冕流电流片的白光和紫外观测研究

日冕电流片是日冕磁重联发生的主要区域, 这一过程将磁能转化为等离子体的热能和动能. 通过选取大角度光谱日冕仪(Large Angle and Spectrometric Coronagraph, LASCO)的白光与远紫外日冕成像光谱仪(Ultraviolet Coronagraph Spectrometer, UVCS)的紫外观测, 研究了2003年1月3日观测到的冕流电流片. LASCO C2白光数据显示电流片中的等离子体团在视场中可从60km·s^-1加速至340km·s^-1, 加速度为 60m·s^-2; 假设视向深度为0.3--1.5R_⊙, 得到所研究电流片在UVCS狭缝高度处的平均电子数密度约为(1.52--7.60)×10⁷cm^-3. 对沿UVCS视场狭缝分布的[Fe xviii ] 974 ? A和Lyα谱线强度进行研究, 发现电流片处的[Fe xviii ]谱线强度比周围明显增大, 计算得到所研究时段内电流片的电子温度范围为(2.94–4.04)×10⁶K; 而在电流片处的Lyα谱线强度相对周围变化不大, 在电流片内部两侧强度比中心略高, 可能的主要原因是电流片内部中心处等离子体的运动速度要比两侧快, 这使得中心比两侧有更强的多普勒暗化作用. 以UVCS观测的Lyα和[Fe xviii ]谱线的辐射强度比和计算的电子温度为约束条件, 发现当狭缝电流片处等离子体运动速度约为237–254 km·s ^?1 时, 通过理论计算的Lyα和[Fe xviii ]谱线的辐射发射率比值和观测谱线强度比值相当. 在该速度范围内, 电流片内部Lyα辐射的碰撞项约为辐射项的42%–57%. 此事件中的冕流电流片比通常情形下的冕流电流片中等离子体温度更高、运动速度更大, 可能的原因在于其南侧爆发的两个日冕物质抛射促进了电流片中的磁重联过程, 更多的磁能释放用于等离子体的加热和加速. 所得研究结果可以为我国将要发射的先进天基太阳天文台(Advanced Space-based Solar Observatory, ASO-S)未来的资料处理提供重要参考.     

COMPARISON OF HTC METHOD AND UV/PERSULPHATE METHOD TO DETERMINE COLLOIDAL ORGANIC CARBON IN SEAWATER

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Continuous measurement of spectrophotometric absorbance in peatland streamwater in northern England: implications for understanding fluvial carbon fluxes

Bog systems tend to have a flashy hydrological regime with low baseflows and rapid and high storm peaks. Water derived from peatlands often contains significant amounts of organic humic and fulvic materials which form the largest fraction of the dissolved organic carbon component of the fluvial carbon flux. However, most estimates of dissolved organic carbon flux from peatlands are based on sampling that is infrequent and which may miss the periods of high flux during storm events. In order to better characterize the behaviour and fluxes of fluvial carbon it is necessary to operate more frequent sampling. This paper presents data from a continuously operating field‐based spectrophotometer simultaneously measuring absorbance across 200–730 nm at 2·5 nm intervals in runoff from an upland peatland stream. It is shown that absorbance at different wavelengths that have previously been used to characterize dissolved organic carbon varies rapidly during storm events. The probe is shown to even detect changes in absorbance characteristics in response to rainfall events before the stream discharge starts to rise. The high‐resolution behaviour of absorbance characteristics during storm events is different depending on the wavelength studied. Thus, the choice of wavelength used as a proxy for dissolved organic carbon needs careful attention and it may be that automated spectrophotometric methods which provide rich time‐series data from across the spectrum can tell us more about fluxes, processes and sources of aquatic carbon in peatland systems in the future than traditional practices have hitherto allowed. Copyright © 2011 John Wiley & Sons, Ltd.     

