Venus lower thermosphere studies

Studies undertaken in this project have sought to understand lower thermospheric structure and dynamics (less than or equal to 145 km), particularly the processes responsible. This is a region just below the reach of in-situ instruments onboard PVO (Pioneer Venus Orbiter) during the first few diurnal cycles. PVO remote airglow observations (nitric oxide, O2, visible, O 1304A) have been coupled with ground-based observations (CO densities, winds, temperatures, O2 IR nightglow) to address the behavior of lower thermospheric winds and chemistry over 95 to 150 km. This interpretation of PVO and related data is accomplished by using the NCAR Venus thermospheric general circulation model (VTGCM) (Bougher et al., 1988; 1990). This model has been modified over the last two years to improve its ability to calculate O, CO, and O2 densities, temperatures, nightglow, and subsolar-to-antisolar and zonal winds over 95 to 150 km (Bougher and Borucki, 1992). Our VTGCM studies show that: (1) O2 visible and IR nightglow distributions can be used to trace lower thermosphere / upper mesosphere winds over 100-130 km. Typically, weak zonal winds (less than or equal to 25 m/sec) and nightglow maximum patches near 0100 LT prevail. Occasionally, strong zonal winds (30-60 m/sec) and airglow patches peaking near 0300 LT characterize the Venus lower thermosphere. (2) It is clear that the dynamics of the Venus 90-130 km region is highly variable on time scales as short as an hour. This is most likely due to the time variable nature of upward propagating gravity waves, which grow in amplitude and eventually break. The resulting turbulence gives rise to local time variable eddy diffusion and momentum drag, both of which strongly impact global density and nightglow distributions. (3) The oxygen chemistry (O, O2, etc.) over 90-120 km is strongly dependent on HO(x) and CLO(x) tracer species that must be properly included in any coupled chemical dynamical model. (4) The density profiles of light species (O, CO, N, He) are strongly affected by large-scale transport by the winds. Strong eddy diffusion is not a suitable model parameterization for approximating these light species, especially for extrapolation into the region below 140 km where PVO in-situ data is lacking. Instead, the fully coupled chemical dynamical VTGCM model should be used to improve estimates of densities within the VTS3 empirical model (Hedin et al., 1983) below 140 km

Zonal Wind Calculations from Mars Global Surveyor Accelerometer and Rate Data

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/76565/1/AIAA-28588-795.pd

Hot carbon corona in Mars' upper thermosphere and exosphere: 2. Solar cycle and seasonal variability

This work presents the variability over seasons (i.e., orbital position) and solar cycle of the Martian upper atmosphere and hot carbon corona. We investigate the production and distribution of energetic carbon atoms and the impacts on the total global hot carbon loss from dominant photochemical processes at five different cases: AL (aphelion and low solar activity), EL (equinox and low solar activity), EH (equinox and high solar activity), PL (perihelion and low solar activity), and PH (perihelion and high solar activity). We compare our results with previously published results but only on the limited cases due to the dearth of studies on solar EUV flux and seasonal variabilities. Photodissociation of CO and dissociative recombination of CO+ are generally regarded as the two most important source reactions for the production of hot atomic carbon. Of these two, photodissociation of CO is found to be the dominant source in all cases considered. To describe self‐consistently the exosphere and the upper thermosphere, a 3‐D kinetic particle simulator, the Adaptive Mesh Particle Simulator, and the 3‐D Mars Thermosphere General Circulation Model are one‐way coupled. The basic description of this hot carbon calculation can be found in the companion paper to this one. The spatial distributions and profiles of density and temperature and atmospheric loss rates are discussed for the cases considered. Finally, our computed global escape rate of hot carbon ranges from 5.28 × 1023 s−1 (AL) to 55.1 × 1023 s−1 (PL).Key PointsSolar cycle and seasonal variability of hot C corona is simulated in 3‐DOur simulation considered PD of CO and DR of CO+ as main sourcesThe estimated escape rates range from 5.28 to 55.1E23 s−1Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/110543/1/jgre20338.pd

Hot carbon corona in Mars’ upper thermosphere and exosphere: 1. Mechanisms and structure of the hot corona for low solar activity at equinox

Two important source reactions for hot atomic carbon on Mars are photodissociation of CO and dissociative recombination of CO + ; both reactions are highly sensitive to solar activity and occur mostly deep in the dayside thermosphere. The production of energetic particles results in the formation of hot coronae that are made up of neutral atoms including hot carbon. Some of these atoms are on ballistic trajectories and return to the thermosphere, and others escape. Understanding the physics in this region requires modeling that captures the complicated dynamics of hot atoms in 3‐D. This study evaluates the carbon atom inventory by investigating the production and distribution of energetic carbon atoms using the full 3‐D atmospheric input. The methodology and details of the hot atomic carbon model calculation are given, and the calculated total global escape of hot carbon from the assumed dominant photochemical processes at a fixed condition, equinox ( L s  = 180°), and low solar activity ( F 10.7 = 70 at Earth) are presented. To investigate the dynamics of these energetic neutral atoms, we have coupled a self‐consistent 3‐D global kinetic model, the Adaptive Mesh Particle Simulator, with a 3‐D thermosphere/ionosphere model, the Mars Thermosphere General Circulation Model to provide a self‐consistent global description of the hot carbon corona in the upper thermosphere and exosphere. The spatial distributions of density and temperature and atmospheric loss are simulated for the case considered. Key Points Hot C corona is simulated at the fixed condition within our frameworks Background atmosphere greatly impacts the structure of hot C corona The estimated global escape rates of hot C is 5.9 x 1023 s‐1Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/107587/1/jgre20239.pd

Three‐dimensional study of Mars upper thermosphere/ionosphere and hot oxygen corona: 2. Solar cycle, seasonal variations, and evolution over history

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/95238/1/jgre2686.pd

Vertical dust mixing and the interannual variations in the Mars thermosphere

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/94815/1/jgre2303.pd

Three‐dimensional study of Mars upper thermosphere/ionosphere and hot oxygen corona: 1. General description and results at equinox for solar low conditions

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/94871/1/jgre2685.pd

Four Martian years of nightside upper thermospheric mass densities derived from electron reflectometry: Method extension and comparison with GCM simulations

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/95498/1/jgre2766.pd