Magnetic fields of sunspots based on combined optical and radio observations

In the present paper we present the results of measurement of magnetic fields in some sunspots at different heights in the solar atmosphere, based on simultaneous optical and radio measurements. The optical measurements were made by traditional photographic spectral observations of Zeeman splitting in a number of spectral lines originating at different heights in the solar photosphere and chromosphere. Radio observations of the spectra and polarization of the sunspot - associated sources were made in the wavelength range of 2–4 cm using large reflector-type radio telescope RATAN-600. The magnetic field penetrating the hot regions of the solar atmosphere were found from the shortest wavelength of generation of thermal cyclotron emission (presumably in the third harmonic of electron gyrofrequency). For all the eight cases under consideration we have found that magnetic field first drops with height, increases from the photosphere to lower chromosphere, and then decreases again as we proceed to higher chromosphere and chromosphere-corona transition region. Radio measurements were found to be well correlated with optical measurements of magnetic fields for the same sunspot. An alternative interpretation implies that different lines used for magnetic field measurements refer to different locations on the solar surface. If this is the case, then the inversion in vertical gradients of magnetic fields may not exist above the sunspots. Possible sources of systematic and random errors are also discussed.     

Thermoluminescence, electron paramagnetic resonance and optical absorption in natural and synthetic rhodonite crystals

Thermoluminescence, electron paramagnetic resonance and optical absorption properties of rhodonite, a natural silicate mineral, have been investigated and compared to those of synthetic crystal, pure and doped. The TL peaks grow linearly for radiation dose up to 4 kGy, and then saturate. In all the synthetic samples, 140 and 340°C TL peaks are observed; the difference occurs in their relative intensities, but only 340°C peak grows strongly for high doses. Al₂O₃ and Al₂O₃ + CaO-doped synthetic samples presented several decades intenser TL compared to that of synthetic samples doped with other impurities. A heating rate of 4°C/s has been used in all the TL readings. The EPR spectrum of natural rhodonite mineral has only one huge signal around g = 2.0 with width extending from 1,000 to 6,000 G. This is due to Mn dipolar interaction, a fact proved by numerical calculation based on Van Vleck dipolar broadening expression. The optical absorption spectrum is rich in absorption bands in near-UV, visible and near-IR intervals. Several bands in the region from 540 to 340 nm are interpreted as being due to Mn³⁺ in distorted octahedral environment. A broad and intense band around 1,040 nm is due to Fe²⁺. It decays under heating up to 900°C. At this temperature it is reduced by 80% of its original intensity. The pink, natural rhodonite, heated in air starts becoming black at approximately 600°C.     

利用NOAA卫星资料估算陆地沙尘量的方法

提出一种利用NOAA卫星可见光通道估算北方干旱陆地上空沙尘含量的方法。该方法考虑到在短时间内某一固定区域的地面反射率变化较小,因此可以利用沙尘暴发生和晴空2个不同时刻卫星测量到的这一像素区的辐射值来消除地面反射率的影响,估算陆地上空沙尘暴的光学厚度。在2002年4月6日左右沙尘暴发生期间,利用该方法计算的沙尘光学厚度与载沙量的结果和同步观测的TSP值与地面气象数据在趋势与分布上是一致的。     

Considering combined or separated roughness and vegetation effects in soil moisture retrievals

For more than six years, the Soil Moisture and Ocean Salinity (SMOS) mission has provided multi angular and full-polarization brightness temperature (TB) measurements at L-band. Geophysical products such as soil moisture (SM) and vegetation optical depth at nadir (τ_nad) are retrieved by an operational algorithm using TB observations at different angles of incidence and polarizations. However, the quality of the retrievals depends on several surface effects, such as vegetation, soil roughness and texture, etc. In the microwave forward emission model used in the retrievals (L-band Microwave Emission Model, L-MEB), soil roughness is modelled with a semi-empirical equation using four main parameters (Q_r, H_r, N_rp, with p = H or V polarizations). At present, these parameters are calibrated with data provided by airborne studies and in situ measurements made at a local scale that is not necessarily representative of the large SMOS footprints (43 km on average) at global scale. In this study, we evaluate the impact of the calibrated values of N_rp and H_r on the SM and τ_nad retrievals based on SMOS TB measurements (SMOS Level 3 product) over the Soil Climate Analysis Network (SCAN) network located in North America over five years (2011–2015). In this study, Q_r was set equal to zero and we assumed that N_rH = N_rV. The retrievals were performed by varying N_rp from −1 to 2 by steps of 1 and H_r from 0 to 0.6 by steps of 0.1. At satellite scale, the results show that combining vegetation and roughness effects in a single parameter provides the best results in terms of soil moisture retrievals, as evaluated against the in situ SM data. Even though our retrieval approach was very simplified, as we did not account for pixel heterogeneity, the accuracy we obtained in the SM retrievals was almost systematically better than those of the Level 3 product. Improved results were also obtained in terms of optical depth retrievals. These new results may have key consequences in terms of calibration of roughness effects within the algorithms of the SMOS (ESA) and the SMAP (NASA) space missions.     

