Analysis of UVB values in the centre of the Iberian Peninsula     

E. Gutirrez-Marco  E. Hernndez  J.L. Camacho  A. Labajo 《Atmospheric Research》2007,84(4):345-352

Records of UV data started in Madrid at the beginning of the 90's decade. After some quality control on the data a seven year period from 1996 to 2002 was selected to perform an analysis of daily and seasonal variability of solar ultraviolet B (UVB) values at the centre of the Iberian Peninsula. Instruments used are a Brewer MKIV spectrophotometer and a YES UVB-1 broadband pyranometer. Both instruments provided integrated daily values according with the Diffey spectrum although they have different measurement procedures. Data statistics from each instrument for the same period and statistical relationships between daily values from both instruments are shown. As broadband YES provided a record with fewer time gaps, analysis of UVI extreme values is performed using that instrument. The relationship between UVB values with ozone, cloudiness and visible radiation has been described in several papers for different places in the world. In this paper, those relationships are shown for Madrid. A discussion about specific problems found when trying to isolate every effective factor is also included. Some of those relationships could be helpful to retrieve UVB values from other ancillary data as visible radiation and cloudiness. Finally, a detailed study for 10 days in June 1997 when the maximum record of daily values from the present time series was obtained, highlight the close correlation between total ozone content and the daily variability of UVB for similar amounts of incoming radiation.  相似文献   

Real-time measurement of volcanic SO2 emissions: validation of a new UV correlation spectrometer (FLYSPEC)     

Keith A. Horton  Glyn Williams-Jones  Harold Garbeil  Tamar Elias  A. Jeff Sutton  Peter Mouginis-Mark  John N. Porter  Steven Clegg 《Bulletin of Volcanology》2006,68(4):323-327

A miniaturized, lightweight and low-cost UV correlation spectrometer, the FLYSPEC, has been developed as an alternative for the COSPEC, which has long been the mainstay for monitoring volcanic sulfur dioxide fluxes. Field experiments have been conducted with the FLYSPEC at diverse volcanic systems, including Masaya (Nicaragua), Poás (Costa Rica), Stromboli, Etna and Vulcano (Italy), Villarica (Chile) and Kilauea (USA). We present here those validation measurements that were made simultaneously with COSPEC at Kilauea between March 2002 and February 2003. These experiments, with source emission rates that ranged from 95 to 1,560 t d⁻¹, showed statistically identical results from both instruments. SO₂ path-concentrations ranged from 0 to >1,000 ppm-m with average correlation coefficients greater than r ²=0.946. The small size and low cost create the opportunity for FLYSPEC to be used in novel deployment modes that have the potential to revolutionize the manner in which volcanic and industrial monitoring is performed.  相似文献   

A new relation between the central spectral solar H I Lyman α irradiance and the line irradiance measured by SUMER/SOHO during the cycle 23     

Claude Emerich  Philippe Lemaire  Werner Curdt  Klaus Wilhelm 《Icarus》2005,178(2):429-433

The spectral irradiance at the center of the solar H I Lyman α (, referred to as Lyα in this paper) line profile is the main excitation source responsible for the atomic hydrogen resonant scattering of cool material in our Solar System. It has therefore to be known with the best possible accuracy in order to model the various Lyα emissions taking place in planetary, cometary, and interplanetary environments. Since the only permanently monitored solar irradiance is the total one (i.e. integrated over the whole Lyα line profile), Vidal-Madjar [1975. Evolution of the solar Lyman alpha flux during four consecutive years. Solar Phys. 40, 69-86] using Orbiting Solar Observatory 5 (OSO-5) satellite Lyα data, established a semi-empirical formula allowing him to deduce the central spectral Lyα irradiance from the total one. This relation has been extensively used for three decades. But, at the low altitude of the OSO-5 orbit, the central part of the solar line profile was deeply absorbed by a large column of exospheric atomic hydrogen. Consequently, the spectral irradiance at the center of the line was obtained by a complex procedure confronting the observations with simulations of both the geocoronal absorption and the self-reversed shape of the solar Lyα profile. The SUMER spectrometer onboard SOHO positioned well outside the hydrogen geocorona, provided full-Sun Lyα profiles, not affected by such an absorption [Lemaire et al., 1998. Solar H I Lyman α full disk profile obtained with the SUMER/SOHO spectrometer. Astron. Astrophys. 334, 1095-1098; 2002. Variation of the full Sun Hydrogen Lyman α and β profiles with the activity cycle. Proc. SOHO 11 Symposium, ESA SP-508, 219-222; 2004. Variation of the full Sun Hydrogen Lyman profiles through solar cycle 23. COSPAR 2004 Meeting], making it—for the first time—possible to measure the spectral and total Lyα solar irradiances directly and simultaneously. A new relation between these two quantities is derived in an expression that is formally similar to the previous one, but with significantly different parameters. After having discussed the potential causes for such differences, it is suggested that the new relation should replace the old one for any future modeling of the numerous Lyα absorptions and emissions observed in the Solar System.  相似文献   

