Geophysical phenomena during an ionospheric modification experiment at Tromsø, Norway

We present an analysis of phenomena observed by HF distance-diagnostic tools located in St. Petersburg combined with multi-instrument observation at Tromsø in the HF modified ionosphere during a magnetospheric substorm. The observed phenomena that occurred during the Tromsø heating experiment in the nightside auroral E_s region of the ionosphere depend on the phase of substorm. The heating excited small-scale field-aligned irregularities in the E region responsible for field-aligned scattering of diagnostic HF waves. The equipment used in the experiment was sensitive to electron density irregularities with wavelengths 12–15 m across the geomagnetic field lines. Analysis of the Doppler measurement data shows the appearance of quasiperiodic variations with a Doppler frequency shift, f_d and periods about 100–120 s during the heating cycle coinciding in time with the first substorm activation and initiation of the upward field-aligned currents. A relationship between wave variations in f_d and magnetic pulsations in the Y-component of the geomagnetic field at Tromsø was detected. The analysis of the magnetic field variations from the IMAGE magnetometer stations shows that ULF waves occurred, not only at Tromsø, but in the adjacent area bounded by geographical latitudes from 70.5° to 68° and longitudes from 16° to 27°. It is suggested that the ULF observed can result from superposition of the natural and heater-induced ULF waves. During the substorm expansion a strong stimulated electromagnetic emission (SEE) at the third harmonic of the downshifted maximum frequency was found. It is believed that SEE is accompanied by excitation of the VLF waves penetrating into magneto-sphere and stimulating the precipitation of the energetic electrons (10–40 keV) of about 1-min duration. This is due to a cyclotron resonant interaction of natural precipitating electrons (1–10 keV) with heater-induced whistler waves in the magnetosphere. It is reasonable to suppose that a new substorm activation, exactly above Tromsø, was closely connected with the heater-induced precipitation of energetic electrons.     

Reinvestigation of the irregularities in the 3H decay

Having in mind the potential impact of the results presented by Veprev and Muromtsev (2012) [13] on our knowledge of the universe, we reinvestigated the liquid scintillation measurement of the count rate variations of ³H. Making use of the sophisticated Quantulus liquid scintillation spectrometer, we found that the measurement of the high-energy tail of ³H spectrum may be significantly influenced by instrumental instability. Thus, the possible explanation for the relatively high count rate variations of Veprev and Muromtsev (2012) [13] can be attributed mainly to the walk of the cut-off in the integrated spectrum, although weak variations of different origin could be masked by such cut-off drifts. In our experiment we have also registered the oscillatory behavior of measured high-energy tail of ³H spectrum, but with very small amplitude (less than 0.5%), which cannot be easily explained only by instrumental instability. When the total ³H spectrum was measured, no significant variations in the count rate were found.     

GNSS基本服务性能评估

针对现有全球卫星导航系统性能评估无规范的评估标准问题,该文提出了以统一模型和算法为评估体系的方法,较详细的评估了全球卫星导航系统公开服务信号的基本性能,主要评估了空间信号误差、广播电离层模型改正效率及伪距单点定位精度等。结果表明:空间信号误差方面,伽利略最优、GPS和北斗三号相当;广播电离层模型方面,北斗全球广播电离层模型改正效果最优,GPSK8与NeQuick模型在低中纬度改正效果相当,北斗区域电离层模型在其服务区内具有较高改正效果;定位方面,北斗、GPS和伽利略静态伪距单点定位的三维位置均方根误差优于5m,格洛纳斯优于10 m;动态伪距单点定位方面,北斗在中国境内定位精度最高;基于统一评估体系下,可以直观对比得到目前各卫星导航系统的性能差异,同时也为后续的建设提供相应的参考。     

