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MARS Electromagnetic Sounding Experiment




Part 1
Scientific and Technical Plan


A proposal for the construction, installation and
operation of a MARSES sounding on the Mars - 2003-2005 Mission:
comparative investigation martian and earth cryolitozone
(possible investigation of subsurface relics of martian life)
and for interpretation of data.

Front Cover
"Islands" near Chryse Planitia. Teardrop-shaped "islands" are shown at the
mouth of Ares Vallis near the southern boundary of Chryse Planitia. Flow
was from the south and apparently diverged around obstacles such as craters
and low hills to form a sharp prow upstream and elongate tail downstream. A
shallow moat surrounds the entire island. Similar patterns on Earth have
been formed by catastrophic floods, wind erosion. and glacial action. From
top to bottom, the three large craters are named Lod, Bok, and Gold. [211-
4987; 21? N, 31? W] (Courtesy of NASA)



Principal Investigators:

( ( (
Yu.R.Ozorovich Stichting"InterECOS"/IKI,NL/RU(7-095-333-3177(7-095-333-
2177(yozorovi@mx.iki.rssi.ru
Experiment Manager:

( ( (
B.Zubkov IKI, RU
Co-Investigators:
V.Linkin IKI , Russia ({7}-095-333-2177 ({7}-095-333-2177 (
gotlib@iki.rssi.ru
V.Gotlib IKI, Russia ({7}-095-333-2177 ({7}-095-333-2177 (
gotlib@iki.rssi.ru
R.Rider MPIC, Germany ({49}-5556-979-439 ({49}-5556-979-149 (
@
Y. Barbin CNRS/SA, France ({33}-164-474-295 ({33}-169-202-999 (
yves.barbin@aerov.jussieu.fr
A.Ocampo JPL, USA ( (
( @
W.Smith JPL,USA
Pascal Lee, NASA Ames,USA
F.Fanale Un. Hawaii , USA ((808) 956-3149( (808) 956-
6322(fanale@kahana.pgd.hawaii.edu
R.O.Kuzmin Vernadsky Inst., RU
V. Andrianov IRE/RAS, RU
S.M.Clifford LPI,USA
R.Grard ESA/SSD, The Netherlands
S.Squyres Cornel U.,USA


Institute Addresses:

GEOPHEX 605 Mercuryy Street,Raleigh,NC 27603-2343
Stichting "InterECOS" Witmakerstraat 10, 6211 JB Maastricht,NL
CEPHAG B.P. 46, F-38402 St. Martin d'Heres, Grenoble
CNRS/SA B.P. 3, F-91371 Verrieres-le-Buisson Cedex, France
Cornell U., Center f. Radiophys. and Space Res., 424 Space Sci. Bldg.
Ithaca, NY 14853-6801, U.S.A.
DESPA CNRS, Observatoire de Paris, 92195 Meudon Cedex, France
DLR Weïling, Postfach 1116, D-82230 Oberpfaffenhofen, Germany
ESA/SSD Postbus 299, NL-2201 AG Noordwijk, The Netherlands
FMI P.O. Box 503, FIN-00101 Helsinki, Finnland
HUT Lab. of Space Techn., P.O. Box 3000, FIN-02015 HUT, Finland
IKI/RAS Profsouznaya ul. 84/32, 117810 Moscow, Russia
IRE/RAS Mokhovaya St. 11, 103907 Moscow, Russia
LPCE 3A, Ave de la Rech. Scient., F-45071 Orlùans Cedex 2, France
LPI Center f. Adv. Space Studies, 3600 Bay Area Blvd., Houston, Texas
77058, U.S.A.
MPAe Max-Planck-Str. 2, D-37191 Lindau/Harz, Germany
NDRE P.O. Box 25, N-2007 Kjeller, Norway
RST Galserwaldstr. 14, CH-9015 St. Gallen, Switzerland
U. K?ln Inst. f. Geophys. u. Meteor., Albertus-Magnus-Platz, D-50923 K?ln,
Germany
U. Leicester Dept. of Phys. and Astron., University Rd., Leicester LE1
7RH, U.K.
U. M?nster Inst. f. Planet., Wilhelm-Klemm-Str. 10, D-48149 M?nster,
Germany
U. Paris-Sud, LGDTP, Bòt. 504, U. Paris-Sud, F-91405 Orsay Cedex, France
Vernadsky Inst. Kosygin St. 19, 117975 Moscow GSP-1, Russia


Executive Summary
MARSES
MARS E/M Sounnding Experiment


Principal Investigators: Yu.Ozorovich (Stichting "InterECOS") NL/RU.
Experiment Manager:
B.Zubkov ( IKI ) RU
.

Co-Investigators:
V. Andrianov (IRE/RAS) RUS
V.Gotlib IKI RUS
V. Barbin (CNRS/SA) F
S.M. Clifford (LPI) USA
F.Fanale Uni. of Hawaii USA
R. O. Kuzmin (Vernadsky Inst) RUS
R.Rider MPICh D
V.M. Linkin (IKI/RAS) RUS
Y.Barbin CNRS/SA France
W.Smith JPL USA
A.Ocampo JPL USA
Yu.Bar-Cohen JPL USA
R.Grard ESA/SSD The Netherlands
S.Squyres Cornel U., USA
Associated scientists:


MARSES (GEM-2,3 and MARS TEM Sounding- 48,97) is sounding instruments
designed for the primary task of searching for water, water-ice or
permafrost layers believed to exist at some depth under the visible surface
of Mars. There is much evidence that water once was abundant on Mars.
There are stream lined islands formed by flowing water, flow patterns
reminiscent of wadis in Earth deserts, and outflow channels thought to have
been formed by sudden out-rush of subterranean water. Secondary tasks are
the measurement of the soil properties of the subsurface of Mars which
include porosity, electrical resistance of the liquid phase, thermal
conductivity, temperature dependence.
Estimates of Martian water ranges from a 50 to a 500 m deep planet-
wide ocean. No obvious mechanism for the escape of water from the planet
has been devised. JeanÄs escape of water via the atmosphere is very slow
(of the order of 3 m over 5 Gy). Assuming that Mars was formed with
approximately the same relative amount of water as the Earth, it must be
assumed that a substantial fraction of this water remains on Mars in one
form or another. It is commonly believed to be bound as ice in the polar
caps and, in the ground, as ice, icy permafrost or even as water. There is
also indirect evidence for widespread presence of ice, bearing permafrost
and liquid fase of water through the existence of rampart craters, terrain
softening, chaotic terrain and thermokarst.
In order to ensure the greatest possible penetration of the
electromagnetic waves into the ground the wavelength must be chosen as long
as possible.
A main task of the MARSES system is to examine changes in subsurface
properties of local areas regolith on Mars surface, and to relate them to
optical images and other remout sensing data in order to understand the
nature of different terrain forms.


The responsibility for the development of the MARSES system and for
the coordination of the modifications of the MARSES system and its
operation will rest with MPICh, with key partners in
JPL/NASA , IRE/RAS and IKI/RAS (Russia), CNRS CEPHAG and SA (France) and
ESA/SSD (the Netherlands). A brief summary of the questions addressed by
MARSES and the measurements which must be made in order to answer them is
given in the following table.

|Is there subsurface |Presence of effects the induce |
|ice/permafrost on Mars?|polarization would be evidence of icy |
| |layers. |
|What is the depth of |Determination of thermophysical |
|the layers and the |parameters subsurface. Search for several|
|nature of the layer |frequency components.. |
|transition? | |
|Does the depth vary |MARSES sounding may covers a wide a range|
|with latitude? |of latitudes |
|Do the layers and the |Comparison of properties of MARSES |
|subsurface sounding |sounding with changes in terrain and |
|correlate with visible |radar surface echo properties. |
|and radar surface | |
|features? | |
|What is the porosity |Measurement of the electrical resistivity|
|and temperature profile|subsurface layers . |
|of the subsurface | |
|lay-ers ? | |
| | |


