一种基于温度参数的热层密度修正方法

热层大气的阻力效应是影响低轨航天器大量空间操作的重要因素, 尤其是经验密度模式, 其固有的至少15%的内符合误差已严重制约航天器轨道计算精度的提高. 针对广泛应用的经验密度模式, 选择物理背景简明、关联参数较少的JACCHIA71模式, 以地磁平静条件下的全球散逸层顶温度最小值T_c及125 km高度拐点温度T_x为对象, 建立密度相对于上述温度参数的条件方程, 推导密度相对于温度参数的解析偏导数, 并给出其最小二乘解. 同时, 利用CHAMP卫星数据对模式进行修正, 模式平均误差从40%降低至3%左右. 通过TG01飞行器的轨道预报比较, 修正前后轨道预报位置精度从2 km提升至1 km左右. 经过CHAMP卫星和TG01飞行器的实测数据检验, 验证了修正算法的正确性和有效性.     

强磁暴期间TIEGCM模式与CHAMP卫星热层大气密度的比较分析

利用NCAR-TIEGCM模式计算了2003年11月20—21日强磁暴期间410km高度上的大气密度,并与CHAMP/STAR加速度计反演数据进行对比和分析. 结果表明,模式结果能够准确反映磁暴期间大气密度的分布和变化情况,与实测结果在变化趋势和量级上具有较好的一致性,但在精细结构和数值大小上仍存在一定差异. 模式低估了磁暴期间大气密度的增幅,实测大气密度增幅高达250%～400%,而模式结果为100%～125%. 模式结果与实测数据的偏差在高纬地区高于低纬地区,日侧高于夜侧. 通过模式和实测数据的分析发现,磁暴期间大气密度扰动具有日夜侧和南北半球不对称性. 此外,模式能够准确反映磁暴期间大气密度扰动从高纬向低纬的传播以及大气密度对SYM-H指数响应的延迟特性.     

不同强度磁暴期间热层大气密度响应特征分析

利用CHAMP卫星数据,对2002-2008年12个不同强度磁暴事件期间的热层大气密度变化特征进行分析,并研究对应磁暴期间大气模式NRLMSISE-00分布特征.结果表明,大磁暴期间日侧大气密度峰值从高纬到低纬的时间延迟为2h,中小磁暴期间的延迟时间为3～4h;春秋季暴时大气密度分布基本呈南北对称分布,而夏冬季大气密度的分布是夏半球大于冬半球,春秋季暴时大气密度大于夏冬季;NRLMSISE-00大气模式得到的热层大气密度很好的体现了半球分布以及季节分布的特征,但模式模拟结果偏小;Dst指数峰值比ap指数峰值更能反应大气密度的变化情况.     

Variations in the thermosphere and ionosphere response to the 17–20 April 2002 geomagnetic storms

The responses of the thermospheric density and ionospheric foF2 to the intense magnetic storms event on 17–20 April were analyzed by using data from CHAMP/STAR and ionosonde stations respectively, and NRLMSISE-00 and IRI-2007 models were used to simulate. The models can capture the tendency of changes, especially under quiet or moderate geomagnetic conditions, but are less accurate under geomagnetic storms. The thermospheric density is sensitive to the EUV emission and geomagnetic activity, and double-peak structure appeared in the dayside. On 19 April dayside, TADs traveled toward the equator with phase speeds of the order of 300–750 m/s, interfered near the equator to produce a total density perturbation of 25%, and then passed through each other and into the opposite hemisphere. For ionospheric foF2, there are non-symmetric hemispheres’ features during the intense geomagnetic activities. In details, middle latitudes in the north and high latitudes in both hemispheres are negative ionospheric storms, and the maximum amplitudes of δfoF2$\delta \mathit{foF}2$ is about 60%, but the amplitudes decrease from the higher to lower latitudes in the Southern Hemisphere. Meanwhile, the equatorial station shows positive phase, and the maximum value is about 100%. Finally, the mechanisms for these features will be discussed in this study.     

