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1.中国地质大学(北京) 地球科学与资源学院,北京 100083
2.中国气象局 国家卫星气象中心,北京 100081
3.中国气象局 中国遥感卫星辐射测量和定标重点开放实验室,北京 100081
Received:08 April 2021,
Revised:30 April 2021,
Published:15 February 2022
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孙诗雅,黄富祥,夏学齐.青藏高原卫星紫外后向散射辐射的正演仿真[J].光学精密工程,2022,30(03):256-263.
SUN Shiya,HUANG Fuxiang,XIA Xueqi.Forward simulation of solar backscattered ultraviolet radiation for satellite over the Tibetan plateau[J].Optics and Precision Engineering,2022,30(03):256-263.
孙诗雅,黄富祥,夏学齐.青藏高原卫星紫外后向散射辐射的正演仿真[J].光学精密工程,2022,30(03):256-263. DOI: 10.37188/OPE.20223003.0256.
SUN Shiya,HUANG Fuxiang,XIA Xueqi.Forward simulation of solar backscattered ultraviolet radiation for satellite over the Tibetan plateau[J].Optics and Precision Engineering,2022,30(03):256-263. DOI: 10.37188/OPE.20223003.0256.
为了定量评估像元下垫面反射率等要素对青藏高原卫星臭氧遥感数据精度的影响,设计了青藏高原卫星太阳紫外后向散射辐射的正演仿真计算。首先提取NOAA卫星SBUV/2青藏高原像元下垫面的观测数据,结合提取的臭氧垂直廓线数据,设计青藏高原正演仿真计算的输入参数,最后输入风云三号卫星紫外臭氧垂直探测仪正演仿真计算系统开展正演仿真计算,利用计算结果,考察卫星紫外臭氧垂直探测仪通道辐射观测值随下垫面特征参数的变化特征。结果表明:当太阳天顶角在30°~88°内变化时,仪器各个通道的辐亮度观测值都随太阳天顶角增大而减小,变率在
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0.002%~
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46.24%,变率随着波长的增大而增大,其中第12通道的最大达到
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46.24%;当像元下垫面反射率在0~0.8内变化时,仪器通道辐亮度观测值的变化特征随波长不同而有显著差异,其中短波长的第1~6通道,对观测值的影响几乎可以忽略不计,而长波长的第7~12通道,观测值随着下垫面反射率的增大而增大,而且这种变率随着波长的增大而快速增加,第12通道的最大变率达到2 903.2%;像元下垫面有效气压的改变,对仪器通道辐亮度观测值的影响可以忽略不计。
To quantitatively evaluate the influence of elements such as reflectivity of the underlying pixel surface on the precision of ozone data from satellite remote sensing over the Tibetan plateau, a forward simulation calculation of solar backscattered ultraviolet radiation for a satellite over the Tibetan plateau was conducted. First, observation data of the underlying pixel surface from NOAA satellites SBUV/2 over the Tibetan plateau were extracted and combined with the extracted ozone vertical profile. The input parameters of the forward simulation calculation for the Tibetan plateau were adjusted. Then, the parameters were input to the forward simulation system of the FY-3 Solar Backscatter Ultraviolet Sounder for forward simulation calculation. Finally, we investigated the characteristics of the observation value changes from the Solar Backscatter Ultraviolet Sounder channel radiation with different parameters through the calculated results. The results show that, when the solar zenith angle varies in the range of 30°–88°, the radiance observation values for each channel of the instrument decrease with an increase in the solar zenith angle. The rate of variation ranges from
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0.002% to
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46.24%. The variability increases with an increase in wavelength, and the maximum value of the 12-th channel was
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46.24%. When the reflectivity of the underlying pixel surface changes within the range of 0-0.8, the variation characteristics of the observed radiance value from the instrument channel significantly vary with the wavelength. For the short-wavelength channels from 1 to 6, the variation of the channel observations was almost negligible. For the long-wavelength channels from 7 to 12, the observed value increases as the reflectivity of the underlying surface increases. Moreover, this rate of change increases rapidly as the wavelength increases, with a maximum variation of 2 903.2% for channel 12. The variation of the effective air pressure on the underlying pixel surface has almost negligible influence on the observation of the radiance from the instrument channel.
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