查找表方法确定气溶胶类型

针对传统气溶胶类型确定方法的局限性以及当前气溶胶类型确定存在的困难,提出一种使用多波段气溶胶光学厚度数据确定气溶胶类型的方法。基于大气颗粒物的散射与吸收特性分析,通过构建查找表的方法实现气溶胶类型的确定。该方法利用Mie散射理论通过正向模拟不同类型气溶胶粒子数量与多波段光学厚度之间的关系来构建查找表,基于该查找表,使用440 nm、670 nm、870 nm及1020 nm 4个波段的气溶胶光学厚度确定气溶胶类型。使用模拟的多波段气溶胶光学厚度数据开展了气溶胶类型的确定实验,分析了不同波段气溶胶光学厚度误差对气溶胶类型确定结果的影响。结果表明,该方法可根据4个波段的气溶胶光学厚度以较高的精度确定出沙尘性、水溶性和煤烟3种气溶胶粒子的数量,从而确定气溶胶类型。     

从空间探测闪电的综述

从空间探测闪电 30多年的历史看 ,一些卫星闪电遥感仪器已提供了许多极有价值的资料 ,例如 ,闪电全球范围内发生的频率 ,其随纬度和季节的变化以及日变化 ,超级闪电的发生等等。这些资料在雷电灾害预警预防、强对流天气监测、某些军事目标的识别等业务和科研工作中得到了应用。本文是关于空间探测闪电的一个综述 ,主要介绍过去 35a一些星载闪电光学探测器 ,并给出由这些仪器观测资料分析所得到的一些重要结果。最后 ,对发展中国星载闪电探测器提出几点建议。     

Plateau de bure observations of IRC+10216: high sensitivity maps of SiC2, SiS,and CS

We have obtained high angular resolution ( 3), and high sensitivity maps of IRC+10216. SiC₂ is found both in a spherical shell and in the very central region, indicating it is formed both in the inner envelope close to the star, and in the outer shell. The molecules SiS and CS are mostly found in the inner parts of the envelope, but are still detectable in the outer region (r 15) where the products of photochemistry are found. The maps show that IRC+10216 has a very clumpy envelope, with strong departures from spherical symmetry; an axis oriented NS-SW (P.A. 20°) can be seen in all maps. The radial brightness distribution of CS has secondary maxima, at the radius where the SiC₂ shell has its peak emission. A preliminary map shows CN in the same shell, but also in a still larger outer shell. Time variations in the mass loss rate, could be invoked to explain the multiple shell structure of this envelope.     

机载光阵探头探测期间云粒子的破碎

机载光阵探头探测时,云粒子(液态和固态)进入二维光阵探头的采样区前,会因与探头探测臂发生机械碰撞,或者与探头外壳产生的湍流和风切变相互作用而破碎。破碎程度与粒子类型、大小、粒子密度、探头入口设计以及飞行空速等有关。利用2008年7~9月探测飞机(Y-12)在山西省太原地区的航测资料并对飞机采样期间的云粒子破碎现象进行介绍和分析,分析结果表明,粒子到达时间间隔分布具有双模态特征:长时间模态是粒子空间分布的真实结构,短时间模态则是云粒子破碎的结果。提出用粒子到达时间间隔阈值作为粒子破碎的判定标准,给出适用于2008年太原地区航测资料的粒子破碎识别阈值,其中适合于探头云粒子成像仪(CIP)的阈值是2×10-5 s,而探头降水粒子成像仪(PIP)的阈值是1×10-4 s。所提的阈值对于以Y-12为机载探测平台,以CIP和PIP探头为探测仪器所获取的其它航次云微物理图像资料的粒子破碎处理也是有一定的参考使用价值。     

光学后向散射法在海洋现场探测无机悬浮颗粒物质的应用研究

本文论述了使用作者于１９８８年研制成功的国内第一台拖曳荧光计系统，通过改换荧光测量滤片为中性滤光片。