利用浮标站观测资料分析台风“贝碧嘉”过境时风浪变化特征

利用北部湾海域一个大型气象浮标站获取的台风"贝碧嘉"过程实测数据,分析了该台风过境时风浪变化特征。分析结果表明:台风的风速时程变化曲线呈"M"形双峰分布,台风眼壁区风速最大,前眼壁区风速大于后眼壁区,前眼壁区和后眼壁区最大风速分别为22.6m/s和20.8m/s;台风眼区气压和风速最小,波高和波周期最大,其中眼区最大风速为2.7m/s,最大波高为5.4m,最大波周期为5.5s;波高最大值出现时间滞后风速最大值40min;台风眼区以外的波高与风速正相关;在台风从浮标站南侧经过期间,风向和波向均沿着顺时针方向旋转,其中风向和波向10min最大旋转角度分别为50°和150°;风向与波向不在同一个方向,两者之间的夹角平均为171°。     

全球升温1.5℃和2.0℃情景下淮河上游干流径流量研究

基于ISI-MIP（The Inter-Sectoral Impact Model Inter-comparison Project）推荐使用的5个全球气候模式数据(HadGEM2-ES,GFDL-ESM2M,MIROC-ESM-CHEM,Nor-ESM1-M,IPSL-CM5ALR),驱动SWIM（Soil and Water Integrated Model）水文模型,研究全球升温1.5℃和2.0℃情景下淮河上游干流径流量变化,得出结论：(1)淮河上游干流径流量年际变化在2种升温情景下均呈先减小后增加趋势。全球升温1.5℃时年径流量较基准期(1986—2005年)增长9.5%,而升温2.0℃情景下涨幅更明显,高达17%。(2) 4个季节径流量在2种升温情景下较基准期均有增长,其中春季涨幅最明显,达24.4%,夏、秋、冬季涨幅分别为7.1%、16.1%、13.5%。全球升温2.0℃时淮河上游干流径流量在4个季节较基准期增长率均大于全球升温1.5℃时。(3)不同气候模式输出日径流量最大值相差较大而平均值相差较小。未来2种升温情景日径流量超过王家坝闸设计流量的日次较基准期均有增加,尤其升温2.0℃情景较基准期增多22次,较升温1.5℃情景多5.8次,表明未来升温2.0℃情景下淮河上游出现极端径流事件的可能性进一步增大。     

Behaviour of the polarization at dm-m wavelengths during the evolution of five two-ribbon flares

The general behaviour of the circular polarization at dm-m wavelengths during the evolution of five two-ribbon flares is investigated. The changes of polarization, if present, occurred 10 to 20 min after the impulsive phases. Increases of the radio and X-ray fluxes occurred at the moments when the H ribbons started to extend over spot umbrae.Proceedings of the Workshop on Radio Continua during Solar Flares, held at Duino (Trieste). Italy, 27–31 May, 1985     

Reconnection driven by an erupting filament in the May 14, 1981 flare

We present observations of the flare of May 14, 1981, which can be classified as a three-ribbon flare. After a detailed analysis in metric, decimetric, microwave, optical, and X-ray ranges we propose that the event was caused by a reconnection process driven by erupting filament. The energy was liberated in the current sheet above the filament in the region between the erupting flux and the overlying field. It is shown that plasma microinstabilities develop as the plasma enters the current sheet. The observations indicate that during the precursor phase a certain low-frequency turbulence, such as ion-accoustic turbulence had to be present.The reconnection rate was growing due to the increasing tension of the stretched overlying field. It is shown that the reconnection proceeded in the Sonnerup-Petschek regime during the precursor, and changed to the pile-up regime in the fast reconnection phase, when the maximal lateral expansion (50 km s^–1) of the H ribbons was observed. The proposed process of reconnection driven by an erupting filament can be applied to three- and four-ribbon flares.     

Kinematics and evolution of twist in the eruptive prominence of August 18, 1980

The prominence which erupted at the SE limb on August 18, 1980 is one of the best observed disparition brusque events: high-resolution monochromatic ground-based observations in the H line were supplemented by the SMM and Solwind satellite coronographic observations; the radio wavelength range was well covered by single-frequency and spectral observations, and the prominence magnetic fields were measured two days before the eruption.The prominence showed a helical-like internal structure from the pre-eruptive phase, up to the late phases of eruption. The pitch angles of the helical-like threads were measured at several positions 31 along the prominence axis, and the evolution of twist was followed during the eruption. These measurements provide an estimate of the parameters which are directly comparable with theoretical models. The pitch angles of the helical threads decreased during the eruption. A redistribution of twist along the prominence axis could not be detected within the accuracy of measurements, although there are indications that the twist was partly transformed into an external kink-type screw of the prominence axis. The value of the total twist did not change during the eruption within the accuracy of the measurements.The kinematics of the process was followed, and accompanying events in the radio-range and soft X-rays are listed. Measurements of the magnetic field vector in the prominence are reviewed briefly. The observations were compared with predictions of cylindrical models, considering the forces acting at the prominence summit. Observational implications and constraints are discussed, and the decrease of the axial electric current and the mass loss are inferred.     

Solar differential rotation determined by polar crown filaments

The rotation rates obtained by tracing 124 polar crown filaments are presented in comparison with previous results. Higher filament rotation rate in polar regions was detected and discussed in terms of the various phenomena such as: the projection effect due to the height of measured tracers, the connection of polar filaments with the magnetic field patterns which show an increase of the rotation rate at high latitudes, rigid rotation of polar filaments which form pivot points, and eventual change of the differential rotation law during the cycle. However, when the height correction for an average height of 1% of the solar radius is applied, the filament rotation rate in polar regions decreases. Then the rotation law becomes: () = 14.45 – 0.11 sin² – 3.69 sin⁴ (° day^–1, sidereal).     

The role of the magnetic field intensity and geometry in the type III burst generation

We study the association of type III bursts related to H flares in different magnetic environments in the period 1970–1981. Special attention is paid to flares which partly cover a major spot umbra (Z-flares). In particular we consider the location of the spots in the active regions and the magnetic field intensities of spots covered by a ribbon. The association rate with type III bursts decreases to 17% when the flare is located inside the bipolar pattern of a large active region, compared with an association rate of 54% when the flare is situated outside it. The association rate increases with the magnetic field intensity of the spot covered by H emission; this is most clearly revealed for the flares occurring outside the bipolar pattern of active regions. Ninety-three percent of the flare-associated type III burst were accompanied by 10 cm radio bursts. For the most general case in which a flare is developing anywhere in an active region, the association with type III bursts generation increases with the increasing magnetic field intensity of the main spot of the group.     

南海ODP1148站深海相渐新统硅质成岩作用

南海ODP1148站分析结果显示，井深475-600m的硅质化石主要表现为蛋白石-CT。随着深度增加，硅质化石破壳率增大，蛋白石-CT的X射线衍射峰强度减弱，自生石英的衍射峰则相应增强，反应了蛋白石-CT向石英的转变，井深620m附近，硅质化石完全溶解，蛋白石-CT衍射峰消失，蛋白石-CT全部转变为石英，样品取心率从470m处的近100%降到485m处的8%，可能是硅质成岩作用，尤其是蛋白石-A向蛋白石-CT的转变影响所致，而取心率的降低，则是此井未能观察到蛋白石-A/蛋白石-CT转变界线的部分原因。