Questions addressed Observations bearing on these question




CONTENTS

Executive Summary iii
Contents v
Acronyms & Abbrevations vii
1.0 Science Objectives 1
1.1 Subsurface Science, Introduction 1
1.1.1 Model of Mars cryolitozone 1
1.1.2 Porosity of the Surface 3
1.1.3 Regolith Temperature 3
1.1.4 On the Stability of the Ice 3
1.1.5 Rampart Crates 4
1.1.6 Terrain Softening 5
1.1.7 Summary of Objectives of the MARSES SubSurface
Observation 5
2.0 Proposed Investigations in Context of Other
Investigation 5
3.0 Technical Description of Instrument 6
3.1 Electrical Properties of the Martian Surface 6
3.2 Physical basis of the method for TEM Sounding 8
3.2.1 The main parameters TEM Device for Mars
Electromagnetic Sounding 8
3.2.2 Conclusion on Frequency Choice 8
3.3 Description of the Instrument 9
3.3.1 Requirement of the Instrument 9
3.3.2 Conceptual Design of the MARSES Instrument 9
3.3.3 MARSES Hardware Overview 9
3.3.3a MARS TEM-48,97 Hardware Overview 9
3.3.8 On Board Data Handling 10
3.3.9 The Date Rate 10
3.3.10 Data processing MARS TEM-48,97 11
3.3.11 Data Transmition to Ground
11
4.0 Data reduction and Scientific Analysis 11
4.3 Interpretation of the Data
11
4.3.1 Detection of Subsurface Discontinuities
11
5.0 Test and Calibration Plans 11
5.1 Testing 11
5.2 The Instrument Calibration and Field Testing
11
6.0 System Level Assemblyy, Integration and
Verification 12
7.0 Flight Operations 12
8.0 Team Qualifications and Experience 12
9.0 Program Managment 12
Reference 13

ANNEX I: The program for field e/m Mars sounding testing 15
ANNEX II: Active-passive microwave remote sensing
of Martian permafrost and subsurface water
15
ANNEX III: MARS TEM-48,97 Instrumentation 16
Acronyms and Abbreviations:

ABL Atmospheric Boundary Layer
A/D Analog to Digital
AIV Assembly, Integration and Verification
CEPHAG Centre d'Etudes des Phùnomønes Alùatoires et de Gùophysique
CNES Centre National d'Ùtudes Spatiales
CNRS Centre National de la Recherche Scientifique
CNRS/SA Centre National de la Recherche Scientifique/Service
d'Aeronomie
CO-I Co-Investigator
CW Continuous Wave
DDS Direct Digital Synthesis
DESPA Departement de Recherche Spatiale
DLR Deutsches Zentrum f?r Luft- und Raumfahrt
DMA Direct Memory Access
EGSE Electrical Ground Support Equipment
EISCAT European Incoherent Incoherent Scatter Association
ELISMA Etude Locale de L'Ionosphere Superieure de Mars
(electromagnetic investigation of Mars)
EM Experiment Manager
EMC Electromagnetic Compatibility
ESA/SSD European Space Agency/Space Science Department
FFT Fast Fourier Transform
FMI Finnish Meteorological Institute
GPS Global Positioning System
GSE Ground Support and test Equipment
HF High Frequency
HRR High Resolution Radar
HUT Helsinki University of Technology
IKI/RAS Space Research Institute/ Russian Academy of Sciences
IRE/RAS Institute of Radio-Engineering and Electronics/Russian
Academy of Sciences
IRFU (Swedish Institute of Space Physics, Uppsala Division)
LFM Linear Frequency Modulation (chirp)
LGDTP Laboratoire de Geologie Dynamique de la Terre et des
Planetes
LPCE Laboratoire de Physique et Chimie de l'Environement
LPI Lunar and Planetary Institute/Centre for Advanced Space Studies
LWR Long Wavelength Radar (on Mars96)
MAS Millimeter Wave Atmospheric Sounder
MDU Mast Deployment Unit
MGS Mars Global Surveyor
MIP Mutual Impedance Probe
MPAe Max-Planck-Institute f?r Aeronomie
NAIC National Astronomy and Ionosphere Center
NDRE Norwegian Defence Research Establishment
PI Principal Investigator
PLL Phase Locked Loop
PRF Pulse Repetition Frequency
PS Principal Scientist
RST Raumfahrt Systemtechnik AG
SC Spacecraft
SNR Signal-to-Noise Ratio
SOUSY Sounding System (MST radar )

1.0 Science Objectives.

1. 1 Subsurface Science, Introduction

Analysis of the ground-based geophysical cryolitozone - related
electromagnetic studies which takes into account characteristics of the
preliminary electrodynamics model of Mars cryolitozone ( this model was
based on the current geological concepts of the cryolitozone structure,
on the estimates of the ice containing material or wet fraction of
subsurface horizons at negative temperatures, on physical-chemical
transitions in the solutions of KCl , NaCl, CaCl2 with the martian
regolith and so on) - all it is shows the potential possibilities of the
Mars electromagnetic sounding in the depth interval up to one kilometer
from the planetary surface or from satellite orbit.
The presence of low conductivity screens in the section structure and bad
grounding conditions should decrease the efficiency of traditional ( or
so called vertical methods of electric sounding, or VES ) contact sounding
methods. But such screen is not a barrier for magnetic field and in these
conditions inductive sounding with controlled source should be more useful.
The usefulness of different methods of inductive sounding ( frequency
modulate or impulse ) in cryolitozone studies will be defined by the
following factors:
- cryolitozone is characterized by the relatively low conductivity of
permafrost soil of weak contrast of geoelectric section;
- the season variations of phase condition of upper and depth's layers of
Mars surface may exit;
- the high and low conductivity screens at the surface and in depth of
permafrost soil may present.
Above mentioned aspects may limit the possibilities of high frequency
sounding (HFS) method for Mars cryolitozone structure studies. The
experience in experimental studies of permafrost clay formation in the
earth's condition similar to Mars permafrost soil shows that the depth
limit of HFS methods is about 50 m.
VIKING experiments showed that Martian soil contains substantial component
of magnetic materials ( about 4%) and therefore Martian surface deposits
are belong to the soil class, completely different from lunar regolith,
which properties are widely used for attention estimates in HFS method.
Chemical composition of Mars subsurface material is characterized by the
following parameters: 40-45% SiO2, 7-7.5% Al2O3, 17-19% Fe2O3, 5-7% MgO , 5-
6% CaO, 0.4-0.7% TiO2, 6-7% SO3, 0.3-0.9% Cl and traces of K.
Chemical analysis formed the base for conclusion that 60-80% of Martian
soil material are the smectic clays mixture with different solvable salts,
such as keyserite ( MgSO4) or sodium chloride
( NaCl ). Iron oxide ( Fe2O3 ), calcytes ( CaCO3) and quarzites ( SiO2)
supposed to be present also.
Martian soils are substantially different by their properties from the pure
surface ices and gletcher ices.Relative magnetic susceptibility of the
Earth soils is close to 1 but Martian soils may have much more larger
values of magnetic susceptibility. Estimates shows that the attention in
this environment may be several orders of magnetitude larger than in ice.

Therefore even in Martian equatorial regions ( from -300 to +300 latitude
) with several hundreds of meters palagonites or montmorillonites layers
HFS method may not bring information about cryolitozone structure up to the
depth of 500 m, that is up to upper border of ice-bearing layer. In the
middle latitude region ( from 300 to 500 ) the depth upper border of
permafrost layer should be equal to 100-150 m and while in high latitudes
it may be at the surface and in this HFS method allows to measure the depth
of permafrost.
The difficulties with the estimation of attention ( that is the sounding
depth) require the comparative studies in the natural earth's conditions
close to conditions on Mars.


