@article{13e2411fdeca4f5c9dd406ff0f320005,
title = "Solar radiation on Mars-Update 1991",
abstract = "Detailed information on solar radiation characteristics on Mars are necessary for effective design of future planned solar energy systems operating on the surface of Mars. In this paper we present a procedure and solar radiation related data from which the daily variation of the global, direct beam, and diffuse insolation on Mars are calculated. Given the optical depth of the Mars atmosphere, the global radiation is calculated from the normalized net flux function based on multiple wavelength and multiple scattering of the solar radiation. The direct beam was derived from the optical depth using Beer's law, and the diffuse component was obtained from the difference of the global and the direct beam radiation. The optical depths of the Mars atmosphere were derived from images taken of the Sun with a special diode on the cameras used on the two Viking Landers.",
author = "J. Appelbaum and Landis, {G. A.} and I. Sherman",
note = "Funding Information: Acknowledgment--We are very grateful to James B. Pollack from the Space Science Division, NASA Ames Research Center, for supplying us with the data from which thef(z, r, al) tables were derived. Thanks are extended to Dr. Dennis J. Flood, NASA Lewis Research Center, and coauthor of reference\[2\]fori nitiating the project and for his support. This work was funded by NASA grant NAGW-2022. Funding Information: Missions to the Martian surface will require electric power. Of the several possibilities, photovoitaic power systems can offer many advantages, including high power to weight ratio, modularity, scalability, and a long history of successful application in space. To design a photovoltaic system, detailed information on solar radiation data on the Martian surface is necessary to allow more accurate estimates of photovoltaic power system size and mass in system analysis and trade-off studies of relevant technology options. Solar irradiance on the Mars surface varies with the season and with the amount of atmospheric dust. A major concern is the dust storms, which occur on both local and global scales, and their effect on solar array output. Global storms may persist for such long periods of time, that the requirement for energy storage quickly becomes much too large to be practical. However, as we have shown \[2\],t here is still an appreciable large diffuse component of sunlight available even at high optical depths of the Mars atmosphere, so that solar array operation is still possible. Mars may be considered {"}clear{"} most of the time for most places, but when the global storms occur, their effects are large. The variation of the solar radiation on the Martian surface is governed by three factors: (a) the variation in Mars-Sun distance, (b) variation in solar zenith angle due to Martian season and time of day, and (c) opacity of the Martian atmosphere. Opacity measurements were derived from images taken of the Sun with a special diode on the cameras used on the two Viking Landers. Viking Lander l (VL1) is located at 22.3°N latitude and 47.9 °W longitude (in Chryse ) and Viking * Current address: Tel-Aviv University, Faculty of Engineering, Tel-Aviv,I srael. This work was done while the author was a National Research Council-NASA Research Associate at NASA Lewis Research Center. Work was funded under NASA grant NAGW-2022. * * Sverdrup Technology, Inc. work funded under NASA contract NAS-33-25266.",
year = "1993",
month = jan,
doi = "10.1016/0038-092X(93)90006-A",
language = "אנגלית",
volume = "50",
pages = "35--51",
journal = "Solar Energy",
issn = "0038-092X",
publisher = "Elsevier Ltd.",
number = "1",
}