基于广义回归神经网络的行星际/太阳风参数和地磁指数的紫外极光强度建模          下载免费PDF全文

胡泽骏  韩冰  连慧芳 《地球物理学报》2020,63(5):1738-1750

极光卵极光强度的空间分布是太阳风-磁层-电离层能量耦合过程的重要表现,并且随着空间环境参数和地磁指数的变化而变化,是空间天气的重要指示器.建立合适的极光强度模型对亚暴的预测以及磁层动力学的研究具有重要意义.本文基于Polar卫星的紫外极光成像仪(Ultraviolet Imager,UVI)数据,采用两种不同的极光强度表征方法,即曲线拟合方法(从UVI图像数据中提取极光强度沿磁余纬方向上的曲线特征,Curve Feature along the Magnetic Co-latitude Direction of the Auroral Intensity,CFMCD_AI)和网格化方法(从UVI图像数据中提取极光强度的网格化特征,Gridding Feature of the Auroral Intensity,GF_AI),来构造极区极光强度特征数据库.然后,利用该数据库,采用广义回归神经网络(Generalized Regression Neural Network,GRNN)构建了以行星际/太阳风参数(行星际磁场三分量、太阳风速度和密度)和地磁指数(AE指数)为输入参数的两种极光强度预测模型(GRNN_CFMCD_AI模型和GRNN_GF_AI模型).利用图像质量评价指数结构相似度(structure similarity,SSIM)作为极光强度模型预测结果和对应的UVI图像的相似性评价标准(完全相似为1,不相似为0,一般认为SSIM大于0.5是具有较好的相似性),对两种极光强度模型进行了性能评价.结果显示,GRNN_GF_AI模型预测结果对应的SSIM值范围为0.36～0.77,均值为0.54,性能优于GRNN_CFMCD_AI模型的.  相似文献   

南京市紫外线辐射强度的变化及影响因子   总被引：1，自引：0，他引：1  

毛宇清  沈澄  姜爱军  严文莲  叶香 《气象科学》2011,31(5):621-625

利用南京市2005-02—2009-01共4 a的紫外线辐射观测资料,分析了到达地面的紫外线辐射强度的变化特征,并探讨了云、污染物浓度和雾、霾天气等对紫外线辐射强度的影响。结果表明,低云量对紫外线强度的衰减更明显,最大达58.15%,蔽光性云层对紫外线辐射强度的衰减可达71%～80%;紫外线辐射强度与污染物浓度呈负相关,其中与NO2的相关性最好,为-0.39;晴空条件下,严重霾对紫外线辐射强度的衰减率可达20%以上,浓雾对紫外线辐射强度的衰减接近50%。  相似文献   

中国对虾人工诱导雌核发育的研究 Ⅱ.紫外线辐射对精子顶体反应和受精能力的影响     

陈本楠  蔡难儿  李光友 《海洋科学》1997,21(1):41-47

研究了 36 5 nm波长紫外线辐射中国对虾精子对其顶体反应和受精能力的影响。结果表明 ,低剂量紫外线辐射促进精子发生顶体反应 ,大剂量辐射使精子丧失发生顶体反应的生理机能并死亡。 36 5 nm波长紫外线能够透过精荚和纳精囊盖 ,对其内精子起到杀伤作用。精液稀释液在紫外线下辐射 5～ 8s,仍有部分精子具有受精能力 ,但胚胎在早期阶段即死亡。人工诱导雌核发育的过程中 ,紫外线辐射精液稀释液 5～ 8s,可获得遗传物质失活的精子 (激活源 )。经透射电镜观察分析 ,紫外线对精子遗传物质的损伤是一种使染色质变性的化学作用。  相似文献   