Day-side ionospheric conductivities at Mars

We present estimates of the day-side ionospheric conductivities at Mars based on magnetic field measurements by Mars Global Surveyor (MGS) at altitudes down to ∼100 km during aerobraking orbits early in the mission. At Mars, the so-called ionospheric dynamo region, where plasma/neutral collisions permit electric currents perpendicular to the magnetic field, lies between 100 and 250 km altitude. We find that the ionosphere is highly conductive in this region, as expected, with peak Pedersen and Hall conductivities of 0.1-1.5 S/m depending on the solar illumination and induced magnetospheric conditions. Furthermore, we find a consistent double peak pattern in the altitude profile of the day-side Pedersen conductivity, similar to that on Titan found by Rosenqvist et al. (2009). A high altitude peak, located between 180 and 200 km, is equivalent to the terrestrial peak in the lower F-layer. A second and typically much stronger layer of Pedersen conductivity is observed between 120 and 130 km, which is below the Hall conductivity peak at about 130-140 km. In this altitude region, MGS finds a sharp decrease in induced magnetic field strength at the inner magnetospheric boundary, while the day-side electron density is known to remain high as far down as 100 km. We find that such Titan-like behaviour of the Pedersen conductivity is only observed under regions of strongly draped magnetospheric field-lines, and negligible crustal magnetic anomalies below the spacecraft. Above regions of strong crustal magnetic anomalies, the Pedersen conductivity profile becomes more Earth-like with one strong Pedersen peak above the Hall conductivity peak. Here, both conductivities are 1-2 orders of magnitude smaller than the above only weakly magnetised crustal regions, depending on the strength of the crustal anomaly field at ionospheric altitudes. This nature of the Pedersen conductivity together with the structured distribution of crustal anomalies all over the planet should give rise to strong conductivity gradients around such anomalies. Day-side ionospheric conductivities on Mars (in regions away from the crustal magnetic anomalies) and Titan seem to behave in a very similar manner when horizontally draped magnetic field-lines partially magnetise a sunlit ionosphere. Therefore, it appears that a similar double peak structure of strong Pedersen conductivity could be a more general feature of non-magnetised bodies with ionised upper atmospheres, and thus should be expected to occur also at other non-magnetised terrestrial planets like Venus or other planetary bodies within the host planet magnetospheres.     

液闪法测量水中氚放射性活度的淬灭效应

采用液体闪烁计数法进行放射性同位素测量时存在淬灭效应,而且几乎每个样品的淬灭程度都不同,并影响测量精度。采用液体闪烁计数法测量水中氚的放射性活度,淬灭是难以避免的,因此要进行淬灭校正,才能使不同淬灭程度的样品的测量结果具有可比性。淬灭校正的方法有很多,外标准校正法是一种比较可靠的方法。文章采用氚外标准校正法进行实验,得出淬灭校正曲线即探测效率E与淬灭参数SQP(E)的关系式为E=0.001 3SQP(E)-0.707 6,经过样品验证,该曲线是可靠的。采用外标准校正法适合于大批样品的测量。     

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电离层闪烁对GNSS接收机性能影响比较分析

电离层闪烁是引起GNSS接收机性能降低甚至失锁的重要环境干扰因素。利用实测数据,比较分析了不同电离层闪烁活动强度下,不同GNSS系统（BD和GPS）接收机的定位性能。结果表明：电离层闪烁较弱时（S4〈0．3）,两种接收机均可以实现基本的定位功能;电离层闪烁较强（S4〉0.7）,且持续时间较长时,不同GNSS接收机将出现定位结果的抖动、跳变或失去定位能力;GNSS接收机应对电离层闪烁影响的能力与接收机设计相关。研究结果可作为抗闪烁接收机开发或闪烁影响分级的参考。     

Watching meteors on Triton

The thin atmosphere of Neptune's moon Triton is dense enough to ablate micrometeoroids as they pass through. A combination of Triton's orbital velocity around Neptune and its orbital velocity around the Sun gives a maximum meteoroid impact velocity of approximately 19 km s⁻¹, sufficient to heat the micrometeoroids to visibility as they enter. The ablation profiles of icy and stony micrometeoroids were calculated, along with the estimated brightness of the meteors. In contrast to the terrestrial case, visible meteors would extend very close to the surface of Triton. In addition, the variation in the meteoroid impact velocity as Triton orbits Neptune produces a large variation in the brightness of meteors with orbital phase, a unique Solar System phenomenon.     

Pulsar investigation using interstellar scintillation

We discuss the resolution of pulsar magnetospheres using interstellar scintillation. The two-dimensional spatial structure of pulsar emission zones can be obtained from analysis of diffractive scintillations at low frequencies. Based on refractive and diffractive scintillation of pulsars we can also reconstruct the distribution of turbulent plasma along the line of sight, and using this analysis a new approach to pulsar distance estimation can be made. This revised version was published online in July 2006 with corrections to the Cover Date.     

双成分星际介质的折射闪烁

本文用比较严格的理论讨论了由连续介质和散射薄屏组成的星际介质对河外射电源的折射闪烁．对折射闪烁引起的流量变化的结构函数Ｄ（τ）（τ为迟后时间）的计算表明，结构函数的幂律部份的指数Ｐ（Ｄ（τ）（∝τＰ）依赖于上述两个成份的相对散射强度，即在连续介质散射为主的情况下；而在薄屏散射为主的情况下；若两个成份的散射可相比较时，１＜Ｐ＜２．因此本模型可以用于解释在河外射电源和脉冲星中观测到的折射闪烁的结构函数具有不同幂指数的情形，特别是Ｐ～１．５的情形．