基于CHAMP卫星观测数据对热层大气密度的经验正交分析

对2003年(太阳活动较高年)至2007年(太阳活动低年) CHAMP卫星的热层大气密度观测数据进行了经验正交函数(EOF)分析, 得到了400 km高度上白天平均大气密度ρ的太阳活动周变化与年度变化等不同变化分量. 研究结果表明, ρ受太阳活动影响较大, 其太阳周变化分量与F10.7指数变化之间的相关系数可高达94.5 %; ρ的太阳周变化分量随纬度增加而减小, 且在中高纬地区, 南半球的值明显大于北半球的值, 在低纬地区则出现基本对称的双峰分布, 即赤道质量密度异常(EMA)结构. 在ρ的年变化中, 呈现出明显的季节变化, 即夏季低冬季高; 同时ρ的年变化幅度随太阳活动增加而增强, 随纬度增加而增强. 将本文结果与经验模式NRLMSISE00在观测条件下的输出数据进行对比, 发现两者的太阳周变化与年变化分量基本一致, 但本文观测数据的太阳周成分随纬度变化略小, 年变化幅度略大, 且NRLMSISE00模式不能再现EMA结构. 研究结果对揭示热层气候学变化特征具有重要意义.     

Pre-storm behaviour of NmF2 and TEC (GPS) over equatorial and low latitude stations in the Indian sector

The pre-storm behavior of NmF₂ and TEC over an equatorial station, Trivandrum (8.47°N, 76.91°E, dip 0.6°S) and a low latitude station, Waltair (17.7°N,83.3°E, dip 20°N) has been studied for a total of 18 strong geomagnetic storms with DST ? −100 nT. The simultaneous measurements of GPS-TEC and NmF₂ over Trivandrum and Waltair during the period 2000–2005 have been considered for the present study. It is found that there is a substantial increase in NmF₂ and TEC before the onset of the storm over Waltair, while the increase is not present at Trivandrum. The origin of pre-storm enhancements in electron density still remains unresolved owing to several conditions in their potential sources and occurrence mechanisms. In the present study an attempt is made to identify the possible mechanisms responsible for such enhancements in electron density of the F-region.     

1998年4月下旬至5月上旬地磁暴的日地事件认证

综合运用SOHO/LASCO、SOHO/EIT关于CME的观测结果和WIND飞船关于太阳风的观测记录,识别了1998年4月下旬至5月上旬发生的磁暴的CME源,分析了与5月初强磁暴群相联系的日地事件.结果表明,所用日地扰动事件关系认证的方法是可行的.本文就上述日地事件所涉及的磁暴群与活动区的关系、CME地磁效应的日面东西不对称性以及磁云与高速流的作用等问题进行了讨论.     

磁云膨胀速度对无力场磁通量管模型拟合结果的影响

为了考察磁云膨胀速度对磁通量管模型拟合结果的影响,选取了1998-2003年中15次引起了较大地磁暴(Dstmin＜-50 nT)的典型磁云事件进行了拟合.与未考虑膨胀速度模型的拟合结果比较,膨胀速度的引入能较好地改善拟合结果,与观测数据的偏差最大能减小30%,并且拟合所得的膨胀速度基本符合统计规律.这个结果说明膨胀的磁通量管模型能更好地反映实际观测的磁云.同时,初步分析了考虑膨胀速度前后磁云各拟合参数的变化.     

武昌地区急始型磁暴期间电离层电子总含量的变化

利用１９８０年４月至１９９０年１２月共１３６次急始型磁暴资料统计研究了武昌地区ＴＥＣ的变化。结果表明，ＴＥＣ的暴时变化出现正相，相对变化值ΔＴＥＣ的暴时变化形态与中高纬地区一些台站所观测到的结果差别较大；如果磁暴急始出现在白天，则急始后３６小时，会出现ΔＴＥＣ的极大值，如果急始出现在夜间，则不会出现极大值，这一现象与太阳黑子数，季节无关。     

