Remote Sensing and Atmosphere

Mohamed Habib Ahmed Elkanzi

doi:doi:10.11648/j.ajaa.20160405.12

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Remote Sensing and Atmosphere

Mohamed Habib Ahmed Elkanzi

Published in American Journal of Astronomy and Astrophysics (Volume 4, Issue 5)

Received: 22 March 2016 Accepted: 11 April 2016 Published: 11 October 2016

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Abstract

The intensities observed along nadiar at the top of atmosphere as a function of solar zenith angle for ƛ = 0.55 micron, haze o refractive index m = 1.50 – 0.031 and aerosols distributed over 0.03 to 10 micron range. As the solar zenith angle increases, the increases in effective atmosphericpath leads to decrease in intensity – approaching to zero a solar zenith of 90. The rate of decrease of intensity with solar zenith angle is more for higher values of reflectivity. The variation with the solar zenith angle at the top of the atmosphere of upward – travelling radiance for each of the lands at bands as seen at an altitude of 45.538 for a surface reflectivity of 0.2. this uses an atmospheric model based on the vertical distribution and content of ozone, aerosol and water vapour for an average mid-latitude summer. Atmosphere.since the solar flux is highest in the spectral interval 0.5-0.6 micron, the upward radiance received by that hand is higher than any other band. Also as the solar zenith angle increases, the upward radiance diminishes as expected because of the added path length through which the solar flux must pass.

Published in	American Journal of Astronomy and Astrophysics (Volume 4, Issue 5)
DOI	10.11648/j.ajaa.20160405.12
Page(s)	60-64
Creative Commons	This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.
Copyright	Copyright © The Author(s), 2016. Published by Science Publishing Group

Keywords

Remote Sensing, Atmosphere Absorption Band, Atmospheric Windows Aerosol

References

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[2]	Estes, J, E., Manual of remte Sensing, 2ed Edition –volume II., American Socity of photogammetry – the Sheridan press, USA, 1983.
[3]	Giboson, P. J, Introductory Remote Sensing Principles and Concept. St Edmunds Bury Press, Great Britanin, 2000.
[4]	Fleming h. e: retrieval of atmospheric temperature profiles from satellite measurements for dynamical forecasting 1992.
[5]	Frits. s. wark, d, q: temperature sounding from satellits, noaatr ness 59 national oseanic atmospheric Washington d.c. 1972. p. 49.
[6]	Kunzi.k.f remote sensing of atmospheric temperature profiles 2009.
[7]	Mather, P, M. and Brand, T. Classification Methods For remotery Sensed date, (2nded), Taylor and Francis Group, LLC, 2009.
[8]	Miler, g. f: fredholm equations of the first kind, in numerical solution of integral equatios, edited by l.m. delvas and j waisvhclarendon press, oxford, 1994.
[9]	Polishchuk, a. l estimations of the information content of meteorological observing system, Leningrad gl, geofis. observ 2002.
[10]	Smith w. l inversion techniques for remote sensing of atmosphere temperature drofiles 2005.
[11]	Thomas, E, G. and Paul, J. C., Atmosphere Climate and Changes, Scientific American Library, New Yurok, 1999.
[12]	Weley, K.K. Modern Physical, 1996.
[13]	Westwater, ed. r inversion techniques in remote sensing of the troposphere, edited by y. e derr, chapter 16, national oceanic and atmospheric administration, Washington, d.c 1972.

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Mohamed Habib Ahmed Elkanzi. (2016). Remote Sensing and Atmosphere. American Journal of Astronomy and Astrophysics, 4(5), 60-64. https://doi.org/10.11648/j.ajaa.20160405.12

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ACS Style

Mohamed Habib Ahmed Elkanzi. Remote Sensing and Atmosphere. Am. J. Astron. Astrophys. 2016, 4(5), 60-64. doi: 10.11648/j.ajaa.20160405.12

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AMA Style

Mohamed Habib Ahmed Elkanzi. Remote Sensing and Atmosphere. Am J Astron Astrophys. 2016;4(5):60-64. doi: 10.11648/j.ajaa.20160405.12

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@article{10.11648/j.ajaa.20160405.12,
  author = {Mohamed Habib Ahmed Elkanzi},
  title = {Remote Sensing and Atmosphere},
  journal = {American Journal of Astronomy and Astrophysics},
  volume = {4},
  number = {5},
  pages = {60-64},
  doi = {10.11648/j.ajaa.20160405.12},
  url = {https://doi.org/10.11648/j.ajaa.20160405.12},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ajaa.20160405.12},
  abstract = {The intensities observed along nadiar at the top of atmosphere as a function of solar zenith angle for ƛ = 0.55 micron, haze o refractive index m = 1.50 – 0.031 and aerosols distributed over 0.03 to 10 micron range. As the solar zenith angle increases, the increases in effective atmosphericpath leads to decrease in intensity – approaching to zero a solar zenith of 90. The rate of decrease of intensity with solar zenith angle is more for higher values of reflectivity. The variation with the solar zenith angle at the top of the atmosphere of upward – travelling radiance for each of the lands at bands as seen at an altitude of 45.538 for a surface reflectivity of 0.2. this uses an atmospheric model based on the vertical distribution and content of ozone, aerosol and water vapour for an average mid-latitude summer. Atmosphere.since the solar flux is highest in the spectral interval 0.5-0.6 micron, the upward radiance received by that hand is higher than any other band. Also as the solar zenith angle increases, the upward radiance diminishes as expected because of the added path length through which the solar flux must pass.},
 year = {2016}
}