东亚和西太平洋闪电时空尺度及光辐射能

利用2002—2014年的TRMM/LIS（Tropical Rainfall Measuring Mission/lightning imaging sensor,热带测雨卫星/闪电成像仪）闪电观测数据分析了18°~36°N和70°~160°E范围内闪电尺度和光辐射能空间分布特征,并选取6个区域（区域1~6）,探讨09:00—14:00（地方时,下同）和18:00—次日06:00两个时段闪电上述属性的逐月变化和参数分布特征。研究指出:闪电空间尺度和光辐射能在深海最大,次之为近海和陆地,持续时间在中国东部近海最大,次之为深海和陆地。不同闪电属性大值分布区域差异明显,小值则分布在区域1和区域2。多数区域分析时段内闪电空间尺度和光辐射能的逐月变化趋势较一致,陆地上它们与闪电活动逐月变化的反向对应关系较明显。分析时段内闪电时空尺度和光辐射能均呈对数正态分布,陆地闪电各属性值比海洋闪电更向小值方向集中。在LIS观测性能较高的18:00—次日06:00,各区域内闪电持续时间中值为0.18~0.29 s,通道延展距离中值为12~21 km,光辐射能中值为0.11~0.52 J·m-2·sr-1·μm-1。分析时段内闪电空间尺度与光辐射能的相关性明显优于它们与持续时间的相关性。     

CSRH阵列设计研究及馈源设计的初步考虑

介绍频谱日像仪天线阵排列及实验馈源设计的研究工作。基于CSRH设计指标,模拟了天线阵T型排列、Y型排列、不规则型和螺旋型排列,给出了每种排列的UV覆盖图像,并在成图质量上对各种排列方式做了分析。最后综合考虑提出建议采用自相似螺旋型排列。     

Influence of natural and anthropogenic activities on UV Index variations – a study over tropical urban region using ground based observations and satellite data

Measurements of total ozone column and solar UV radiation under different atmospheric conditions are needed to define variations of both UV and ozone and to study the impact of ozone depletion at the Earth’s surface. In this study, spectral and broadband measurements of UV-B irradiance were obtained along with total ozone observations and aerosol optical depth measurements in the tropical urban region of Hyderabad, south India. We specifically used an Ultra-Violet Multifilter Rotating Shadow band Radiometer (UVMFR-SR), to measure UV irradiance in time and space. To assess the aerosol and O₃ effects on ground-reaching UV irradiance, we used measurements from a Microtops II sun photometer in addition to the Tropospheric Ultraviolet Visible radiation (TUV) model. We also assessed the Defense Meteorological Satellite Program – Operational Line Scanner (DMSP-OLS) night time satellite data for inferring biomass burning fires during the study period. Results clearly suggested a negative correlation between the DMSP-OLS satellite derived fire count data and UVMFR-SR data suggesting that aerosols from biomass burning are directly attenuating UV irradiance in the study region. Also, correlation analysis between UV index and ozone measurements from sun photometer and TOMS-Ozone Mapping Instrument (OMI) indicated a clear decrease in ground reaching UV-B irradiance during higher ozone conditions. The higher levels are attributed to photochemical production of O₃ during the oxidation of trace gases emitted from biomass burning. Results also suggested a relatively high attenuation in UV irradiance (~6% higher) from smoke particles than dust. We also found a relatively good agreement between the modeled (TUV) and measured UV irradiance spectra for different atmospheric conditions. Our results highlight the factors affecting UV irradiance in a tropical urban environment, south India.     

A three-dimensional satellite retrieval method for atmospheric temperature and moisture profiles

A three-dimensional variational method is proposed to simultaneously retrieve the 3-D atmospheric temperature and moisture profiles from satellite radiance measurements. To include both vertical structure and the horizontal patterns of the atmospheric temperature and moisture, an EOF technique is used to decompose the temperature and moisture field in a 3-D space. A number of numerical simulations are conducted and they demonstrate that the 3-D method is less sensitive to the observation errors compared to the 1-D method. When the observation error is more than 2.0 K, to get the best results, the truncation number for the EOF＇s expansion have to be restricted to 2 in the 1-D method, while it can be set as large as 40 in a 3-D method. This results in the truncation error being reduced and the retrieval accuracy being improved in the 3-D method. Compared to the 1-D method, the rms errors of the 3-D method are reduced by 48% and 36% for the temperature and moisture retrievals, respectively. Using the real satellite measured brightness temperatures at 0557 UTC 31 July 2002, the temperature and moisture profiles are retrieved over a region （20°-45°N, 100°- 125°E） and compared with 37 collocated radiosonde observations. The results show that the retrieval accuracy with a 3-D method is significantly higher than those with the 1-D method.     

