Evidence for solar neutrino flux variability and its implications

Although KamLAND apparently rules out resonant-spin-flavor-precession (RSFP) as an explanation of the solar neutrino deficit, the solar neutrino fluxes in the Cl and Ga experiments appear to vary with solar rotation. Added to this evidence, summarized here, a power spectrum analysis of the Super-Kamiokande data reveals significant variation in the flux matching a dominant rotation rate observed in the solar magnetic field in the same time period. Three frequency peaks, all related to this rotation rate, can be explained quantitatively. A Super-Kamiokande paper reported no time variation of the flux, but showed the same peaks, there interpreted as statistically insignificant, due to an inappropriate analysis. This modulation is small (7%) in the Super-Kamiokande energy region (and below the sensitivity of the Super-Kamiokande analysis) and is consistent with RSFP as a subdominant neutrino process in the convection zone. The data display effects that correspond to solar-cycle changes in the magnetic field, typical of the convection zone. This subdominant process requires new physics: a large neutrino transition magnetic moment and a light sterile neutrino, since an effect of this amplitude occurring in the convection zone cannot be achieved with the three known neutrinos. It does, however, resolve current problems in providing fits to all experimental estimates of the mean neutrino flux, and is compatible with the extensive evidence for solar neutrino flux variability.     

P-T大气稳定度日夜分界限取值的研究

本文用两种不同日夜分界限统计了成都、重庆的P-T大气稳定度频率。结果表明,两种分界统计大气稳定度频率,不稳定类完全相同;以h=0分界比以h=k_1分界中性频率增加,稳定频率减少,两者频率差值大小与地理位置、气候和天气特征有关;这与理论分析完全符合。通过对比指出,h=0分界的应用有局限性。同时,通过计算表明,实际工作中,太阳赤纬σ每十日取一概略值已足够精确了。     

Fourier parameters and moments of polarization profiles of magnetically active lines. Fourier vector magnetograph

A new method is proposed to determine all components of the solar magnetic fields using the cumulants of the profile of a magnetic sensitive line. The method is based on polarization measurements in a number of points of the line profile and subsequent calculation of the amplitudes and phases of its two first Fourier-harmonics.     

太阳耀斑的光球磁场和色球速度场观测

太阳磁场望远镜安装了CCD图象接收处理系统后,得到许多精细结构的两维、实时磁场、速度场图。本文对其中观测的两群黑子,做耀斑磁场、速度场分析。在此基础上指出,异极性磁区相互渗透是普遍存在的,耀斑亮核均发生在异极性磁区相互挤压的前锋。这就为挤压无力场耀斑模式提供了有力的证据。同时发现,在耀斑发生的区域,流场的方向是向下的。     

IPS observations at stelab for the fruitful coming decade

We have been carrying out solar wind measurements using the interplanetary scintillation (IPS) method. Our IPS observation system is operated at a frequency of 327MHz and consists of four stations located at Toyokawa, Fuji, Sugadaira and Kiso. The present system, however, has insufficient sensitivity to measure enough IPS sources for observing the solar wind with adequate spatial and temporal resolution. Therefore we have been excuting the upgrade project since 1994 in order to observe a larger number of compact radio sources. The Fuji system has been improved successfully and has achieved sensitivity by a factor over five compared with the previous system. The upgrade project is now in progress for the Toyokawa and Sugadaira station.     

The Study of Kuiper Belt Objects With ESO and ISO

Amajor objective of the Infrared Space Observatory (ISO) is the determination of the sized and albedoes of several objects in the "Kuiper disc".The method by which this will be achieved is described.It is shown that the unknown shapes and surface thermal properties proviede additional complications to the interpretation of ISO data.The requirement for ground-based measurements of the visual light curves of these objects is demonstrated and the implications of the results of the ISO observ Vations is discussed.     

太阳高层大气物质交换的热机效应——色球-日冕过渡区模型

我们认为存在于太阳高层大气中的一种稳定的物质交换,可以起到冷却日冕和加热色球一日冕过渡区的热机作用。还考虑到来自日冕的热传导和过渡区的辐射损失,计算了太阳过渡区的温度、密度和速度分布。并对物质流通量及速度边值与太阳过渡区厚度之间的关系作了讨论。     

基于盐湖资源的硝酸熔盐储能材料性能研究

太阳能光热发电是可再生能源发展的主要方向。作为太阳能光热发电的核心技术,熔融盐以热容量大、粘度低、蒸汽压低、使用温度范围宽等诸多独特的性能优势,成为光热发电储能的首选。相比之下,硝酸熔盐具有优良的传热和流体流动等特性,使其在光热储热系统中的性能优势较为突出。我国盐湖地区具备太阳能光热发电的发展空间和优势,丰富的无机盐资源可以降低相关相变储能材料的生产成本,有利于推进太阳能的规模化发展、能源结构的调整优化。据此,立足于盐湖资源的开发利用,以硝酸盐系列传热蓄热介质的工业应用为背景,针对产业化的二元硝酸盐熔盐做了更深入的系统研究;在此基础上,通过添加硝酸镁,制备了低熔点的三元熔盐储能材料;并将碳纳米管引入到硝酸盐体系,进一步提升了其导热性能。这不仅为硝酸熔盐储热材料的制备提供了理论基础,也为其在光热发电的应用打开了更多的可能性。     

The significance of meteorite density and porosity

Non-destructive, non-contaminating, and relatively simple procedures can be used to measure the bulk density, grain density, and porosity of meteorites. Most stony meteorites show a relatively narrow range of densities, but differences within this range can be useful indicators of the abundance and oxidation state of iron and the presence or absence of volatiles. Typically, ordinary chondrites have a porosity of just under 10%, while most carbonaceous chondrites (with notable exceptions) are more than 20% porous. Such measurements provide important clues to the nature of the physical processes that formed and evolved both the meteorites themselves and their parent bodies. When compared with the densities of small solar system bodies, one can deduce the nature of asteroid and comet interiors, which in turn reflect the accretional and collisional environment of the early solar system.