Effects of space weather on the ionosphere and LEO satellites’ orbital trajectory in equatorial,low and middle latitude

We study the effects of space weather on the ionosphere and low Earth orbit (LEO) satellites’ orbital trajectory in equatorial, low- and mid-latitude (EQL, LLT and MLT) regions during (and around) the notable storms of October/November, 2003. We briefly review space weather effects on the thermosphere and ionosphere to demonstrate that such effects are also latitude-dependent and well established. Following the review we simulate the trend in variation of satellite’s orbital radius (r), mean height (h) and orbit decay rate (ODR) during 15 October–14 November 2003 in EQL, LLT and MLT. Nominal atmospheric drag on LEO satellite is usually enhanced by space weather or solar-induced variations in thermospheric temperature and density profile. To separate nominal orbit decay from solar-induced accelerated orbit decay, we compute $r\text{,}h$ and ODR in three regimes viz. (i) excluding solar indices (or effect), where $r=r_0\text{,}h=h_0$ and $\mathit{ODR}={\mathit{ODR}}_0$ (ii) with mean value of solar indices for the interval, where $r=r_m\text{,}h=h_m$ and $\mathit{ODR}={\mathit{ODR}}_m$ and (iii) with actual daily values of solar indices for the interval ($r\text{,}h$ and ODR). For a typical LEO satellite at h?=?450?km, we show that the total decay in r during the period is about 4.20?km, 3.90?km and 3.20?km in EQL, LLT and MLT respectively; the respective nominal decay ($r_0$) is 0.40?km, 0.34?km and 0.22?km, while solar-induced orbital decay ($r_m$) is about 3.80?km, 3.55?km and 2.95?km. h also varied in like manner. The respective nominal ${\mathit{ODR}}_0$ is about 13.5?m/day, 11.2?m/day and 7.2?m/day, while solar-induced ${\mathit{ODR}}_m$ is about 124.3?m/day, 116.9?m/day and 97.3?m/day. We also show that severe geomagnetic storms can increase ODR by up to 117% (from daily mean value). However, the extent of space weather effects on LEO Satellite’s trajectory significantly depends on the ballistic co-efficient and orbit of the satellite, and phase of solar cycles, intensity and duration of driving (or influencing) solar event.     

1998年5月空间天气大事件的地磁场响应

地磁场与1998年5月空间大事件相对应的是5月1日至16日发生的大磁暴（k=8)。磁暴主相开始的几个小时伴随有丰富的Pc型地磁脉动，包括P c2,Pc3,Pc4等。在增暴的恢复相，甚至还有Pc5巨型脉动，在行星标磁场Bz由北向转向南向时，磁暴主相开始；南向分量达到最大值后大约2小时，地磁H分量达到最小值，恢复相开始，并且，这次磁暴与太阳风电场也存在一定的对应关系。     

The response of the ionosphere over Ilorin to some geomagnetic storms

The effects of some geomagnetic storms on the F2 layer peak parameters over Ilorin, Nigeria (Lat. 8:53°N, Long. 4.5°E, dip angle, −2.96°) have been investigated. Our results showed that the highest intensity of the noon bite-out occurred during the March equinox and lowest during the June Solstice on quiet days. Quiet day NmF2 disturbances which appeared as a pre-storm enhancement, but not related to the magnetic storm event that followed were observed at this station. These enhancements were attributed to the modification of the equatorial electric field as a result of injection of the Auroral electric field to the low and equatorial ionosphere. For disturbed conditions, the morphology of the NmF2 on quiet days is altered. Daytime and nighttime NmF2 and hmF2 enhancements were recorded at this station. Decreases in NmF2 were also observed during the recovery periods, most of which appeared during the post-noon period, except the storm event of May 28–29. On the average, enhancements in NmF2 (i.e. Positive phases) are the prominent features of this station. Observations from this study also indicate that Dst, Ap and Kp which have been the most widely used indices in academic research in describing the behavior of geomagnetic storms, are not sufficient for storm time analysis in the equatorial and low latitude ionosphere.