珠穆朗玛峰北坡山谷太阳辐射和大气的特征与分析

2006年5月27日～6月30日HEST2006大气科学实验对珠峰北坡山谷的辐射(总辐射、净辐射)和温、湿度、风等进行了综合观测.沿珠峰北坡山谷布设了3个观测站,3个测站的辐射、温度、风都表现出明显的日变化规律,它们在08:00或09:00(地方时,下同)达到极大值.3个测站总辐射和净辐射的日变化都七匕较一致.从日变化最大值出现的时间来看,各站的辐射通量早于气温,气温早于风速.3个测站中任意2站之间辐射(总辐射、净辐射)最大值之比与温度和风速最大值之比均比较接近.因辐射状况、地形结构、大气温度等不同,远离珠峰区域的风一天之内多次改变风向,靠近珠峰区域则24h都为南风.珠峰北坡山谷不同区域风向风速变化存在明显时差,南风强于北风,且持续时间长.研究表明,辐射能量对于珠峰北坡大气运动具有重要的驱动作用,是控制和改变其大气运动方式最基本、最重要的因子.净辐射在不同区域风向转变或风速变化过程中起着决定性的作用.     

太阳常数的变化与太阳软x射线辐射流量及低频天波时延的关系

本文对1982年在陕西临潼接收的美国罗兰-C西北大平洋链Y台发射的100kHz低频一跳天波时延的实测资料及SMS－GOES测量的太阳1～8A软x射线的每日辐射流量与SMM／ACRIMI测量的太阳常数之间的关系进行了分析。结果表明：太阳1～8A软x射线辐射流量与太阳常数之间存在较强的负相关;低频一跳天波时延与太阳常数之间存在着较强的正相关。并对此进行了讨论。     

1997年昆明日偏食射电快速过程的观测

介绍了１９９７年３月９日昆明日偏食过程中云南天文台四波段射电高时间分辨率同步观测结果,通过掩食和露放黑子前后射电快速起伏率的变化现象,推测日冕缓变源存在电子加速过程,它可能对射电快速起伏率的增强有贡献。     

应用遥感图像提取煤层自燃信息时必须考虑的几个影响因素

煤层自燃是中国北方煤田中普遍存在的灾害现象,它不但烧掉了大量的煤炭资源,而且还污染了环境。实践证明,利用遥感影像判别火区位置、圈定火区范围和对火区进行动态监测,及时为灭火工程提供信息,是一项经济和社会意义很大的工作。由于受多种因素的制约,不同地区、不同波段、不同时相、不同空间分辨率的遥感图像,其影像特征（含与煤层自燃有关的热异常影像特征）都有较大的差异,因而从图像上分析和提取地物的热红外辐射特征时,需要考虑遥感图像类型、成像时间、地形条件、气象条件和岩性特征等因素的影响。本文着重讨论了地表辐射温度与上述各项因素之间的关系。     

Interplanetary scintillation observations of interaction regions in the solar wind

Co-rotating interaction regions (CIRs) between fast and slow streams of plasma are a prominent feature of the solar wind. Measurements of interplanetary scintillation (IPS) using the three widely separated antennas of the EISCAT facility have been used to detect the compression regions at the leading edges of interaction regions and to determine the location and velocity of the structure. Observations show that interaction regions have developed as close to the Sun as 25–30 solar radii, a result supported by theoretical modelling which shows that the conditions needed for CIRs to develop exist inside 30 solar radii.     

天再旦与日食

《汲冢纪年》有“懿王元年天再旦于郑”的记载。今日学者大多认为是日食。果真如此,对研究地球自转的长期变化会有重要作用。本文考查了在懿王可能所处的９６６～８９５ＢＣ,７２年中,有可能引起“天再旦”的日食,并从纪时日食的角度对地球自转不均匀引起的世界时改正数ΔＴ数值作了分析和讨论。     

Measurements of the direction of the solar wind using interplanetary scintillation

EISCAT observations of the interplanetary scintillation of a single source were made over an extended period of time, during which the orientation of the baselines between the two observing sites changed significantly. Assuming that maximum correlation between the scintillations observed at the two sites occurs when the projected baseline is parallel to the direction of plasma flow, this technique can be used to make a unique determination of the direction of the solar wind. In the past it has usually been assumed that the plasma flow is radial, but measurements of eleven sources using this technique have indicated conclusively that in at least six cases observed at mid or high heliocentric latitude there is a significant non-radial component directed in four cases towards the heliocentric equator and in two cases towards the pole.     

Signatures of interplanetary transients behind shocks and their associated near-surface solar activity

Interplanetary transients with particular signatures different from the normal solar wind have been observed behind interplanetary shocks and also without shocks. In this paper we have selected four well-known transient interplanetary signatures, namely: magnetic clouds, helium enhancements and bidirectional electron and ion fluxes, found in the solar wind behind shocks, and undertaken a correlative study between them and the corresponding solar observations. We found that although commonly different signatures appear in a single interplanetary transient event, they are not necessarily simultaneous, that is, they may belong to different plasma regions within the ejecta, which suggests that they may be generated by complex processes involving the ejection of plasma from different solar regions. We also found that more than 90% of these signatures correspond to cases when an H flare and the eruption of a filament occurred near solar central meridian between 1 and 4 days before the observation of the disturbance at 1 AU, the highest association being with flares taking place between 2 and 3 days before. The majority of the H flares were also accompanied by soft X-ray events. We also studied the longitudinal distribution of the associated solar events and found that between 80% and 90% of the interplanetary ejecta were associated with solar events within a longitudinal band of ±30° from the solar central meridian. An east-west asymmetry in the associated solar events seems to exist for some of the signatures. We also look for coronal holes adjacent to the site of the explosive event and find that they were present almost in every case.     

On a time-symmetric Hermite integrator for planetary N-body simulation

We describe a P(EC) ⁿ Hermite scheme for planetary N -body simulation. The fourth-order implicit Hermite scheme is a time-symmetric integrator that has no secular energy error for the integration of periodic orbits with time-symmetric time-steps. In general N -body problems, however, this advantage is of little practical significance, since it is difficult to achieve time-symmetry with individual variable time-steps. However, we can easily enjoy the benefit of the time-symmetric Hermite integrator in planetary N -body systems, where all bodies spend most of the time on nearly circular orbits. These orbits are integrated with almost constant time-steps even if we adopt the individual time-step scheme. The P(EC) ⁿ Hermite scheme and almost constant time-steps reduce the integration error greatly. For example, the energy error of the P(EC)² Hermite scheme is two orders of magnitude smaller than that of the standard PEC Hermite scheme in the case of an N  = 100,  m  = 10²⁵ g planetesimal system with the rms eccentricity 〈 e ²〉^1/2 ≲0.03.     

A numerical algorithm for dissipative Keplerian particle discs

We present a numerical algorithm designed to study the evolution of a distribution of solid particles orbiting around the Sun that could be applied to similar systems in which f _c ≤ Ω/2π, where f _c is the frequency of collisions, and Ω is the orbital angular speed. A number of sample particles are used to represent the whole system. Binary collisions are treated in a novel way using a Monte Carlo method that works as follows. Orbits are locally sampled to compute the velocity dispersion. Then the velocity vectors of the sample particles are modified according to random collisions with virtual particles which have velocities taken from a normal distribution computed using the previously found local velocity dispersion. The energy and momentum taken up by the virtual particles are redistributed among the neighbours of the sample particle undergoing the collision, so that conservation laws are satisfied. Simulations using this model give an estimation of the final distribution of inclinations and the associated evolutionary time-scale.