Analytical Solutions For Martian Nighttime Oh* Layer
M. Grygalashvyly, Leibniz-Institute Of Atmospheric Physics, Kühlungsborn, Germany (Gryga@Iap-Kborn.De),
D. S. Shaposhnikov, Moscow Institute Of Physics And Technology, Moscow, Russia, A. S. Medvedev, Max
Planck Institute For Solar System Research, Göttingen, Germany, G. R. Sonnemann, Leibniz-Institute Of Atmospheric Physics, Kühlungsborn, Germany, P. Hartogh, Max Planck Institute For Solar System Research, Göttingen, Germany.

Introduction:
Airglow Emissions Of Oh* In The Earth Mesopause Region Are Used For Obtaining Information
About Gravity Wave, Planetary Wave And Tidal Parameters, Chemical Distributions (O And H), And Temperature (Trends, Solar Cycle Effects, And Annual Variations). Recently, Hydroxyl Emissions Were Found In
The Martian Atmosphere (Clancy Et Al., 2013), Thus,
We Can Expect Similar Applications Of This Emission
For This Planet.
In Order To Study Morphology And Variability Of
The Layer, The Corresponding Parameters Should Be
Introduced. The Concentration Of Oh* At Peak And
Peak Altitude Represent A Natural Choice For This Purpose. For Interpretation Of Measurements, It Is Desirable To Establish Straightforward Relations Between
These Quantities And The Ambient Temperature, Air
Density And Concentration Of Minor Species Involved
In Photochemical Reactions.
Analytical Approaches:
Assuming The Photochemical Equilibrium For Excited