1.1.1 Model of Mars cryolitozone.

Mars cryolitozone formation appears to be cyclic process ( defined by
initial atmospheric composition, geological structure of the surface,
astronomical parameters of the planet and so on ) which determined current
cryolitozone structure with heterogeneous character in depth, meridional
and latitude dimensions.
Current condition of Martian atmosphere evolution are characterized by
clearly visible deficit of atmosphere saturation by water vapor in the
latitude region from - 500 to + 500.
This leads to the ice evaporation from surface permafrost layers and to
formation of dry frost soil in this latitude region above the ice
containing soil.
Photogeological analysis of the newly formed impact craters on Mars, which
excavated permafrost layers to the depths from several dozens of meters
to kilometers and form fuidized ejects, is the only method ( indirect ) of
estimation the depth distribution of Mars permafrost which is necessary for
the design of hypothetical electrodynamics model. This analysis shows that
the upper border depth interval for mean model is 150-300 m. These data are
very important for the estimation of necessary depth limit for sounding and
for the determination of dynamic range of depth, where the main changes of
phase conditions of subsurface permafrost may be observed, which have a
influence on the diffusion of water vapor into boundary layer of
atmosphere.
Let's suppose on the base of the photogeological analysis of
electrodynamics properties of permafrost and the possible phase conditions
of subsurface Martian soil layers the following cryolitozone structure for
calculation model:

1 st layer - dry frozen soil
( = 104 Om x m
2 nd layer - transition layer defined by (
= 10 - 103 Om x m
diurnal or seasonal temperature
wave
3 rd layer - permafrost
( = 103 Om x m

4th layer - salt solution with negative (
= 10 Om x m .
temperatures


Various data allow to estimate that the dry layer of frozen Mars soil may
be formed during in 3.5 billion of years period.Therefore the upper border
position of the permafrost layer may be used as specific indicator of Mars
climate evolution. Since the amount of surface moisture and its
distribution character are conditioned by the cryolitozone scale structure
its investigation is considered to be an important aspect of the
forthcoming Martian projects. In order to create Martian climate and
atmosphere circulation models the whole complex of information on surface
provided by optical and infrared observations, regional albedo surface
measurements, ground layer thermal flow investigation, etc must be
carefully studied. To that end the studies of permafrost formation global
distribution and their appearance in h ( 1 m thick layer may prove to be
essential.
The only way to obtain information about Mars's surface mezoscale
structure is to a high spatial resolution panoramic equipment onboard.
Mars' surface radioimages would allow to identify regions differing in ice
percentage content in cryogenic surface structures or in mineralized
solutions of negative temperature and to estimate the relative quantity of
cryogenic formations - permafrost fractions as well as to measure the
soil looseness or porosity degree. In additional it would be possible to
restore various regions' average vertical temperature, humidity and
porosity profiles of less 1 meter thick surface layer.
These dependencies combined with results of depth sounding (0.5 - 1 km)
and magnetotelluric ( 1 - 5 km) sensing would provide new and more
detailed information on Martian crust structure and character and its
cryolitozone necessary to create a more reliable paleoclimatic model of
the planet and possible ( or more probable ) place of the relict martian
life in the past and now.
Instrumentation on the Mariner 9, the Viking 1 and 2 missions, and more
recently on the Mars Pathfinder and the Global Surveyor together with
observations with the Hubble telescope have provided for a quite rich
picture of both the Martian surface and the atmosphere. The images have
shown a relatively dry surface with polar caps of water ice and CO2 ice
which varies with season. There is sample geological evidence that there
has been water flowing over the surface in abundance. The surface is criss-
crossed with wadi-like riverbeds, bearing testimony to past violent water
flows (Carr, 1986; Baker, 1982; Squyres, 1984). Theoretical estimates of
the permafrost thickness range from 3 to 7 km near the poles to between 1
and 3 km near the equator (Fanale et al., 1986). Liquid water should exist
under the ground ice, at least at middle latitudes. The depth to the top of
the ice layer and the transition depth from ground ice to liquid water
appear to have had significant effects on the morphology of surface
features (e.g., outflow channels, rampart craters, terrain softening).

Water may be a prerequisite for life forms in the solar system, at least
for life forms as we know them, and the search for water is a primary task
of MARSES. Hence the interest to establish the presence and properties, or
states, of the water. Life is with certainty only known to exist on our
planet. With so far only one planet, the Earth, available to define the
boundary conditions for life, it is of the greatest interest to research
the conditions on another planet, and then to determine if life is or is
not present there. This would immediately and immensely add to our
understanding and definition of the conditions for the occurrence of life.



1.1.2 Porosity of the Surface
The surface is covered by craters due to meteoroid impact which occurred
over the 4.5 Gy of existence of the planet. It is estimated that the
impact activity has crushed, redistributed and turned over as much as 2 km
of regolith, and has left a material which is porous and with a basement
which if heavily fractured (Fanale, 1976). Based on the experience gained
from seismic investigations on the moon (Binder and Lange, 1980) it is now
assumed that the porosity in the Mars regolith decreases as an exponential
function with depth but with different parameters because of the difference
in gravity and temperature: [pic]
where h is the depth below the surface. Scaling from the lunar experience
the constant K is 2.8 km (Clifford, 1981, 1984). From measurements on the
Viking landers the surface porosity is about 50 % (Clark et al., 1976), and
the self compacting depth is roughly 11 km (depth where porosity has fallen
to 1 %). This would allow a global ocean 1.4 km deep to be hidden in the
pores of the regolith (Clifford, 1984).

1.1.3 Regolith Temperature
The temperature of the interior of the Martian regolith cannot be predicted
with any precision because neither the thermal conductivity nor the
geothermal heat flux is known. It is generally agreed that the upper part
of the Martian regolith remains below the freezing temperature of water of
273 K. Such a region is often referred to as a cryolithosphere (Kuzmin,
1977). Note that we assume solute-free water and that the actual freezing
point could be lower. The mean surface temperature is low enough to keep
the water frozen at the surface at all latitudes. At some depth the
temperature is higher, and the pressure also higher, allowing water to
exist in liquid form. The exact lower boundary of the cryolithosphere is
not known. If measurements can be made of the lower boundary of the
cryolithosphere the depth can have a bearing on the solute content, the
thermal conductivity and on the geothermal flow from the Martian interior.

1.1.4 On the Stability of the Ice
Although the surface temperature is everywhere below the freezing point
of water, Viking Orbiter
Atmospheric Water Detectors indicate a global frost point temperature of
200 K. As a result of this the ground ice can only exist in equilibrium
with the atmosphere at latitudes above 40?. The cryolithosphere near the
equator therefore is desiccated to considerable depths over periods
comparable with the lifetime of the planet. The process of desiccation is
controlled by the rate at which H2O molecules can diffuse through the
regolith, which in turn depends on the nature of the porosity, i. e. the
size of the pore voids. Subsurface sounding mesurements of water vapor
content will be made from the martian surface in situ., and will provide
interesting corroborative evidence in support of this scenario.

From this very brief account of the physical/thermodynamic state of the
regolith of Mars it is clear that ice can exist close to the surface at
higher latitudes. Near the equator the ice is likely to exist only at some
considerable depth, if at all. Furthermore there is probably a lower edge
to the cryolithosphere below which the water can exist in fluid form. The
physical evidence discussed so far is not the only one to support the
notion that large amounts of water ice exists at some depth under the
surface of Mars.
[pic]
Figure 1.1 Example of the desiccation of the surface layers as a function
of time, starting with a uniform layer of ice, showing the migration of the
ice toward higher latitudes. (Fanale et al, 1986)

1.1.5 Rampart Craters
Studies of rampart craters and periglacial features suggest that a large
amount of ground ice should be present within the Martian megaregolith
(Kuzmin et al.,1988; Rossbacher and Judson, 1981; Squyres et al., 1992).
Due to sublimation processes and the porous nature of the megaregolith, the
ground ice table is covered with a dry layer. One of the most obvious
indications of volatiles at depth are provided by rampart craters.
According to Boyce (1980) and Kuzmin (1980), the minimum rampart crater
size may be an indicator of the depth to which an impact event must
excavate the regolith to reach the ground ice table. The rampart crater
distribution indicates a meridional distribution of the depth to the ground
ice table with deep ground ice at equatorial latitudes and near surface
ground ice at mid and high latitudes. The top of the ground ice layer is
found at a depth exceeding 0.3 kilometer at equatorial latitudes and 150
meters for high latitudes, with a minimum value of 30 meters in Acidalia
Planitia and Utopia Planitia. (Costard and Kargel, 1995) There is a
discontinuity in the depth of ground ice near latitude 35?-40? which might
be related to the stability of near-surface ground ice, as the soil never
reaches the frost point during the year poleward of about 40? and is
therefore in equilibrium with the atmosphere. In this case, water is always
stable as ice. These morphologic observations agree with the theoretical
calculations of the distribution of volatiles within the crust (Squyres et
al., 1992; Clifford, 1993).

