Saturday, July 22, 2017

Mars: Part 3 Effects of Suspended Dust


by Dr. Robert Duncan-Enzmann 
reproduced from the Enzmann Archives by WKS

Dust particles, ice crystals, and droplets effect capsules designed for unmanned descent, landing, deployment, and subsequent use. Effects recommended for study are as follows:

* Visibility at ultra-violet, optical, and infra-red frequencies as functions of attenuation, scattering, albedo.
* Communications at radio and radar frequencies as functions of attenuation, refraction, and static noises due to the exchange of energy between particles and antenna.
* Physical effects of particles on equipment including erosion, probability of burial by dunes, bearing strength of terrain recently formed by Aeolian-forces.

The behavior of particles in the atmosphere of a planet may be considered first of all from the point of view of forces tending to introduce them to the atmosphere and forces tending to remove them from the atmosphere. Solid particles will most strongly and most immediately effect objects close to, or on the surface of a planet. Forces working to remove particles from an atmosphere are particle-particle collisions or other interactions, which can only be of significance when particles are of sub-micron size or electrically active, particle-particle interactions in media like nuée-ardent where particles are very dense and may average millimeters in extent, and finally, the more important settling in a gravitational field through a viscos atmosphere. The rate of settling is approximated by Stokes law as given below. If the Kaplan atmosphere for Mars is used, settling rates are slightly slower than those for the Earth. If an 80mb atmosphere is used, settling rates through the atmosphere of Mars through the lower troposphere are about 2 ½ to 3 ½ times as long as those for earth. 

(Stokes’ Law: The force of viscosity on a small sphere moving through a viscous fluid is given by:Fd = 6 π η Rv {\displaystyle F_{d}=6\pi \,\eta \,R\,v\,}where:
Fd is the frictional force – known as Stokes' drag – acting on the interface between the fluid and the particle
η is the dynamic viscosity (Some authors use the symbol μ)
R is the radius of the spherical object
v is the flow velocity relative to the object.
In SI units, Fd is given in Newtons, η in Pa·s, R in meters, and v in m/s.)

If wind forces are to be considered in the landing, there are periods during which winds will be at a maximum. These are found when a possible landing site is also the site of the sub-Solar spot or within a few degrees of it. Extreme wind-shear may be expected in the troposphere with movements toward the spot at the surface, and away from the spot toward the tropopause. The least windy times in the path or vicinity of the sub-Solar spot will be in the early morning hours.

If wind forces anticipated are sufficient to force selection of locations where these are to be minimized below a particular value, the following zones should be avoided in the selection of landing sites: 

* The sub-Solar spot.
* The Zone of Trade Winds, which are stronger somewhat south of the Equator, rather than being at a maximum over the Equator.
* The zones of Northern and Southern Westerlies.
* The zones of Northern and Southern Easterlies.

The pandorae-pretum/hellespontus warm thermal anomaly (Lat. 350S Long. 3450) where Easterly cyclonic circulation persists in a belt of prevailing Westerlies. 

In addition to these zonal winds, some effort should be devoted to avoiding a landing in major atmospheric channels, such as that of the Mars Dry Hemisphere, where winds would tend to be stronger than those over the hemisphere from longitude 2700 to longitude 900. Still further precautions may be taken to minimize tropospheric turbulence and buffeting by avoiding regions of severe thermal updraft.

Avoidance of thermal updraft may be somewhat difficult as the areas of maximum biological, geological, topographic, atmospheric, geochemical, etc. interest are the very areas in which updraft would be at a maximum. However, the severity might be reduced by choosing landing sites somewhat in the lee of such prominences.

In general, optimum landing sites, from the point of view of minimum tropospheric turbulence and wind force per unit area subsequent to landing, may be chosen in the Doldrum zones. Within this belt, the lee side of probable topographic anomalies could be further defined.

Interaction of Atmospheres with Lithospheres and Hydrospheres

Interactions may be classified as changes in the atmosphere, and changes in the lithosphere and hydrosphere. Changes in the atmosphere are a result of adding or subtracting substances, changing the size of eddies, changing the kinetics of the atmosphere, and changing the physical parameters of the atmosphere such as temperature, pressure, etc. Changes in the lithosphere are due to erosion, deposition, exchange of matter such as oxygen, nitrogen (usually through the aid of organisms), or carbon dioxide. Changes in the hydrosphere are due to addition of matter via precipitation or solution, subtraction of matter by evaporation or exsolution, friction or pressure-induced currents or changes in levels, and physical changes, particularly heating and cooling.

These processes in the terrestrial environment are understood empirically and, to an extent, analytically. Knowledge concerning the Mars environment is sufficient to provide data which can be manipulated to give at least order of magnitude parameters, which can be refined as more information concerning the environment becomes available.

As detailed in a previous paragraph, only a fraction of the atmosphere of Mars is being considered. This extends from the Stratospheric-zone through the troposphere to the immediate surface. Within this limited vertical section through the atmosphere of Mars, only features which would affect the descent, landing, deployment, and subsequent stability of the unmanned vehicle will be considered. The first of the features considered are those which are not strongly affected by relatively minor surface features.

References for the Mars dust series parts 1-3:
Norman Sissenwine  
F G Finger
M F Harris
S Teweles
Calvin E Anderson
Elmar R Reiter
F G Beuf  
F A Berry  
E Bollay  
Norman Beers  
George Ohring
Owen Cote  
Alden A Loomis  
R S Schorer  
O G Sutton
Gerard Kuiper  
Milton Klein  
Kwang Yu
Richard Harrison
Thomas F Malone
Gerard de Vaucouleurs
  

Friday, July 14, 2017

Voyage Beyond Apollo, video




Voyage Beyond Apollo video

Apollo 17, The Final NASA Voyage? (Part 1)
Director: Marie Morgan Producer: William Kurchak
Video Production: Timothy Buell

Dr. Robert Duncan-Enzmann's Conference on Planetology and Space Mission Planning aboard the cruise ship Stattendam in 1972.