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TY  - JOUR
T1  - Remote Sensing and Atmosphere
AU  - Mohamed Habib Ahmed Elkanzi
Y1  - 2016/10/11
PY  - 2016
N1  - https://doi.org/10.11648/j.ajaa.20160405.12
DO  - 10.11648/j.ajaa.20160405.12
T2  - American Journal of Astronomy and Astrophysics
JF  - American Journal of Astronomy and Astrophysics
JO  - American Journal of Astronomy and Astrophysics
SP  - 60
EP  - 64
PB  - Science Publishing Group
SN  - 2376-4686
UR  - https://doi.org/10.11648/j.ajaa.20160405.12
AB  - The intensities observed along nadiar at the top of atmosphere as a function of solar zenith angle for ƛ = 0.55 micron, haze o refractive index m = 1.50 – 0.031 and aerosols distributed over 0.03 to 10 micron range. As the solar zenith angle increases, the increases in effective atmosphericpath leads to decrease in intensity – approaching to zero a solar zenith of 90. The rate of decrease of intensity with solar zenith angle is more for higher values of reflectivity. The variation with the solar zenith angle at the top of the atmosphere of upward – travelling radiance for each of the lands at bands as seen at an altitude of 45.538 for a surface reflectivity of 0.2. this uses an atmospheric model based on the vertical distribution and content of ozone, aerosol and water vapour for an average mid-latitude summer. Atmosphere.since the solar flux is highest in the spectral interval 0.5-0.6 micron, the upward radiance received by that hand is higher than any other band. Also as the solar zenith angle increases, the upward radiance diminishes as expected because of the added path length through which the solar flux must pass.
VL  - 4
IS  - 5
ER  -

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Author Information

Mohamed Habib Ahmed Elkanzi

Department of Astronomy and Meteorology, Faculty Science and Technology, Omdurman Islamic University, Khartoum, Sudan

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APA Style

Mohamed Habib Ahmed Elkanzi. (2016). Remote Sensing and Atmosphere. American Journal of Astronomy and Astrophysics, 4(5), 60-64. https://doi.org/10.11648/j.ajaa.20160405.12

Copy | Download

ACS Style

Mohamed Habib Ahmed Elkanzi. Remote Sensing and Atmosphere. Am. J. Astron. Astrophys. 2016, 4(5), 60-64. doi: 10.11648/j.ajaa.20160405.12

Copy | Download

AMA Style

Mohamed Habib Ahmed Elkanzi. Remote Sensing and Atmosphere. Am J Astron Astrophys. 2016;4(5):60-64. doi: 10.11648/j.ajaa.20160405.12

Copy | Download

@article{10.11648/j.ajaa.20160405.12,
  author = {Mohamed Habib Ahmed Elkanzi},
  title = {Remote Sensing and Atmosphere},
  journal = {American Journal of Astronomy and Astrophysics},
  volume = {4},
  number = {5},
  pages = {60-64},
  doi = {10.11648/j.ajaa.20160405.12},
  url = {https://doi.org/10.11648/j.ajaa.20160405.12},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ajaa.20160405.12},
  abstract = {The intensities observed along nadiar at the top of atmosphere as a function of solar zenith angle for ƛ = 0.55 micron, haze o refractive index m = 1.50 – 0.031 and aerosols distributed over 0.03 to 10 micron range. As the solar zenith angle increases, the increases in effective atmosphericpath leads to decrease in intensity – approaching to zero a solar zenith of 90. The rate of decrease of intensity with solar zenith angle is more for higher values of reflectivity. The variation with the solar zenith angle at the top of the atmosphere of upward – travelling radiance for each of the lands at bands as seen at an altitude of 45.538 for a surface reflectivity of 0.2. this uses an atmospheric model based on the vertical distribution and content of ozone, aerosol and water vapour for an average mid-latitude summer. Atmosphere.since the solar flux is highest in the spectral interval 0.5-0.6 micron, the upward radiance received by that hand is higher than any other band. Also as the solar zenith angle increases, the upward radiance diminishes as expected because of the added path length through which the solar flux must pass.},
 year = {2016}
}

Copy | Download

TY  - JOUR
T1  - Remote Sensing and Atmosphere
AU  - Mohamed Habib Ahmed Elkanzi
Y1  - 2016/10/11
PY  - 2016
N1  - https://doi.org/10.11648/j.ajaa.20160405.12
DO  - 10.11648/j.ajaa.20160405.12
T2  - American Journal of Astronomy and Astrophysics
JF  - American Journal of Astronomy and Astrophysics
JO  - American Journal of Astronomy and Astrophysics
SP  - 60
EP  - 64
PB  - Science Publishing Group
SN  - 2376-4686
UR  - https://doi.org/10.11648/j.ajaa.20160405.12
AB  - The intensities observed along nadiar at the top of atmosphere as a function of solar zenith angle for ƛ = 0.55 micron, haze o refractive index m = 1.50 – 0.031 and aerosols distributed over 0.03 to 10 micron range. As the solar zenith angle increases, the increases in effective atmosphericpath leads to decrease in intensity – approaching to zero a solar zenith of 90. The rate of decrease of intensity with solar zenith angle is more for higher values of reflectivity. The variation with the solar zenith angle at the top of the atmosphere of upward – travelling radiance for each of the lands at bands as seen at an altitude of 45.538 for a surface reflectivity of 0.2. this uses an atmospheric model based on the vertical distribution and content of ozone, aerosol and water vapour for an average mid-latitude summer. Atmosphere.since the solar flux is highest in the spectral interval 0.5-0.6 micron, the upward radiance received by that hand is higher than any other band. Also as the solar zenith angle increases, the upward radiance diminishes as expected because of the added path length through which the solar flux must pass.
VL  - 4
IS  - 5
ER  -

Copy | Download