The ultraviolet reflectance of Enceladus: Implications for surface composition

The reflectance of Saturn’s moon Enceladus has been measured at far ultraviolet (FUV) wavelengths (115-190 nm) by Cassini’s Ultraviolet Imaging Spectrograph (UVIS). At visible and near infrared (VNIR) wavelengths Enceladus’ reflectance spectrum is very bright, consistent with a surface composed primarily of H₂O ice. At FUV wavelengths, however, Enceladus is surprisingly dark - darker than would be expected for pure water ice. Previous analyses have focused on the VNIR spectrum, comparing it to pure water ice (Cruikshank, D.P., Owen, T.C., Dalle Ore, C., Geballe, T.R., Roush, T.L., de Bergh, C., Sandford, S.A., Poulet, F., Benedix, G.K., Emery, J.P. [2005] Icarus, 175, 268-283) or pure water ice plus a small amount of NH₃ (Emery, J.P., Burr, D.M., Cruikshank, D.P., Brown, R.H., Dalton, J.B. [2005] Astron. Astrophys., 435, 353-362) or NH₃ hydrate (Verbiscer, A.J., Peterson, D.E., Skrutskie, M.F., Cushing, M., Helfenstein, P., Nelson, M.J., Smith, J.D., Wilson, J.C. [2006] Icarus, 182, 211-223). We compare Enceladus’ FUV spectrum to existing laboratory measurements of the reflectance spectra of candidate species, and to spectral models. We find that the low FUV reflectance of Enceladus can be explained by the presence of a small amount of NH₃ and a small amount of a tholin in addition to H₂O ice on the surface. The presence of these three species (H₂O, NH₃, and a tholin) appears to satisfy not only the low FUV reflectance and spectral shape, but also the middle-ultraviolet to visible wavelength brightness and spectral shape. We expect that ammonia in the Enceladus plume is transported across the surface to provide a global coating.     

UVolution, a photochemistry experiment in low earth orbit: Investigation of the photostability of carbonates exposed to martian-like UV radiation conditions

The detection and identification of carbonates on Mars are of prime importance to establish the evolution of its atmosphere, correlated to the history of the liquid water, or even to determine the existence of a possible ancient biological activity. Till date, no large deposits of carbonates have been found. In fact, their detection is specific to local areas and in very low amounts. The absence of such deposits is commonly attributed to the harsh environmental conditions at the surface of Mars. Additionally, the presence of UV radiation has been proposed to explain their photodecomposition and hence their absence. However, contradictory results from laboratory experiments mimicking Mars’ surface UV radiation did not resolve the behaviour of carbonates in such an environment, which is why we exposed, in low Earth orbit and in laboratory experiments, both abiotic and biotic calcium carbonates to UV radiation of wavelength above 200 nm, the same spectral distribution as the one reaching the surface of Mars. For low Earth orbit (LEO) exposure, this was done for the UVolution experiment on board the BIOPAN ESA module, which was set outside a Russian Foton automated capsule, and exposed to space conditions for 12 days in September 2007. The targeted carbonates are biominerals and abiotic samples. Our laboratory results mainly show that the exposed carbonates appear to be stable to UV radiation if directly exposed to it. The LEO experiment results tend to the same conclusion, but the integrated exposition time to Solar UV during the experiment is not sufficient to be conclusive. However, the stability of the biominerals derived from the laboratory experiment could strengthen the interest to explore deeper their potential as life records at Mars. Hence, they should be considered as primary targets for in situ analyses during future missions.     

Statistical study of EUV and X-ray transient brightenings

Using the visual inspection and base difference method and data from the X-ray Telescope(XRT)onboard Hinode and TRACE with improved spatial and temporal resolution,we selected 48 X-ray transient brightenings(XTBs)and 237 EUV transient brightenings(ETBs)to study the connection between these two types of transient brightenings(TBs).These ETBs and XTBs have smaller areas(8.42 Mm2 and 36.3 Mm2,respectively,on average)and shorter durations(9.0 rain and 6.9 min,respectively,on average)than previous studies.These XTBs show three types of morphological structure: point-like,single-loop and multiple-loop.We find only 20% of the ETBs have corresponding XTBs while the other 80% have no X-ray signatures at all.This is presumably due to the small amount of released energy,which is not enough to heat the plasma to coronal temperatures which produce X-ray emission rather than being due to the limitation of spatial resolution and temperature sensitivity of the X-ray instrument.These small ETBs may significantly contribute to the coronal heating.