大功率无线电波加热低电离层

等离子体对大功率电波的欧姆耗散会使电子温度升高,进而导致电子密度和其他等离子体参数改变,实现电离层的地面人工变态.本文基于大功率无线电波与低电离层相互作用的自洽模型,分析了不同入射条件下电离层参数的变化,主要结论如下:电离层D区是电波的主要吸收区,并且其吸收强度随入射频率的升高而降低,当入射频率为6 MHz（有效入射功率为200 MW）时电子温度的最大增幅约为520 K,电子密度最大增幅为7300 cm^-3左右;电子温度达到饱和所需时间小于电子密度的饱和时间,前者具有μs量级,后者具有ms量级;停止加热后,电子温度和密度迅速恢复到初始状态,恢复时间均小于各自的饱和时间,但量级相当;入射功率越高,电子温度和密度的增幅越大,并且饱和时间也越长,在相同入射条件下,夜晚的饱和时间要大于白天.     

基于一维模型的高频电波加热电离层F层数值研究

基于电离层一维仿真加热模型,详细介绍了模型中电子的动量方程、连续性方程、能量方程和各类参量表达式,利用对角矩阵追赶法数值求解电离层F层加热过程,分析了不同时次电子数密度和电子温度的变化,讨论了不同频率和不同功率电波加热的情形.结果表明:当高频电波加热高电离层时,电子温度迅速增加,并很快趋近于饱和状态;电子密度的变化较为迟缓,但在加热过程中其变化幅度却越来越大;电子密度变化量在沿磁场方向上形成空洞和上下稠团两峰一谷构型;频率越大、功率越高的电波加热时,电子密度的变化也越大,但存在一适值频率的电波对电子温度的影响最小.      

大功率无线电波与低电离层的相互作用

地面入射的大功率无线电波能加热电离层等离子体，引起电离层电子温度和密度的扰动，实现电离层的地面人工变态．本文中，着重考虑电波和电离层相互作用过程中的自吸收，构造一个自治的相互作用模型，在一定功率和频率的加热电波作用下，利用该模型计算了白天低电离层电子温度和由温度的变化而引起的电子密度的变化．计算结果表明，在白天低电离层，电波的自吸收在90km以下比较显著，而最大温度变化在70km高度上，大约增加了2倍．在α复合的假设下，电子密度变化幅度随高度的增加而减少，在70km处，大约增加55％、120km处则为4％左右．     

基于各向异性分布的非相干散射雷达谱仿真

基于离子在加热条件下呈现各向异性分布的假设,建立离子声波激发条件下非平衡态的三维离子速度分布函数模型,给出任意视线方向上非相干散射谱的计算方法,分析幅度修正因子、离子声速粒子组分、雷达波束方向与磁场方向夹角及温度各向异性对功率谱的影响.研究结果可以解释离子线谱超过一个量级的幅度增强现象和上行离子线强于下行离子线的不对称现象,对加热强扰动电离层条件下的等离子体参数反演具有重要意义.      

预加热时间对低电离层预加热幅度调制的影响

基于电离层连续方程和能量方程，建立预加热模式下低电离层幅度调制加热理论模型，模拟大功率电波幅度调制电离层电导率和电流随时间的变化，分析预加热时间对幅度调制产生的极低频/甚低频（ELF/VLF）强度的影响.结果表明，低电离层中的电流能够被大功率电波有效调制，可以作为ELF/VLF电波的辐射源.预加热幅度调制模式在预加热时间较长时效果更明显.在考虑能耗的情况下，当有效辐射功率为200MW及高频波的调制频率f_ELF/VLF为1kHz时，预加热幅度调制模式辐射ELF/VLF加热0.1s时效果最好，强度可提高约7.95dB.      

背景条件对低电离层预加热幅度调制的影响

基于电离层连续性方程和能量方程,建立了预加热模式下低电离层幅度调制加热理论模型,研究预加热阶段电离层电子密度和调制阶段电流随预加热时间的变化,探讨不同背景条件对幅度调制产生的极低频/甚低频（ELF/VLF）电磁波强度的影响.结果表明,预加热调制在90~100km高度效果较好,在夜间进行预加热调制激发的ELF/VLF强度增幅不明显,各季节中在春季调制强度增幅最大,太阳高年预加热调制比太阳低年的效果好,低纬地区强度增幅远大于中纬地区强度增幅.在一定加热条件下（有效辐射功率200MW,频率1kHz）,不同背景条件（除夜间外）下的预加热幅度调制模式在考虑能耗情况下,均在预加热10s时效果最好.      