Rampart crater distribution reveals that type 1 rampart craters (single
continuous and multilobate ejecta with peripheral ridges). together with
low mobility ejecta, are frequently observed in the equatorial region.
There is a good relationship between type 1 ejecta and ridged plains for
Coprates, Lunae Planum, Western Amazonis, Chryse Planitia, South Elysium
and Syrtis Major. These observations suggest that the near-surface
materials contain fewer volatiles than the underlying materials (Horner and
Greeley, 1987; Thomas and Masson, 1985). Type 2 rampart craters (double
continuous ejecta) deposit with high mobility, occur at a latitude higher
than 40?N (where ground-ice remains stable) in Utopia and Acidalia
Planitiae. The highest percentage of rampart craters occur in large
topographic basins near and below -1000 m, especially in areas that are
close to the convergent terminations of outflow channels (Costard and
Kargel, 1995).- At about 41?S, 257?W to the east of Hellas Planitia, a
regional concentration of rampart craters suggests the presence of a
volatile-rich sedimentary plain at the mouth of Harmaklis, Ma'adim and
Reull Valles. The occurrence in the same area of three channels, at a
latitude higher than 40? and within a topographic basin are optimal
conditions for the development of a permanent ground-ice (Costard, 1989).
Young volcanic units in Tharsis Montes exhibit a low density of rampart
craters, excepted for provinces surrounding Tharsis and Elysium regions.
Particularly SE Arcadia Planitia and East of Elysium exhibit an unusual
concentrations of rampart craters. The explanations proposed is the
volatile enrichment beneath the Tharsis and Elysium lavas (Cave, 1993).

[pic]
Figure 1.2 Depth to ground-ice based on study of rampart craters (Costard,
1996)

1.1.6 Terrain Softening
Both the flow of debris and the softening of the terrain bear witness to
flow or creep which can be ascribed to the viscous effect of the ice
between the grains or rocks in the regolith. In the flow patterns there
are often a steepening of the contours toward the end of the flow,
indicating that the flow pattern is deep and that the lower layers of the
flow first slow down and are partly overrun by the overlaying layers so
that a steep and sharp edge arises.

In the case of terrain softening one can imagine that the regolith, made
viscous by the presence of ice, softens sharp contours by internal flow.
The edges of craters become lower, the slopes more gentle and the diameter
larger. The central floor of the crater bulges up in the middle, the
originally concave slopes turn convex and the crater finally disappears. A
similar development would take place in the case of aeolian obscuration and
burial by debris. However, the aeolian blanketing would preferentially
soften small features rather than large ones, and there is evidence that
this is not so in the pictures obtained by Mariner 9 and from the Viking
landers.

All of what has been discussed as evidence that there is ice in the
regolith on Mars is vague and calls for direct measurement of the
interfaces between the dry regolith and one which is filled with ice in the
interstices. It also calls for measurements to look through the icy
regolith to search for the transition to the liquid phase. All of these
tasks must be addressed with MARSES.

1.1.7 Summary of Objectives of the MARSES SubSurface Observations
The important step in our study is to establish a complete history of the
volatile storage. Studying the correlations between the diameter of rampart
craters and the extension of the corresponding fluidized ejecta, allows us
to specify the depth of the ground-ice table in the megaregolith. MARSES
would permit the comparison of the actual ground ice thickness with that
deduced from rampart craters analysis. An eventual difference between the
radar echoes and the rampart crater results should give important
information about the diffusion rate of the volatiles toward the surface.

Any detection of these morphological indicators would give us some visible
records about possible subsurface volatiles. These characteristics will be
compared to the radar data, with a view to establish a possible link
between the morphology at the surface and the deeper layers of the ground
ice.


2.0 Proposed Investigations in Context of Other Investigations

The proposed investigations are connected to and have a bearing on a number
of other types of observations and on theoretical work. It relates to the
findings of the Russian Mars series of spacecraft, to Mariner, Viking and
Phobos observations. Our observations with MARSES relate in one way or
another to the following problems or observations:
Optical data by space observers of crater statistics, of shapes of impact
craters, of flow channels, modeling the thickness of the upper layered
structure crater relief, assessment of small scale structure variation over
the surface
Lander data (Viking missions, Pathfinder), investigation of similarity of
chemical composition of the soil-like materials of greatly separated
(6500 km) samples, classification of surface materials (rock, aeolian
deposited dust, sedimentary structures, crust moisture content, nature of
crust, material clotting ), estimation of their physical parameters
Microwave observations on Mars Express are designed to monitor atmospheric
water vapor, and the interpretation of these results will almost certainly
be of importance in understanding the water budget on Mars which the MARSES
experiment is designed to assess
Theoretical models of the distribution of ice, water, presence of brines in
relation to heat flux from the interior of Mars and the heat conductivity
in the surface material
Ground radar observations root-mean-square-slope estimation (2o-4o),
estimation of dielectric constant of the Martian upper layers (2-3) for
microwaves
Radio emission observations estimation of dielectric constant of the
Martian upper layers (2.34-2.70) for microwave observations

3.0 Technical Description of Instrument

3.1 Electrical Properties of the Martian Surface
The reflection, refraction and absorption of radio waves depends on the
dielectric constant ( (=('-i('') of the medium. For a homogeneous medium
the reflectivity is given by R2 = ((((-1)/(((+1)(2, the damping of a radio
signal at frequency f is given by (2(f((' tan()/c where tan(=tan((''/(') is
known as the loss tangent. The skin depth, d, for weak absorption, is given
by d = ( / ((' tan(.

Radar measurements of Mars have given values for (' of 3.5 (Pettengill et
al., 1969) for the upper layers. The dielectric constant of the first 100 m
of the Moon is thought to be related to the density, ( (in g cm-3) of the
soil by (' = (1.93(0.17)( and tan(=0.006 ( (Olhoeft and Strangeway, 1975).
Based on this (' is thought to lie between 3 and 9, and the skin depth
between 2000 and 600 m at a frequency of 1 MHz. The frequency dependence of
both (' and tan( are slight above 1 MHz and the skin depth is, therefore,
approximately proportional to wavelength (Krupenio, 1980).

For pure water ice (' ( 3.0 and tan( ( 2.1 ( 10-5 e(T /f where (=0.101(?C)-
1 and T is the ice temperature (in (C) (Paunder, 1969; Finkelshtein et al.,
1977). Assuming an ice temperature of -30?C, the skin depth becomes 2800 m.
In reality the ice will be mixed with rocks so that the above must be an
upper estimate. Finkelshtein et al., (1977) found (' = 3.7 and tan( = 0.18
for frozen earth type mountain rocks with a weight content of ice of 0.75,
at -10?C at 1 MHz leading to a skin depth on the order of 150 m. There is
also a possibility that stable brines exist on Mars (Zent and Fanale, 1986;
Kuzmin, 1983). This has an effect particularly on the loss tangent and the
depth of the liquid-solid isotherm. The latter will occur closer to the
surface than in the case of a mixture of pure ice and rocks (Andrianov, et
al., 1993; Armand et al., 1994)

Table 3.1.1 shows the skin depth for three different upper layer
compositions assuming a temperature of -60(C for the ice (there is no
temperature dependence for hard rock). The two frequencies correspond
roughly to the extremes which will be used by the radar for ground sensing.
Clearly the skin depth can vary a lot depending on the material which means
that the depth of the echoes together with their frequency dependence can
tell us about the material composition.