Cassini UVIS observations of the Io plasma torus: IV. Modeling temporal and azimuthal variability     

A.J. Steffl  P.A. Delamere 《Icarus》2008,194(1):153-165

In this fourth paper in a series, we present a model of the remarkable temporal and azimuthal variability of the Io plasma torus observed during the Cassini encounter with Jupiter. Over a period of three months, the Cassini Ultraviolet Imaging Spectrograph (UVIS) observed a dramatic variation in the average torus composition. Superimposed on this long-term variation, is a 10.07-h periodicity caused by an azimuthal variation in plasma composition subcorotating relative to System III longitude. Quite surprisingly, the amplitude of the azimuthal variation appears to be modulated at the beat frequency between the System III period and the observed 10.07-h period. Previously, we have successfully modeled the months-long compositional change by supposing a factor of three increase in the amount of material supplied to Io's extended neutral clouds. Here, we extend our torus chemistry model to include an azimuthal dimension. We postulate the existence of two azimuthal variations in the number of superthermal electrons in the torus: a primary variation that subcorotates with a period of 10.07 h and a secondary variation that remains fixed in System III longitude. Using these two hot electron variations, our model can reproduce the observed temporal and azimuthal variations observed by Cassini UVIS.  相似文献   

Observation of the hydrogen corona with SPICAM on Mars Express   总被引：1，自引：0，他引：1  

J.Y. Chaufray  E. Quémerais 《Icarus》2008,195(2):598-613

A series of seven dedicated Lyman-α observations of exospheric atomic hydrogen in the martian corona were performed in March 2005 with the ultraviolet spectrometer SPICAM on board Mars Express. Two types of observations are analyzed, observations at high illumination (for a solar zenith angle SZA equal to 30°) and observations at low illumination (for a solar zenith angle equal to 90° (terminator), and near the south pole). The measured Lyman-α emission is interpreted as purely resonant scattering of solar photons. Because the Lyman-α emission is optically thick, we use a forward model to analyze this data. Below the exobase, the hydrogen density is described by a diffusive model and above the exobase, it follows Chamberlain's approach without satellite particles. For different hydrogen density profiles between 80 and 50,000 km, the volume emission rates are computed by solving the radiative transfer equation. Such an approach has been used to analyze the Mariner 6, 7 exospheric Lyman-α data during the late 1960s. A reasonable fit of the set of observations is obtained assuming an exobase temperature between 200 and 250 K and an exobase density of ∼1-4 × 10⁵ cm⁻³ in good agreement with photochemical models. However, when considering the average exospheric temperature of 200 K measured by other methods [Leblanc, F., Chaufray, J.Y., Witasse, O., Lilensten, J., Bertaux, J.-L., 2006a. J. Geophys. Res. 111 (E9), doi:10.1029/2005JE002664. E09S11; Leblanc, F., Chaufray, J.-Y., Bertaux, J.-L., 2007. Geophys. Res. Lett. 34, doi:10.1029/2006GL028437. L02206; Bougher, S.W., Engel, S., Roble, R.G., Foster, B., 2000. J. Geophys. Res. 105, 17669-17692; Mazarico, E., Zuber, M.T., Lemoine, F.G., Smith, D.E., 2007. J. Geophys. Res. 112, doi:10.1029/2006JE002734. E05014] a supplementary hot population is needed above the exobase to reconcile Lyman-α measurements with these previous measurements, particularly for the observations at low SZA. In this case, the densities and temperatures at the exobase for the two populations are 1.0±0.2×¹⁰⁵ cm⁻³ and T=200 K and 1.9±0.5×¹⁰⁴ cm⁻³ and T>500 K for the cold and hot populations respectively at low SZA. At high SZA, the densities and temperatures are equal to 2±0.4×¹⁰⁵ cm⁻³ and T=200 K and n=1.2±0.5×¹⁰⁴ cm⁻³ and T>500 K. These high values of the hot hydrogen component are not presently supported by the theory. Moreover, it is important to underline that the two population model remains relatively poorly constrained by the limited range of altitude covered by the present set of SPICAM measurements and cannot be unambiguously identified because of the global uncertainty of our model and of SPICAM measurements. For a one population solution, an average water escape rate of 7.5 × 10⁻⁴ precipitable μm/yr is estimated, yielding a lifetime of 13,000 years for the average present water vapor content of 10 precipitable microns.  相似文献   