扇贝多肽在体外对免疫细胞活性的影响及其抗紫外线的氧化损伤作用   总被引：9，自引：2，他引：9  

刘晓萍  王玉贞  韩彦弢  于业军  王跃军  王春波 《海洋与湖沼》2001,32(4):414-419

采用噻唑盐（MTT）比色方法研究在紫外线辐射损伤条件下扇贝多肽对免疫细胞的保护作用，并探讨扇贝多肽对胸腺细胞和脾细胞活性的影响，结果表明，扇贝多肽具有抗紫外线氧化损伤的作用，可减轻或抑制紫外线对胸腺细胞和脾细胞的氧化损伤，并且呈剂量依赖性，扇贝多肽在0.5%-10.0%的浓度范围内，其抗氧化能力随浓度的增高而增强，在正常条件下可显著增强免疫细胞的活性，并且可拮抗雌激素对免疫细胞的抑制作用。提示扇贝多肽不仅具有抗氧化损伤作用，而且具有免疫增强使用。  相似文献   

Influence of aerosol multiple scattering of ultraviolet radiation on martian atmospheric sensing     

M.-P. Zorzano  C. Córdoba-Jabonero 《Icarus》2007,190(2):492-503

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Lunar atmospheric H₂ detections by the LAMP UV spectrograph on the Lunar Reconnaissance Orbiter     

S. Alan Stern  Jason C. Cook  Jean -Yves Chaufray  Paul D. Feldman  G. Randall Gladstone  Kurt D. Retherford 《Icarus》2013

We report on the detection of H₂ as seen in our analysis of twilight observations of the lunar atmosphere observed by the LAMP instrument aboard NASA’s Lunar Reconnaissance Orbiter. Using a large amount of data collected on the lunar atmosphere between September 2009 and March 2013, we have detected and identified, the presence of H₂ in the native lunar atmosphere, for the first time. We derive a surface density for H₂ of 1.2 ± 0.4 × 10³ cm⁻³ at 120 K. This is about 10 times smaller than originally predicted, and several times smaller than previous upper limits from the Apollo era data.  相似文献   

Hubble observations of Jupiter’s north–south conjugate ultraviolet aurora     

J.-C. Gérard  D. Grodent  A. Radioti  B. Bonfond  J.T. Clarke 《Icarus》2013

Comparisons of the northern and southern far ultraviolet (UV) auroral emissions of Jupiter from the Hubble Space Telescope (HST) or any other ultraviolet imager have mostly been made so far on a statistical basis or were not obtained with high sensitivity and resolution. Such observations are important to discriminate between different mechanisms responsible for the electron acceleration of the different components of the aurora such as the satellite footprints, the «main oval» or the polar emissions. The field of view of the ACS and STIS cameras on board HST is not wide enough to provide images of the full jovian disk. We thus compare the morphology of the north and south aurora observed 55 min apart and we point out similarities and differences. On one occasion HST pointed successively the two polar regions and auroral images were seen separated by only 3 min. This makes it possible to compare the emission structure and the emitted FUV power of corresponding regions. We find that most morphological features identified in one hemisphere have a conjugate counterpart in the other hemisphere. However, the power associated with conjugate regions of the main oval, diffuse or discrete equatoward emission observed quasi-simultaneously may be different in the two hemispheres. It is not directly nor inversely proportional to the strength of the B-field as one might expect for diffuse precipitation or field-aligned acceleration with equal ionospheric electron density in both hemispheres. Finally, the lack of symmetry of some polar emissions suggests that some of them could be located on open magnetic field lines.  相似文献   

Measurements of winds on Mars with Hubble Space Telescope images in 2003 opposition     

V.G. Kaydash  M.A. Kreslavsky  Yu.G. Shkuratov  J.F. Bell III 《Icarus》2006,185(1):97-101

The winds of Mars at the water cloud level are measured by tracking cloud features in sequential high-resolution Hubble Space Telescope UV images for 5 days during the perihelion season in 2003. Global circulation model (GCM) predictions are in general agreement with the observations for the zonal wind component, but reveal significant differences for the meridional component.  相似文献   

New Horizons Alice ultraviolet observations of a stellar occultation by Jupiter’s atmosphere     

