC), followed by a sharp decrease to −87 nT. A second SSC on January 24 followed by a shock on January 25 was also observed. These SSCs before the main storms and the short recovery periods imply the geomagnetic storms are CME  -driven. The sudden jump of solar wind dynamic pressure and IMF _Bz$B_z$ are also consistent with occurrence of CMEs. This is also reflected in the change in total electron content (TEC) during the storm relative to quiet days globally. The response of the ionospheric to geomagnetic storms can also be detected from wave components that account for the majority of TEC variance during the period. The dominant coherent modes of TEC variability are diurnal and semidiurnal signals which account upto 83% and 30% of the total TEC variance over fairly exclusive ionospheric regions respectively. Comparison of TEC anomalies attributed to diurnal (DW1) and semidiurnal (SW2) tides, as well as stationary planetary waves (SPW1) at 12 UTC shows enhancement in the positive anomalies following the storm. Moreover, the impact of the geomagnetic storms are distinctly marked in the daily time series of amplitudes of DW1, SW2 and SPW1. The abrupt changes in amplitudes of DW1 (5 TECU) and SW2 (2 TECU) are observed within 20°S–20°N latitude band and along 20°N respectively while that of SPW1 is about 3 TECU. Coherent oscillation with a period of 2.4 days between interplanetary magnetic field and TEC was detected during the storm. This oscillation is also detected in the amplitudes of DW1 over EIA regions in both hemispheres. Eventhough upward coupling of quasi two day wave (QTDWs) of the same periodicity, known to have caused such oscillation, are detected in both ionosphere and upper stratosphere, this one can likely be attributed to the geomagnetic storm as it happens after the storm commencement. Moreover, further analysis has indicated that QTDWs in the ionosphere are strengthened as a result of coherent oscillation of interplanetary magnetic field with the same frequency as QTDWs. On the otherhand, occurrences of minor SSW and geomagnetic storms in quick succession complicated clear demarcation of attribution of the respective events to variability of QTDWs amplitudes over upper stratosphere.     

Study of VLF wave with relativistic effect in Saturn magnetosphere in the presence of parallel A.C. electric field

Cassini radio and plasma wave surveys aim to study radio emissions, plasma waves, thermal plasma and dust near Saturn. Using the characteristic solution and dynamics method, the influence of electron beam on the loss cone and bi-Maxwellian distribution of whistler mode waves in the parallel alternating electric field and magnetic field is studied. The dispersion relation and the growth rate of Saturn's magnetic layer were deduced and calculated in detail. Parameter analysis is performed by changing the parameters of the plasma like number density, AC frequency, temperature anisotropy, etc. The influence of AC frequency on Doppler shift and the comparative study of growth rate of oblique and parallel propagating waves are analyzed using generalized distribution function. We found temperature anisotropy ${\text{A}}_{\text{T}}=1.25$ can explain the linear spatiotemporal growth rate of whistler mode waves. It provides the majority of the observed frequency integral power. It can be seen that the effective parameters for the generation of Whistler mode waves are not only temperature anisotropy, but also the relativistic factors discussed in the results and discussion section, and the AC field frequency and width of the loss cone distribution function.     

高海况下反舰导弹对舰船目标攻击策略

反舰导弹攻击海面舰船目标时,通常根据目标的散射特征数据进行目标类型判定并做出决策。但是在高海况下:如果导弹横浪飞行,海浪对导弹命中目标的影响会变小,基本能保证可靠命中目标;但如果导弹顶浪飞行,则海浪会引起目标雷达反射截面积(Radar Cross Section,RCS)的起伏甚至突变,影响导弹对目标的锁定和判断。文章建立了不同海况和舰船目标的融合模型,并针对融合模型仿真计算了导弹不同突击方向时的 RCS,最终根据高海况时舰船横浪或顶浪航行的原则,按照捕捉概率最大的方向确定导弹的攻击方向。     

基于不相干平面波叠加以模拟混响声场的航天器低频声固耦合分析

文章针对航天器在混响声场中的随机振动问题,提出一种通过多个不相干的平面波线性叠加以模拟混响声场的实现方法,给出了每个平面波的具体参数并从理论上证明其满足理想混响声场假设。在此基础上利用有限元-边界元耦合方法对整星低频声固耦合问题进行分析,并用混响室噪声试验响应数据进行了验证。研究结果表明:该方法理论推导正确,为航天器低频声固耦合分析及声振力学环境预示提供了一种新的有效手段。     

The radiation impedance of electrodynamic tethers in a polar Jovian orbit

Juno, the second mission in the NASA New Frontiers Program, will both be a polar Jovian orbiter, and use solar arrays for power, moving away from previous use of radioisotope power systems (RPSs) in spite of the weak solar light reaching Jupiter. The power generation at Jupiter is critical, and a conductive tether could be an alternative source of power. A current-carrying tether orbiting in a magnetized ionosphere/plasmasphere will radiate waves. A magnitude of interest for both power generation and signal emission is the wave impedance. Jupiter has the strongest magnetic field in the Solar Planetary System and its plasma density is low everywhere. This leads to an electron plasma frequency smaller than the electron cyclotron frequency, and a high Alfven velocity. Unlike the low Earth orbit (LEO) case, the electron skin depth and the characteristic size of plasma contactors affect the Alfven impedance.     

低中等雷诺数超声速轴对称射流气动声场

采用线性抛物化稳定性方程(LPSE)方法对低、中等雷诺数条件下的超声速轴对称射流进行了研究。结果表明:射流中不稳定波的增长特性决定了声辐射的特性。在低雷诺数条件下,不稳定波的频率范围较窄,且由于不稳定波的增长区间较长,因此声辐射的范围较宽,声源不集中,声辐射的方向角不明确。在中雷诺数条件下,不稳定波的频率范围较宽,且由于不稳定波的增长区间较短,因此声辐射的范围较窄,声源集中,声辐射的方向角较明确;且随着斯特劳哈尔数增加,声辐射的方向角增加。在低雷诺数条件下,射流基本流的法向速度对射流气动声场的影响较弱,而在中等雷诺数条件下,其对射流的气动声场影响较强。      

基于线性频散信号构建的复杂航空结构Lamb波高分辨率损伤成像

在对复杂航空结构的Lamb波损伤成像中,Lamb波频散容易使信号波包发生扩展和变形,从而降低信号的分辨率,并最终影响损伤监测结果,因此Lamb波频散补偿已成为急需解决的一个重要问题。目前常用的频散补偿方法需要理论计算Lamb波频散曲线,难以适用于复杂航空结构。本文利用现场直接测得的相对波数曲线进行线性频散信号构建(Linearly-dispersive signal construction,LDSC)的频散补偿处理,解决了航空复杂结构中Lamb波频散难以补偿的问题。然后,将LDSC用于延迟叠加损伤成像中,以实现高分辨率损伤成像。为了降低多反射的复杂航空结构形式对成像结果的影响,引入了1.5波峰正弦调制的准宽带Lamb波激励波形。最后通过在真实复杂的某型飞机大梁结构上的实验证明了所提方法的有效性。