宇宙噪声的电离层闪烁

本文给出了薄相屏近似条件下的电离层闪烁Fourier功率谱和Bessel功率谱与电离层不均匀结构电子密度涨落空间谱之间的关系。对窄波瓣天线Riometer获得的宇宙噪声资料进行了分析,结果表明:宇宙噪声资料包含着电离层不均匀结构的信息。Riometer观测结果也可用于电离层闪烁问题的研究。     

南京地区斜向加热电离层效应数值模拟

与垂直加热相比,斜向加热电离层具有灵活性高、影响范围广和便于实际操作等优势.在非偏区考虑欧姆吸收,基于电子能量方程和连续性方程构建电波斜向加热低电离层的物理模型,并利用IRI-2007和NRLMSISE-00经验模型提供的背景参数对南京地区斜向加热低电离层进行数值模拟,对比不同加热条件下电子温度和电子密度的扰动情况.研究结果表明:电波加热效果随入射仰角和有效辐射功率的增大而增大;电子温度和电子密度增幅随电波频率增大而减小;X波模比O波模造成的电子温度扰动幅度和电子密度扰动幅度更大,同时X波模比O波模能更快地使电子温度和电子密度达到稳定状态;一定范围内较小仰角、较低频率、较大有效辐射功率的电波能使电子密度更快达到稳定,后两者还能加快电子温度达到稳定的过程;电子温度达到稳定所需时间随入射电波仰角呈单峰变化,仰角为62°时达到最大.      

极光区电离层Hall电导率的观测及其在E层电子加热情况下的特征

本文利用欧洲的ＥＩＳＣＡＴ雷达观测资料及与这配合的地磁观测数据，用电离层参数直接计算和地面磁场反演两种方法导出了极区电离层Ｈａｌｌ电导率，特别显示出在强对流电场激发的Ｅ层等离子体不稳定波对电子加热情况下，电导率明显增高。     

太阳宁静及耀斑期间1AU附近等离子体轫致辐射研究

在太空等离子体中，尤其在等离子体内部磁场较弱时，轫致辐射是等离子体能量损失的主要机制．本文对太阳宁静及耀斑期间1AU处等离子体轫致辐射计算表明，等离子体辐射强度If的变化与辐射的电磁波频率有直接的关系．当辐射频率，接近于等离子体频率，fpe时，辐射强度显著增大．随着电磁波辐射频率的增大，辐射强度随频率增大作缓慢对数下降．辐射亮温Tb与等离子体电子温度Te、介质光深成正比．Tb与If随辐射频率变化的整体趋势一致．在相同的辐射频率情况下，太阳宁静期间If值、Tb值低于太阳耀斑期间If值、Tb值．     

热流效应对场向电流确定的影响

给出了任意速度分布函数条件下复频率的介电函数和色散关系的求解方法. 讨论了16矩近似条件下, 场向热流对电子速度分布函数, 介电函数实部与虚部, 以及离子与电子谐振频率和阻尼率的影响, 并与平衡态时麦克斯韦分布等离子体的计算结果进行了比较. 忽略场向热流效应, 正向电子漂移速度条件下, 上行等离子线探测, 会过高估计场向电流; 负向电子漂移速度条件下, 上行等离子线探测会过低估计场向电流. 对上下行等离子线同时探测情况, 忽略热流效应同样会过高估计场向电流.      

Electron density inversed by plasma lines induced by suprathermal electron in the ionospheric modification experiment

Incoherent scatter radar (ISR) is the most powerful ground-based measurement facility to study the ionosphere. The plasma lines are not routinely detected by the incoherent scatter radar due to the low intensity, which falls below the measured spectral noise level of the incoherent scatter radar. The plasma lines are occasionally enhanced by suprathermal electrons through the Landau damping process and detectable to the incoherent scatter radar. In this study, by using the European Incoherent Scatter Association (EISCAT) UHF incoherent scatter radar, the experiment observation presents that the enhanced plasma lines were observed. These plasma lines were considered as manifest of the suprathermal electrons generated by the high-frequency heating wave during the ionospheric modification. The electron density profile is also obtained from the enhanced plasma lines. This study can be a promising technique for obtaining the accurate electron density during ionospheric modification experiment.     

