100—200km热层大气光电离率及电子密度剖面对太阳活动的响应

本文利用新的太阳EUV辐射资料、中性大气结构模式及大气成分的吸收及电离特性,计算了100—200km大气的光电离率随高度、太阳天顶角及太阳活动的变化,求得了E-F1谷的变化特征;利用完整的光化模式求得了电子密度随太阳天顶角的变化及对太阳活动的响应,并与IRI模式作了比较.结果表明,1.太阳活动指数与光电离率间的相关关系一般为正,但在一定的高度范围内,或在天顶角大于临界值Xcr=60°时,两者之间可出现负相关;2.太阳活动明显地影响E-F1谷高与谷厚,当天顶角不变时,谷高与谷厚均与太阳活动成正相关;3.本模式与IRI间的偏差因子明显随高度及太阳天顶角而变化.     

The DynaMICCS perspective

The DynaMICCS mission is designed to probe and understand the dynamics of crucial regions of the Sun that determine solar variability, including the previously unexplored inner core, the radiative/convective zone interface layers, the photosphere/chromosphere layers and the low corona. The mission delivers data and knowledge that no other known mission provides for understanding space weather and space climate and for advancing stellar physics (internal dynamics) and fundamental physics (neutrino properties, atomic physics, gravitational moments...). The science objectives are achieved using Doppler and magnetic measurements of the solar surface, helioseismic and coronographic measurements, solar irradiance at different wavelengths and in-situ measurements of plasma/energetic particles/magnetic fields. The DynaMICCS payload uses an original concept studied by Thalès Alenia Space in the framework of the CNES call for formation flying missions: an external occultation of the solar light is obtained by putting an occulter spacecraft 150 m (or more) in front of a second spacecraft. The occulter spacecraft, a LEO platform of the mini sat class, e.g. PROTEUS, type carries the helioseismic and irradiance instruments and the formation flying technologies. The latter spacecraft of the same type carries a visible and infrared coronagraph for a unique observation of the solar corona and instrumentation for the study of the solar wind and imagers. This mission must guarantee long (one 11-year solar cycle) and continuous observations (duty cycle > 94%) of signals that can be very weak (the gravity mode detection supposes the measurement of velocity smaller than 1 mm/s). This assumes no interruption in observation and very stable thermal conditions. The preferred orbit therefore is the L1 orbit, which fits these requirements very well and is also an attractive environment for the spacecraft due to its low radiation and low perturbation (solar pressure) environment. This mission is secured by instrumental R and D activities during the present and coming years. Some prototypes of different instruments are already built (GOLFNG, SDM) and the performances will be checked before launch on the ground or in space through planned missions of CNES and PROBA ESA missions (PICARD, LYRA, maybe ASPIICS).     

太阳活动预报中的模糊识别综合指数

在太阳活动预报中,预报因子的选取和处理对预报效果影响甚大。本文在云台原有的平均综合指数基础上,运用模糊识别方法,给出了一种模糊识别综合指数,它能更好地表征太阳日面活动区的活动特征。这种方法简单、方便,较充分地利用了预报因子中所含有的有用信息,从而使识别预报率有所提高。     

黑山峡大柳树坝址区断裂构造格局与F201断层活动性研究

黑山峡大柳树坝址区主干活动断裂F201的规模及活动强度是影响坝址稳定的主要因素,通过分析坝址区基本断裂构造格局,阐述了F201断层活动对坝区内另一条主干断层F7(8)以及位于坝址上的数条次级断层的控制牵动效应.通过对F201现代活动规模及强度的讨论,认为该断层现代活动规模大于60 km以上.探槽显示,晚第四纪以来至少发生过7次震级古地震事件.其中大于7级的至少有4次.     

