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An investigation and analysis of the density and thermal balance of the Martian ionosphereThe major photochemistry consisted of solar EUV and photoelectrons comprising 70 percent and 30 percent respectively, of the initial source of CO2(+) and O(+). The energetic O2(+) provided a substantial source of energy to the ambient ions, distributing of the order of 1.6 x 10 to the -7 power W/sq m at an average of 160 km. This input can be compared to that from the ambient electrons of 1.3 x 10 to the -7 power W/sq m with average deposition at 145 km and from the calculated thermal conduction of 1 x 10 to the -9 power W/sq m at 270 km and 1 x 10 to the -8 power at 230 km for assumed dip angles of 2 deg and 12 deg respectively, for a 10nT magnetic field. At altitudes above 250 km upward, vertical fluxes of the order 6 x 10 to the 10th power/sq m/sec for the thermal ions were calculated. The net ionization of O(+) and CO2(+) by charge exchange with incoming solar wind protons varied from 5 x 10 to the 8th power to 5 x 10 to the 12th power /sq m/sec for assumed field strengths of 50nT to 2nT on the dayside of the planet.
Document ID
19790022952
Acquisition Source
Legacy CDMS
Document Type
Contractor Report (CR)
Authors
Rohrbaugh, R. P. (Pennsylvania State Univ. University Park, PA, United States)
Date Acquired
September 3, 2013
Publication Date
July 27, 1979
Subject Category
Lunar And Planetary Exploration
Report/Patent Number
NASA-CR-162141
PSU-IRL-SCI-463
Accession Number
79N31123
Funding Number(s)
CONTRACT_GRANT: NGL-39-009-003
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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