Characteristics of field line resonance type geomagnetic pulsations and variations of plasmaspheric plasma density distribution

The period of field line resonance (FLR) type geomagnetic pulsations depends on the length of the field line and on the plasma density in the inner magnetosphere (plasmasphere), where field lines are closed. Here as FLR period, the period belonging to the maximum occurrence frequency of the occurrence frequency spectrum (equivalent resonance curve) of pulsations has been considered. The resonance system may be replaced by an equivalent resonant circuit. The plasma density would correspond to the ohmic load. The plasma in the plasmasphere originates from the ionosphere, thus FLR period, occurrence frequency are also affected by the maximum electron density in the ionosphere. The FLR period has shown an enhancement with increasing F region electron density, while the occurrence frequency indicated diminishing trend (possible damping effect). Thus, the increased plasma density may be the cause of the decreased occurrence of FLR type pulsations in the winter months of solar activity maximum years (winter anomaly).     

Electromagnetic ion cyclotron resonance heating in the VASIMR

Plasma physics has found an increasing range of practical industrial applications, including the development of electric spacecraft propulsion systems. One of these systems, the Variable Specific Impulse Magnetoplasma Rocket (VASIMR) engine, both applies several important physical processes occurring in the magnetosphere. These processes include the mechanisms involved in the ion acceleration and heating that occur in the Birkeland currents of an auroral arc system. Auroral current region processes that are simulated in VASIMR include lower hybrid heating, parallel electric field acceleration and ion cyclotron acceleration. This paper will focus on using a physics demonstration model VASIMR to study ion cyclotron resonance heating (ICRH). The major purpose is to provide a VASIMR status report to the COSPAR community. The VASIMR uses a helicon antenna with up to 20 kW of power to generate plasma. This plasma is energized by an RF booster stage that uses left hand polarized slow mode waves launched from the high field side of the ion cyclotron resonance. The present setup for the booster uses 2–4 MHz waves with up to 20 kW of power. This process is similar to the ion cyclotron heating in tokamaks, but in the VASIMR the ions only pass through the resonance region once. The rapid absorption of ion cyclotron waves has been predicted in recent theoretical studies. These theoretical predictions have been supported with several independent measurements in this paper. The ICRH produced a substantial increase in ion velocity. Pitch angle distribution studies show that this increase takes place in the resonance region where the ion cyclotron frequency is equal to the frequency on the injected RF waves. Downstream of the resonance region the perpendicular velocity boost should be converted to axial flow velocity through the conservation of the first adiabatic invariant as the magnetic field decreases in the exhaust region of the VASIMR. In deuterium plasma, 80% efficient absorption of 20 kW of ICRH input power has been achieved. No evidence for power limiting instabilities in the exhaust beam has been observed.     

Asymmetric X-ray line broadening in solar flares

The symmetry and time development of X-ray spectral lines are examined for many flares using Yohkoh Bragg Crystal Spectrometer (BCS) observations. We examine the degree of line blueshift and asymmetric broadening as a function of flare impulsiveness. The results of the analysis present a consistent observational picture for the 16 flares that were studied. The blueshift of the total flare spectrum increases with increasing fractional rate of change of flux. This result supports models that predict stronger heating in flares results in more blueshifted plasma. It also suggests that most flares will exhibit very weak or no blueshifts if the peak fractional energy release rate remains relatively low. This will be the case if stationary plasma builds up quickly by early ‘gentle’ evaporation or rapid slowing of moving plasma, even when most of the hot plasma is generated by explosive chromospheric evaporation.     

双麦克斯韦分布下极区中层尘埃粒子带电研究

在大功率微波照射下，极区中层夏季回波（PMSE）会立刻消失，该现象被称为极区中层加热现象.在大功率微波照射极区中层时，电子在微波电场加速下产生的定向运动速度与热运动速度可以比拟，极区中层的尘埃等离子体服从双麦克斯韦分布.基于双麦克斯韦分布下尘埃粒子充电理论给出极区中层尘埃粒子的电荷分布，比较了大功率微波对极区中层加热前和加热时，尘埃粒子电荷以及极区中层电子浓度的变化.结果表明，采用大功率微波装置加热极区中层会影响电子对尘埃粒子的充电进而导致电子浓度变化，这对解释极区中层加热现象具有重要意义.      

原子磁强计原子气室无磁加热温控系统设计

介绍一种用于原子磁强计原子气室的无磁加热温控系统设计。针对温控系统加热电流产生的磁场干扰，设计了双层加热丝加热膜结构的加热器件，该加热器件利用同层平行反向电流和层间平行反向电流产生的磁场相互抵消以减小加热电流磁场噪声；设计了滑动平均滤波器对采集的温度信号实施滤波以减小随机噪声的干扰；结合设计的高频加热信号的产生电路、幅度控制电路和功率放大电路开展了实验测试。测试结果表明，研制的双层加热丝加热膜结构加热器件相比单层加热丝加热膜结构加热器件的电流磁场噪声抑制能力提高了约16倍，实现的无磁加热温控系统的温控能力达到1.2‰。