As described in Section 1.1, it is thought that Mars has a cryolithosphere
which may be regarded in simple terms as a top layer of "dry frozen rock"
above a layer of frozen icy rock (Kuzmin, 1983). The "dry" layer is thought
to be 10-40 m deep at high latitudes and 300-400 m deep at low latitudes.
The "icy" layer is believed to be 600-2500 m at high latitudes and 500-
800 m deep at the equator. Below these layers there may be wet rock and
possibly even liquid water. A radar in the MHz band should therefore be
able to penetrate the dry upper layers to maybe several kilometers, and
perhaps a further few hundred to thousands of meters into any "icy" layers.

Table 3.1.1 Values of dielectric constants with penetration depths at 5 MHz
| |Hard rock |Fresh ice |salty (2%) ice |
|Paramet|('|(''|tan(|d |(' |('' |tan(|d |(' |(''|tan|d |
|er | | | | | | | | | | |( | |
|f, ( | | | |(m( | | | |(m( | | | |(m|
| | | | | | | | | | | | |( |
|f=0.5MH|5 |0.5|0.1-|200-|3.1|2.10|5.10|2000|3.9|1.1|0.3|80|
|z | |-0.|0.01|2000|6 |-3 |-4 | | |8 | | |
|((=600m| |05 | | | | | | | | | | |
|) | | | | | | | | | | | | |
|f=5 |5 |0.5|0.1-|20-2|3.1|2.10|5.10|2000|3.3|0.1|0.0|60|
|MHz | |-0.|0.01|00 |6 |-4 |-5 | | |5 |4 | |
|((=60m)| |05 | | | | | | | | | | |

As a simple model of the multiple layer structure we take a uniform double
layer where the top layer has a complex dielectric constant (1 and depth L,
and the underlying layer has a complex dielectric constant (2. In this case
the reflectivity takes the form
[pic]with [pic] and [pic] where ( is the phase path through the upper layer
and back. The reflection coefficients are defined as in the case of a semi-
infinite half space as: [pic] and [pic]

It is clear that the reflection coefficient of the double layer can exhibit
oscillations with frequency, that the depth of these oscillations depends
on the depth of the layer and the amount of attenuation in the top layer.
Fig. 3.1.2 shows the reflection coefficient as a function of frequency for
a fixed value of L=100 m and for (1=4 and two cases of (2. The solid line
is for (2=6 and the dotted for (2=3, which are possible values of the
dielectric constant for the Martian ground. The values of tan( are of the
order of 0.001 implying low attenuation. One can regard the curve in
Fig. 3.1.2 as the result of interference between reflections from two
layers which explains why the technique of using multiple frequencies to
measure depth is sometimes referred to as interferometry. In the short
pulses which we intend to synthesize the layers would show up as discrete
scatterers at ranges corresponding to the depth of the layer transitions.

[pic]Figure 3.1.2 Variation of reflectivity with frequency when dielectric
constant of the lower layer is larger than the upper layer (fully drawn)
and when it is lower (dotted).

For large radar wavelengths, the limiting value of R2 is R2 = ((((-
1)/(((+1)(2, [pic]. For short radar wavelengths, assuming sufficient
absorption, the reflection is determined by the top layer, and the
reflection takes the same form, except that (2 is replaced by (1. In
practice such clear-cut oscillations such as in Fig. 3.1.2 may not be
observed because there may be a gradual transition of electrical properties
with depth or more than one internal interface. In addition the depth of
the layer or the electrical properties may vary over the lateral area
sampled by the radar. Therefore, in order to measure curves like that of
Fig. 3.1.2 it is necessary to step through the frequency band in as short a
time as possible to minimize the lateral extent of satellite motion over
the surface.

3.2 Physical basis of the method for TEM Sounding.

In the TEM sounding the transmitter and receiver coils are used when the
current is switched on or off in the transmitter coil the field induces
inside the surface eddy currents which in turn induce secondary voltage in
the receiver coil. For the homogeneous half-space ( in the near zone ) the
induction voltage in the receiver coil is given by

E(t)= I x Q x q ( ( ( ) -3/2 ( (/ t )5/2/ 20 (1)

where Q,q - the surface of a transmitter and a receiver coil (m2)
respectively,
( = 1/( - resistivity ( 1/ (m),
( - magnetic susceptibility.
In this case the sounding depth ( the skin-layer thickness ) can be
estimated as
( ~ 2/( t x ()1/2= Z
On the Earth the minimum received signal may be ~ 10 (V, on the Mars where
industrial noices are absent it can be order of magnitude less, this allows
sounding more deeply.
The sounding in the near zone imposes the limitation on the dimension of
the coil :
R ( coil) ~ (

3.2.1 The main parameters Transient Electromagnetic Device for Mars
Electromagnetic
Sounding

Before we must to stay the necessary dependencies between of the sounding
time t ( (s ), the level of signal in the receiver coil E ( (V) and the
depth of sounding Z (m), which it will be estimate on the base the skin-
layer thickness.
This dependencies is :
E(t)= 1.6 x 104 x ( I x Q x q ) x ( (2 t5)-0.5 , ( 4 )
t = 50 x ( I x Q x q/E )0.4 x (-0.6 , ( 5 )
Z = 7 x ( ( x I x Q x q / E ) 0.2 .( 6
)
The formula (6) which allowed to detect the depth of sounding on the base
dates about the mean resistivity of underground geological structure and
the level of the signal in the receiver coil E ( t ), and (5) will allowed
the perpetrate time of sounding.
As illustrated the model, with the availability the frozen salinity
solution on the depth 400 m , the value of (( slopes down until 100 ( x m
.
This value was adopted as the mean resistivity of a sectional geological
structure and to set the value of Emin= 10 (V. It is reasoned that our
transmitter and receiver coil will have 10 - turns with
R= 10 m and I= 10 A.
When from (5) and (6) it's founded that tmax= 1907 (s, and Zmax= 440 m.
If we are defined as tmax=2000 (s and to give the value of ( from
dependencies with index 10-2 and 10-3 ( 300 and 170 ( x m, respectively
), it is allowed to determine the level of signal E = 1.7 and 4 (V, and
depth Zmax = 775 and 583 m, respectively.
In such a manner the min level of signal in the receiver coil must to
select in order to 1 (V.
The equipment for transient electromagnetic sounding consist of
transmitter and receiver. Transmitter generates in a wire loop a sequence
of rectangular current pulses with intensity 1-10 ( and more ) amperes.
Magnetic field generated by this currents which flow in any conductors
inside the earth.
These eddy currents set up a secondary magnetic field which is registered
by a receiver loop. Since the eddy currents don't case instantly after
transmitted current is switched off, but decay gradually, their presence is
discovered by the transient voltage that they induce in the receiver coil.
So,the recording of these "transients" is a means of detecting conductors
in the earth. The better conductor , the more voltage and the longer this
transient. The decay process can be measured by a recorder at various delay
times. The importent advantage of TEM technology over continuous e/m wave
systems is fact that the measurement are taken when the transmitter is
switched off.
The depth of investigations depends on the loop's size L, current intensity
I, receiver's sensitivity, maximal delay time, subsurface soil resistivity
R0.
The common image of the calculation depths gives the next Table:
____________________________________________________________________________
____
L,m :
R0

: 3 10 30
100 300
____________________________________________________________________________
____
12.5
34 43 53 68 84
25.0
58 74 93 118 147
37.5
81 103 128 163 203
50.0
102 129 161 205 255
____________________________________________________________________________
____
Field work experiance shows that in favorable conditions modern TEM
instruments provide depth sounding range from 3 m - 300 m.

3.2.2 Conclusion on Frequency Choice
The conclusion to be drawn from the discussion in Sections 3.2-1 and 3.2-2
is that the frequency must be chosen as low as possible.
We are, therefore, striving to make observations of the surface in the
band up to 1 MHz and design the MARSES system accordingly.

