{"title":"Modelling of the twilight sky brightness using a numerical solution of the radiation transfer equation","authors":"Yu.E. Belikov","doi":"10.1016/0021-9169(95)00175-1","DOIUrl":null,"url":null,"abstract":"<div><p>A model of solar light scattering in the terrestrial spherical atmosphere is developed on the basis of a numerical solution of the radiation transfer equation. It allows us to model the twilight sky brightness. This brightness for the range of solar zenith angles of 92–106 degrees and wavelength 530 tun has been compared with the experimental data and with other calculated results. Modelling has been carried out for standard altitude distributions of the molecular number density and ozone absorption coefficient and for the aerosol model of Toon and Pollack (1976). The different layers' contribution and the contribution of different orders of scattering from'some altitudes to the zenith intensity have been obtained. The role of multiple scattering in the twilight sky brightness and a hypothesis on the high turbidity of the upper atmosphere are discussed.</p></div>","PeriodicalId":100754,"journal":{"name":"Journal of Atmospheric and Terrestrial Physics","volume":"58 16","pages":"Pages 1843-1848"},"PeriodicalIF":0.0000,"publicationDate":"1996-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.1016/0021-9169(95)00175-1","citationCount":"7","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Journal of Atmospheric and Terrestrial Physics","FirstCategoryId":"1085","ListUrlMain":"https://www.sciencedirect.com/science/article/pii/0021916995001751","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 7
Abstract
A model of solar light scattering in the terrestrial spherical atmosphere is developed on the basis of a numerical solution of the radiation transfer equation. It allows us to model the twilight sky brightness. This brightness for the range of solar zenith angles of 92–106 degrees and wavelength 530 tun has been compared with the experimental data and with other calculated results. Modelling has been carried out for standard altitude distributions of the molecular number density and ozone absorption coefficient and for the aerosol model of Toon and Pollack (1976). The different layers' contribution and the contribution of different orders of scattering from'some altitudes to the zenith intensity have been obtained. The role of multiple scattering in the twilight sky brightness and a hypothesis on the high turbidity of the upper atmosphere are discussed.
京公网安备 11010802042870号
京ICP备2023020795号-1
分享
求助内容：
应助结果提醒方式：
扫码关注我们