重庆主城区紫外线辐射强度变化特征分析   总被引：1，自引：0，他引：1       下载免费PDF全文

胡春梅  陈道劲  廖峻 《气象与环境学报》2009,25(2):23-27

研究重庆主城区紫外线辐射强度的变化规律,为业务预报和客观预报方法的研究提供基础。利用2004年3月—2008年2月的实况观测资料,分析主城区紫外线辐射强度的日、月、季和年变化规律。结果表明：重庆主城区日平均最大辐射量出现在中午13时—14时。7月和8月的辐射强度为全年最强,出现辐射等级四级的概率最大;而1月和12月为全年最弱,没有出现过辐射等级高于三级的样本。季节平均辐射强度夏、春、秋、冬依次减弱。2004年和2006—2007年平均辐射强度相当,2005年较弱。  相似文献   

紫外辐照条件下二维填料对聚丙烯耐老化行为的影响          下载免费PDF全文

郭凡  刘志启  李娜  王庭胜  李丽娟 《盐湖研究》2020,28(3):54-60

采用水热法合成了二维层状材料——镁镍铁水滑石(MgNiFe-LDH),考察不同水热时间和水热温度对MgNiFe-LDH合成的影响,通过X射线衍射(XRD)、傅里叶变换红外光谱(FT-IR)、扫描电镜(SEM)和热分析(TG/DTG)等测试方法,对样品的结构、形貌及热性能进行表征。将合成的MgNiFe-LDH添加至聚丙烯(PP)制备MgNiFe-LDH/PP复合材料,通过对材料加速老化测其力学性能,研究了添加MgNiFe-LDH前后材料机械性能变化。结果表明,当Mg~(2+):Ni~(2+):Fe~(3+)=2∶1∶1,水热温度140℃、水热时间24 h时,合成的MgNiFe-LDH为片状,形貌较为规整,颗粒粒径约为2μm。MgNiFe-LDH/PP复合材料经加速老化后,填充MgNiFe-LDH复合材料的抗老化性能优于纯PP,当MgNiFe-LDH的填充量为6 wt%复合材料拉伸强度不变,可明显提高PP的抗老化性能。  相似文献   

Ultraviolet sky surveys. Instruments, findings, and prospects     

Noah Brosch 《Experimental Astronomy》1999,9(3):119-187

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中国地区近地面太阳紫外辐射的分布及其对大气臭氧层破坏的响应   总被引：7，自引：4，他引：7       下载免费PDF全文

熊效振  王庚辰 《大气科学》1993,17(5):611-620

本文在充分考虑太阳紫外辐射在大气中传输的物理过程的基础上,引入局地地面气压、臭氧和地表反照率的时空变化,利用Delta-Eddington近似法计算了中国地区冬季(1月)和夏季(7月)晴天时地面太阳紫外辐射(0.290—0.400μm)和紫外B辐射(0.290—0.325μm)的分布,并进一步计算出臭氧总量减少5％、15％时紫外B的变化.结果指出,由于臭氧总量的减少,中国北部地区紫外B的增加比南部地区显著.平均而言,臭氧总量减少1％时,冬季紫外B将增加1％左右,夏季紫外B将增加0.6％—0.7％.  相似文献   

Structure and Evolution of White Dwarfs and their Interaction with the Local Interstellar Medium     

M. A. Barstow  K. Werner 《Astrophysics and Space Science》2006,303(1-4):3-16

The development of far-UV astronomy has been particularly important for the study of hot white dwarf stars. A significant fraction of their emergent flux appears in the far-UV and traces of elements heavier than hydrogen or helium are, in general, only detected in this waveband or at shorter wavelengths that are also only accessible from space. Although white dwarfs have been studied in the far-UV throughout the past ∼25 years, since the launch of IUE, only a few tens of objects have been studied in great detail and a much larger sample is required to gain a detailed understanding of the evolution of hot white dwarfs and the physical processes that determine their appearance. We review here the current knowledge regarding hot white dwarfs and outline what work needs to be carried out by future far-UV observatories.  相似文献