3.3 Description of the Instrument

3.3.1 Requirements of the Instrument
From the discussions in the previous sections it is clear that the
instrument must be a long wavelength radar operating at frequencies below
1 MHz if possible. In order to probe the subsurface structure with a depth
resolution sufficient to resolve, or discriminate layers of about 100 m
thickness, as some of the models of the subsurface imply may be present,
the bandwidth must be about 1 MHz.

3.3.2 Conceptual Design of the MARSES Instrument
From the discussion in Section 3.2 it is clear that the frequency of the
sounding system must be chosen as low as possible in order to ensure
penetration of the waves to sufficient depths.
On the other hand in order to identify the depth of layers to an accuracy
on the order of 100 m the bandwidth of the signal must be at least 1 MHz.
The relative bandwidths of the signal, therefore, becomes very large.

3.3.3 MARSES Hardware Overview
3.3.3a MARS TEM-48,97 Hardware Overview

Figure 3.1.1 shows a block diagram of the MARS TEM-48,97. There are
basically two main elements, the antenna and the electronics box. Here we
summarize the function of each sub unit.
[pic]Figure 3.1.1 Block diagram of the MARS TEM-48,97







The antenna consists of two identical concentric transmitter coil and
receiver coil. Each of these is connected to the electronics box by twisted
pair.

|Unit |Mass |Power |Size |Comments |
| |[kg] |[W] |[cm3] | |
|Electronics Block |0.4 |0.2 |245 | |
|(With box and | | |(7*14*2.| |
|connectors) | | |5) | |
| | |24 | | |
|Pulse generator | | | | |
|(activ) | | | | |
| | |0.0 | | |
|Pulse generator | | | | |
|(passiv) | | | | |
| Pulse generator | |2.4 | | |
|(activ 10%) | | | | |
|Antenna system |0.5 |0.0 |300 |R=6 Ohm |
|(d=0.3mm, L=15m) | | | | |
|Total |0.9 |2.6 |545 |Pulse generator |
| | | | |(activ 10%) |


3.3.8 On Board Data Handling

3.3.9 The Data Rate
The primary output of the MARSES are the complex dependence of the
subsurface parameters.


The Maximum data is estimated from the following parameters:

Maximum MARS TEM Device data file : 256 000 bits


The above estimate excludes some status information concerning the MARSES
parameters which would only need to be sent much less often. For example,
time, attenuator value, transmitter current and voltage, command
information which would contain frequencies and pulse lengths and pulse
separations need to be sent at regular intervals.



3.3.10 Data processing MARS TEM-48,97
The data processing includes two stages. First stage (during field
measurements ) includes preliminary processing. During this stage, TEM-
FAST Pro System stacs the data of measurements, determines the noise level
and precision of measurements, permits to operate fit the parameters of the
System to optimize the process of sounding and following interpretation.
Second stage consist of the determination of martian subsurface structure.
There are two class of models which can be found: layered section and
gradient smoth section. Depend on data quality and preliminary geological
information one can find the electrical conductivity distribution verses of
depth
which depend on the rocks properties, water contents, temperature,
salinity, porosity and other parameters of the section consideration.

3.3.11 Data Transmission to Ground
The data file of 256 000 bits estimated above could be transferred to the
spacecraft memory by the envisaged MIL-STD-1553 B low data rate bus
(<100kbps). In the event of using the monopulse technique with twice this
rate we will have to store the data in the experiment memory before
transferring to the spacecraft and to the ground.

4.0 Data reduction and Scientific Analysis

The data analysis and interpretation of the data will depend on several
different data sets derived from the observations:
Sounding curves as a function of time delay for detection of layered
structure
Reflected power as a function of frequency, which gives rise to periodic
variations in reflectivity if there is a discrete layer present

4.3 Interpretation of the Data

4.3.1 Detection of Subsurface Discontinuities
Consider a preliminary analysis of the sounding dates from the point of
view of solving the inverse radar sounding problem i.e. a determination of
parameters of a subsurface soil layer.


5.0 Test and Calibration Plans

5.1 Testing
All the instrument sub-systems will be tested by the producers. Producers
of the sub-systems will perform thermal and vacuum tests. After extensive
checking and tests individually the sub systems will be brought together,
assembled as a complete system and tested at JPL,IKI under the supervision
of the EM. After integration the whole instrument is tested with a complete
testing cycle:
vibration test
thermal test
vacuum test
EMC test etc.
The resistance to radiation will be confirmed by calculation.

To test the digital processing unit ground test equipment will be built.
Such equipment was built for the Mars96 processor (TMS 320C30) at IKI. This
equipment and the software modules is available for re-use to the extent
allowed by the new design.

The instrument performance verification and integration to the spacecraft
will be done at the spacecraft manufacturer.

5.2 The Instrument Calibration and Field Testing
At the IKI/JPL testing and calibration MARSES instrument will be carried
out using the engineering or spare instrument model. The measurement
results will be processed with the developed software and simulation
models. Also these results will be compared with simultaneous soundings
from a another methods.


6.0 System Level Assembly, Integration and Verification

The System Level Assembly, Integration and Verification (AIV) of the MARSES
instrument should be carried out in accordance with pre-launch AIV
programme at spacecraft system level. During AIV the following will be
checked: power consumption, reception and implementation of all commands,
data production, transmission of the telemetered parameters and any special
requirements of the instrument.


7.0 Flight Operations

Operation of MARSES is primarily to obtain sounding subsurface layers which
dictates the main flight operations.The operational concept of the MARSES
experiment is based on:
New Multifrequency Electromagnetic Sensor :
A. Small rover HFS (high-frequency sounding) with Antenna size ( 0.5 m.
B. Small station HFS sounding with Antenna size ( 0.5 m.
and Low-frequency sounding MARS TEM-48,97 for main operational modes:
A. Penetrate probe with Antenna size ( 100 m.
B. Small rover MARSES Sounding with Antenna size ( 50 m.
C. Small station MARSES Sounding Antenna size ( 5 m.


8.0 Team Qualifications and Experience

Key Personnel


The qualification and experience of the team members are listed in the
attached list of CV's. Further details of the experience of the PI's and
the Experiment Manager can be found in the next section. The relevant
experience of the team members is summarized and two publications of
importance for the project are references with each.

8.1 Curriculum Vitae and Publications of Team Members

Principal Investigators

Ph.D. Yu.R.Ozorovich: Executive Director Stichting "InterECOS" since
1990; Senior Research Scientist IKI since 1979.
Ozorovich Yu.R. , et al, Tentative of e/m ( low-frequency ) sounding of
the cryolitozone of Mars, Preprint IKI,No.1477, 1988

Co-Investigators:




9.0 Program Management

InterECOS/JPL will have the responsibility for the coordination of the
implementation of the instrument and for the analysis and distribution of
the data to the science team members.


There will be a responsible Lead Scientist in each national group who will
communicate with the PI through the Project Manager on matters relating to
the instrument development. The science team will interact directly with
the PI. There will be regular project meetings to discuss the development
of the instrumentation and to plan for the data taking, reduction and
analysis. Smaller working groups will be formed to solve specific task
arising in the course of the project. It is expected that there will be a
certain dynamism in the make-up of the team, with younger members entering
and older retiring to Co-I or Associated Scientist status.