Thomas K. Greathouse  G.R. Gladstone  S.A. Stern  R.J. Vervack Jr.  M.H. Versteeg  L.A. Young  H. Throop 《Icarus》2010,208(1):293-305

The Alice ultraviolet spectrograph onboard the New Horizons spacecraft observed two occultations of the bright star χ Ophiucus by Jupiter’s atmosphere on February 22 and 23, 2007 during the approach phase of the Jupiter flyby. The ingress occultation probed the atmosphere at 32°N latitude near the dawn terminator, while egress probed 18°N latitude near the dusk terminator. A detailed analysis of both the ingress and egress occultations, including the effects of molecular hydrogen, methane, acetylene, ethylene, and ethane absorptions in the far ultraviolet (FUV), constrains the eddy diffusion coefficient at the homopause level to be  cm² s⁻¹, consistent with Voyager measurements and other analyses (Festou, M.C., Atreya, S.K., Donahue, T.M., Sandel, B.R., Shemansky, D.E., Broadfoot, A.L. [1981]. J. Geophys. Res. 86, 5717-5725; Vervack Jr., R.J., Sandel, B.R., Gladstone, G.R., McConnell, J.C., Parkinson, C.D. [1995]. Icarus 114, 163-173; Yelle, R.V., Young, L.A., Vervack Jr., R.J., Young, R., Pfister, L., Sandel, B.R. [1996]. J. Geophys. Res. 101 (E1), 2149-2162). However, the actual derived pressure level of the methane homopause for both occultations differs from that derived by [Festou et al., 1981] and [Yelle et al., 1996] from the Voyager ultraviolet occultations, suggesting possible changes in the strength of atmospheric mixing with time. We find that at 32°N latitude, the methane concentration is  cm⁻³ at 70,397 km, the methane concentration is  cm⁻³ at 70,383 km, the acetylene concentration is  cm⁻³ at 70,364 km, and the ethane concentration is  cm⁻³ at 70,360 km. At 18°N latitude, the methane concentration is  cm⁻³ at 71,345 km, the methane concentration is  cm⁻³ at 71,332 km, the acetylene concentration is cm⁻³ at 71,318 km, and the ethane concentration is  cm⁻³ at 71,315 km. We also find that the H₂ occultation light curve is best reproduced if the atmosphere remains cold in the microbar region such that the base of the thermosphere is located at a lower pressure level than that determined by in situ instruments aboard the Galileo probe (Seiff, A., Kirk, D.B., Knight, T.C.D., Young, R.E., Mihalov, J.D., Young, L.A., Milos, F.S., Schubert, G., Blanchard, R.C., Atkinson, D. [1998]. J. Geophys. Res. 103 (E10), 22857-22889) - the Sieff et al. temperature profile leads to too much absorption from H₂ at high altitudes. However, this result is highly model dependent and non-unique. The observations and analysis help constrain photochemical models of Jupiter’s atmosphere.  相似文献   

Comparison of Brewer spectrophotometer ultraviolet data from similar latitudes in the Northern and Southern Hemisphere     

M. G. Kimlin  J. M. Sabburg  A. V. Parisi  R. S. Meltzer 《Journal of Atmospheric and Solar》2003,65(16-18):1401-1410

This paper presents UV data recorded over 12 months in 2000/2001 at a southern hemisphere (Toowoomba) and similar latitude northern hemisphere (BigBend and Everglades) sites using Brewer Spectrophotometers. The peak daily erythemally weighted UV (DUV) at the Toowoomba site was 8.8% and 25% higher compared to that at the BigBend and Everglades sites, respectively. The Everglades site exposures are lower than the BigBend site exposures in summer and spring. This may be due to the higher cloud cover for the Everglades site. The summer DUV values between Toowoomba and BigBend are similar. In spring, the average DUV value is the greatest at BigBend compared to the other two sites. Results indicate that variability between the measurement sites is due to varying cloud and ozone, and possibly due to aerosol and airmass differences of each region. Of these different site-specific local atmospheric conditions, cloud was the main contributor to the differences in UV between the sites.  相似文献