VLA and MERLIN observations of RZ Cassiopeiae

We present radio interferometric observations of the Algol-type binary system RZ Cassiopeiae made with the VLA and MERLIN arrays at 6 cm over an incomplete orbital cycle of the system (1.195 d). We detected RZ Cas with both instruments. The images were unresolved in both cases, with angular extents comparable to the synthesized beams. The peak flux density in the VLA image was 1.14 mJy beam⁻¹ and in the MERLIN image it was 0.93 mJy beam⁻¹. The derived brightness temperatures are  4.02 × 10⁸  and  4.35 × 10⁸ K  and the effective electron energies are 0.347 and 0.346 MeV for the MERLIN and VLA data respectively. The radio light curve shows an interesting modulation centred close to the primary eclipse which seems to correlate with ASCA SIS observations of the system. The results can be interpreted as an emitting region on the outer hemisphere of the cool component aligned along the centroid axis of the binary system.     

Chromospheric Ca II H and K emission among subdwarfs

Echelle spectra have been obtained of the Ca  II H and K lines for a sample of metal-poor subdwarf stars as well as for a number of nearby Population I dwarfs selected from among those included in the Mount Wilson HK survey. The main conclusion of this paper is that Ca  II H- and K-line emission does occur among subdwarfs. It is particularly notable among those subdwarfs with colours of B − V ≥0.75; all such stars observed exhibit chromospheric emission, although emission is observed among some subdwarfs bluer than this colour. The Ca  II K emission profile in most subdwarfs exhibits an asymmetry of V / R >1, similar to that seen in the integrated light of the solar disc. Two quantitative indicators of the contrast between the peaks in the emission profile and the neighbouring photospheric line profile are introduced. Measurements of these indicators show that the level of Ca  II emission among the subdwarfs is similar to that among low-activity Population I dwarfs.     

花椒品种抗冻性比较研究

秦安1号、油椒和大红袍是甘肃省花椒主产区的主要栽培品种。对其一年生休眠枝在不同低温（0～-40℃）处理不同时间（24～72 h）,通过测定相对电导率、超氧物岐化酶（SOD）活性和丙二醛（MDA）含量,对花椒品种休眠枝的抗冻性进行了比较研究。结果表明,各品种休眠枝的相对电导率和MDA含量从低到高均依次为:秦安1号＜油椒＜大红袍,品种间差异性均达到显著水平（P＜0.05）;SOD活性秦安1号略高于油椒,二者差异性虽未达到显著水平,但均显著高于大红袍（P＜0.01）;相同温度下,3品种休眠枝的相对电导率、MDA含量均随低温持续时间的延长而升高,大红袍休眠枝上升更加明显。SOD活性均随处理时间的延长而降低。引起各花椒品种休眠枝低温伤害的临界温度范围为-15～-20℃。从相对电导率、MDA含量和SOD活性的变化综合分析,供试的3个花椒品种中,秦安1号的抗冻性最强,油椒次之,大红袍抗冻性最弱。     

全球变化与浙江洪水大势

根据历史和实测资料分析,对于全球变化下浙江近期洪水的运作大势,可得如下几点认识：（１）在未来的十几年之内,浙江省将处在枯水年占优势的阶段,但全球变化将使浙江洪水的时空变化更为剧烈,使沿海地区的洪水灾害更为严重。（２）由于浙江省的大中洪水一般都集中在太阳黑子活动的峰谷年前后,而近期的２００４年和２００９年分别是黑子活动第２３周期的峰年和谷年,因此这两年前后必须予以足够的重视。（３）浙江洪水对厄尔尼诺现象具有较好的响应,因此厄尔尼诺同年或次年也必须引起足够的重视。（４）根据浙江历史上的台风重灾年资料,利用灰色灾变预测分析,可得浙江未来第一、第二和第三个台风重灾年分别为２００１、２００４和２００８年,其中后两个台风重灾年与太阳黑子活动第２３周期的峰年和谷年是大致吻合的。（５）植被破坏、河道设障等人类活动会产生一定的增灾效应,从而使浙江未来的洪水灾害更为严重。     

一种可能的地震成因模型

提出了一种地震成因模型。认为不仅水库地震、矿震等是被人类工程活动诱发的，其它地震也很可能有诱发因素起作用。这种作用不仅仅是触发了地震，地震的孕育很可能也与其有关。诱发因素包括人类工程活动、地外天体的特殊位置、地球自转角速度的变化、气象异常等。这些因素对地壳产生了附加垂直力，后者引起局部地层弯曲，进而导致应力集中、构造应力作用方式的改变乃至地震发生。     

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