References

Andrianov, V.A., Subsurface radar remote sensing of inhomogeneous ground
of a planet, Proc. Of the IEE Int. Conf. ``RADAR 92ÄÄ, Brighton, UK, 12-13
Oct., 365, 458 - 460, 1992
Andrianov, V.A., Subsurface radar of the layered - inhomogeneous soil of
a planet, J. Comm. Techn. a. Electronics, 38(5), 16 - 27, 1993, (Translated
from: Radiotekhnika I electronika, 37(11), 1937 - 1938, 1992)
Andrianov, V.A., I.N. Kibardina, R.O. Kuzmin, Deep structures of the
dielectric permittivity of the Mars cryolitorphere, Astronomicheski
vestnik, 27(6), 1-11, 1993
Andrianov V.A., N.A. Armand and O.V.Yushkova, Influence of conditions of
the radiowave propagation on subsurface radiolocation of soil of planets,
Proc. of the IEE Int. Conf. ``RADAR 97ÄÄ, Edinburgh, UK, 14-16 Oct., 449,
316-318, 1997
Armand, N.A., V.A. Andrianov and D. Ya. Shtern, The method of
determination of dielectric permittivity of planet ground, Patent # 2 002
272 ( 17 08 92 ), Bulletin of inventions, 40, 152, 1992
Armand N.A., et al., Dielectric permittivity of Mars ground at various
saline compositions of ice, Proc. of the Int. Working Meeting on
Comparative Planetology (Brown-Vernadsky Microsymp. XX), Moscow, 20, 11-12,
1994
Armand, N.A., et al., The long wavelength radar for Mars surface and
ionosphere probing, Proc. of the IEE Int. Conf. ``RADAR 97ÄÄ, Edinburgh,
UK, 14-16 Oct., 449, 819-822, 1997
Axford , W.I., A commentary on our present understanding of the Martian
magnetosphere, Planet. Space Sci., 39,167-175,1991
Baker, V.R., The Channels of Mars, Austin : University of Texas Press,
1982
Barlow, N.G. and T.L. Bradley, Martian impact craters : correlations of
ejecta and interior morphologies with diameter, latitude and terrain,
Icarus, 87, 156-179, 1990
Binder, A.B. and M.A. lange, On the thermal history of a moon of fission
origin, JGR, 85, 3194-3208, 1980
Boyce, J.M., A method for measuring heat flow in the Martian crust using
impact crater morphology,NASA TM-80339, 114-118, 1980
Carr, M.H., Mars : A water-rich planet?, Icarus, 56, 187-216, 1986
Cave, J. A., Ice in the northern lowlands and southern highlands of Mars
and its enrichment beneath the Elysium lavas, J. Geophys. Res.,98, 11079-
11097, 1993
Clark, B.R. and R.P. Mullin, Martian glaciation and the flow of solid
CO2, Icarus, 27, 215-228, 1976
Clifford, S.M., A pore volume estimate of the Martian megaregolith based
on a lunar anal, in ``Third Int. Coll. On MarsÄÄ, LPI Contrib. 441
Abstracts,46-48, 1981
Clifford, S.M., A model for the climatic behavior of water on Mars, PhD
Thesis, U. Michigan, 1984
Clifford, S.M., A model for the hydrologic and climatic behavior of water
on Mars, J. Geophys. Res., 98, 10973-11016, 1993
Coldberg, B.G., Digital frequency synthesizers, Englewood Cliffs, NJ
?Prentice Hall, 1993
Costard, F.M., The spatial distribution of volatiles in the Martian
hydrosphere, Earth, Moon and Planets, 45, 265-290, 1989
Costard, F. and J. Kargel, Outwash plains and thermokarst of Mars,
Icarus, 114, 93-112, 1995
Fanale, F.P., Martian volatiles : Their degassing history and geochemical
fate, Icarus, 28, 179-202, 1976
Fanale, F.P., et al., Global distribution and migration of subsurface ice
on Mars, Icarus, 67, 1-18, 1986
Finkelshtein, M. I.., V. L. Mendelson and B. A. Kutev, The Earth sub-
surface radar investigation, Sov. Radio, 174, 1977
Horner, V.M. and R. Greeley, Effects of elevation and ridged plains
thickness on Martian crater ejecta morphology, Proc. Lunar Planet Sci.
Conf. XVII, J. Geophys. Res. Suppl., 92, E561-569, 1987
Krupenio, N. N., Radio investigation of the Moon and Earth-group planets,
Review of recent results in science and technology, Series Astronomy AN, in
Russian, 18, 1980
Kuzmin, R.O., Questions of the structure of the Martian cryolithosphere,
in ``Problems of CryolithologyÄÄ, Moscow University Press, 6, 7-25, 1977
Kuzmin, R.O., Morphology of fresh Martian craters as an indicator of the
depth of the upper boundary of the ice-bearing permafrost : A photogeologic
study, Lunar Planet. Sci. Conf. XI Abstracts, 585-586,1980
Kuzmin, R. O., Martian cryolithosphere, Nauka Press, Moscow, (in
Russian), 140, 1983
Kuzmin, R.O., et al., Mars : estimation of the relative ice content in
upper layers of the permafrost, Lunar Planet. Sci. Conf. XIX Abstracts, 657-
658, 1988
Mouginis-Mark, P.J., Martian fluidized crater morphology : Variations
with crater size, latitude, altitude and target material, J. Geophys. Res.,
84, 8011-8022.
Nielsen, E., et al., The "Long Wavelength Radar" on the Mars94 orbiter,
Adv.Space Res., 15(4), 163-178, 1995
Olhoeft, G. R. and D. W. Strangeway, Dielectric properties of the first
100 meters of the moon, Earth and Planetary Science Letters, 24, 394, 1975
Ozorovich Yu.R. et al, Martian Balloon Experiment: Possibilities
investigation cryolitozone of Mars by e/m sounding, Preprint
IKI,No.1420,1988.
Ozorovich Yu.R.,et al, Tentative of e/m sounding (low-frequency) sounding
cryolitozone of Mars, Preprint IKI, No. 1477,1988.
Ozorovich Yu.R., et al, Microwave remote sensing of Mars surface
parameters, Preprint IKI, No.1531, 1988
Paunder, E., The physics of ice, MIR, Publ. H., 189, 1969
Pettengill, G., et al., Radar measurement of Martian topography, Astron.
J., 74, 461, 1969
Jakosky, B.M. and D.O. Muhleman, A comparison of the thermal and radar
characteristics of Mars, Icarus, 45, 25-38, 1981
Shtern, D., et al., Long wavelength radar LWR RKL-M, Users's Manual, Max-
Planck-Institut f?r Aeronomie, 1996
Squyres, S.W., The history of ater on Mars, Ann. Rev. Earth Planet.
Sci., 12, 83-106, 1984
Squyres, S.W. et al., Ice in the Martian regolith, in ``MarsÄÄ, (H.H.
Kieffer, et al., Eds.), The University of Arizona Press, 523-554, 1992
Thomas, P. and Ph. Masson, Martian fluidized crater distribution :
tectonic implications, Earth, Moon and Planets, 34, 169-176, 1985
Zent A.P. and F.P. Fanale, Possible Mars brines : equilibrium and kinetic
considerations, J. Geophys. Res., 91(B 4), D 439 - D 445, 1986
Won I.J., GEM-2: A New Multifrequency Electromagnetic Sensor, JEEG,
V.1,Issue 2, 129-137, 1966




ANNEX I:

THE PROGRAMM FOR FIELD ELECTROMAGNETIC MARS

SOUNDING TESTING.

According to general program of MARS-2003-2005 experiments, there will be
two kind of equipments for soundings:"high freguency" radar and "low
freguency" TEM (Transient Electromagnetic) sounding. Really,both of the
instruments are operating in time domain.Radar operates in the range of
times: 100 ns throughout 1000 ns and TEM instrument in the range 3-4 (s
throughout 300-500 (s. Radar uses permeativity as the main parameter of
media and TEM uses conductivity.
The main objective of the experiments is to construct the section of
Martian cryolitozone till the depth of order of tenths and first hundreds
meters.Both of the equipments are ready and have been tested in Earth's
conditions.
The main objective of this field experiment is the equipment testing, and
analysis of their possibilities in the conditions close to Martian ones.
According to today understanding of Martian rocks properties, one can wait
that typical rocks which compose Martian cryolitozone are poligonites and
montmorolinities till the depth of order of first several hundreds meters.
These rocks are not typical for Earth that is why it is necessary to test
both sounding ways.
There several of regions where some of the parameters are close to Martian
conditions:
Antartic, Iceland, Hawaii ( volcanic area ).
Below there is short formulation of the main points of field experiments
for both of the
equipments ( complex testing ).

RADAR EQUIPMENT
1. The estimation of maximal depth of sounding and resolution of radar-
sounding in the
conditions rocks close to Martianes ones.
2. The determination of influence of local inhomogeneties ( relief ) on
sounding results.
3. The estimation of influence of antennae configuration on the field
results.
4. Correction of technology of measurements and of software.

TEM EQUIPMENT
1. The estimation of maximal depth of sounding and resolution of TEM-System
in the
conditions of rocks close to Martian ones.
2. The determination of influence of antennae configuration on the results.
3. The determination influence of local inhomogeneities on sounding
results.
4. An investigation of the possibility to separate superparamagnetic (SPM)
layers in the massive of rocks.
5. An investigation of possibility to investigate underground water
component
using induced polarization ( IP ) effect.
6. Investigation of optimal configuration of antennas and device for
registration
of IP-effect and SPM- effect and of their separation from induction
effects.
7. Modification of instrument, hardware and software according to field
studies
and to creat new instrument, hardware and software for applied studies
in the
earth's conditions, include environmental and geophysical studies.



ANNEX II:

ACTIVE-PASSIVE MICROWAVE REMOTE SENSING OF MARTIAN PERMAFROST
AND SUBSURFACE WATER.

The existance of a large Martian cryolitozone consisting of different
cryogenic formations both on the surface- polar caps ice and in subsurface
layer ( and probably overcooled salt solutions in lower horizons) is
conditioned mostly by the planet's geological history and atmosphere
evolution. The very structure of the cryolitozone with its strongly
pronounced zone character owing to drying up of 0 to 200 m thick surface
layer in the
equatorial latitudes ranging from + 30 to - 300 was formed in the course
of long-periodic climatic variations and at present is distincly
heterogeneous both depthward and in latitudinal and longtudinal dimensions.
The dryed up region of Martian frozen rocks is estimated to have been
developing during more than 3.5 bln years, so the upper layer boundary of
permafrost can serve as a sort of indicator reflecting the course of
Martian climatic evolution.
Since the emount of surface moisture and its distribition character are
conditioned by the cryolitozone scale structure its investigation is
considered to be an important aspect of the forthcoming Martian projects.
In order to create Martian climate and atmosphere circulation models the
whole complex information on surface provided by optical and infrared
ranges observations, regional albedo surface measurements, ground layer
thermal flow investigations, etc. must be carefully studed.
To that end the investigation of permafrost formation global distribution
and their appearance in h ( 1 m thick layer may prove to be essential.
Along with optical and infrared observations the method of orbital
panoramic microwave radiometry in centi- and decimeter ranges would
contribute to the mapping of the cryolitozone global surface distribution.
This ANNEX II discusses methodical and experimental possibilities of this
global observation of Martian
cryolitozone as the additional way for investigation subsurface of Mars.
Mars' observations by means of ground and on- board instruments are known
to have been conducted in recent years. These observations provided
information on Mars' surface mean temperature values and their seasonal
variations. Radar measurements allowed to estimate dielectric constant and
soil upper layer density values.
Mars' surface radiation measurements by a 3,4 cm radiometer aboard Mars-3
and 5 automatic interplanetary stations (1971-1973) proved to be more
informative. Radiobrightness temperature variations were registered along
the flight route.
As a result surface temperature latitudinal distribution estimates in a
spatial resoulution element, were obtained
as well as more precise values of dielectric constant and soil density of
centimeter fractions thic surface layer.
No more experiments using microwave radiometers were conducted since.
The only way to obtain information about Mars surface mezoscale structure
is to use a high spatial resolution panoramic equipment on-board. Mars'
surface radioimages would allow to identify regions differing in ice
percentage content in cryogenic surface structures or in mineralized
solutions of negative temperature and to estimate relative quantity of
cryogenic formations - permafrost fractions as well as to measure the soil
looseness
or porosity degree. In addition it would be possible to restore various
regions' average vertical temperature,
humidity and porosity profiles of less than 1 metre thick surface layer.
These dependencies combined with the results of depth inductive sounding (
0.5 km ) and magnitotelluric ( 1- 5 km ) sensing would provide new and
more detailed information on Martian crust structure and character and its
cryolitozone necessary to create a more reliable paleoclimatic model of the
planet.
Experiment equipment and methods
Space experiment is conducted to obtain maps of temperature and humidity
global distribution of Martian cryolitozone upper layer by means of
radiothermal images of the surface. Analysis of the available data produces
estimates of the soil integral content, degree of salt solutions
mineralization and porosity. Regions of permafrost and ice formations are
identified as well. One could possibly estimate average profiles of
temperasture, humidity and porosity of a 0,5-1 metre thick surface layer.
For that purpose one should apply observations
by a two-channel scanning radiometer of centimetre and decimetre ranges.
Fluctuational sensitivity of each channel is ( 0,10 K, time constant of
integration is 1 s. The two channels share an antenna, an inflatable or
self-opening one with a mechanically scanning beam; aperture is about 3-4 m
in size; directivity diagram - 30. Spatial resolution element ( pixel ) is
about 20 km, observation belt is of 200 -
400 km depending on the orbit parameters. Restoration accuracy of the
radiobrighness temperature absolute
values is of order of 2-30K. Microwave block dimensions are up to
500x500x300 mm; weight is ( 10 kg.
Antenna fastening and joint to microwave block are hard. Registering system
is a digit tape-recorder. Information stream is up to 1 kb/s. Power
consumption is up to 50W/27V. Radiometer observations are conducted along
the route of the Martian orbital station in accordance with the experiment
general program. Observation angle is ( ( 0-300 ; polarization is vertical.
Frequency of the radiometer calibration is not less that once in 24 hours.
Radiometer scale calibration and measurement of antenna-feeder unit
transition coefficient can be carried out against standard sources as well
as the relict radiation (( 30K ) with the antenna proper orientation.
Generally it is desirable to match the radiometer system observation zone
with that of optical and TV systems and infrared radiometer as well.
Martian surface radioimages should be geographically identified. Data
processing and temperature and humidity maps drawing is performed by
processor system back on Ground.
( From: Ozorovich Yu.R., Raizer V.Yu., Microwave remote sensing of Martian
cryolitozone, Preprint IKI,
No.1768, 1991)



ANNEX III: MARS TEM - 48,97 Instrumentation
The main characteristics of the equipment are as follows:
MARSES TEM - 48,97
Transmission:
current switch on time ( us)
( single loop 25x 25 mxm,I=1A) less than 100
current switch off time ( us)
(single loop 25x25 m * m, I=1A) less than 3
- current output (A) 1 or 3 (selectable)
-Period of repetition current pulses (5/16...5*16)
(s (selectable)
-current times on/off 3/1
-coil resistance limits (Ohm) 0.1-20
-coil inductance limits (uH) not more than 500

Detection:
- Band width (MHz) not less than 2
- No. of sampling channels 16 or 48 (selectable)
- minimum analysis time delay ((s) 4
- maximum analysis time delay (msec) 16
- maximum Number signal averaged 32-92,160 (selectable)
- voltage resolution (uV) 0.125
- instrument noise (uV) 0.05
- noise 50/60 Hz filtering (dB) better than 60
- input voltage range(V) 1e-7...5

- measurement units:
- E.M.F/current V/A
- errors of measurements V/A
- systematic errors without external noise (%) less than 0.3

Types of loops configuration:
coincident (one wire) or dual (two wires)
- available transmitter coil (m*m)
(0.1*0.1)...(100*100)
Measurement time (minutes) 0.2-22 ( selectable )

Power supply:
- internal rechargeable lead-acid batteries
- voltage (V) 12
- capacity (A*h) 2
- available operation time (h) 8-10
- external power supply optional

Output & terminal
- any IBM compatible computer with standard RS 232 interface

Weight (kg):
- with lead-acid battery, 12 V, 2 Ah less than 2
- Dimension (mm) 330x100x30
- Temperature range -15 + 50 0C
- Temperature changing rate (0C/min) less than 5

-----------------------
MARSES

[pic]

Frequency (MHz)

[pic]

[pic]

[pic]

PI. ,
Yu.R.Ozorovich
( UA,
Stichting InterECOS)

Experiment Manager

B.Zubkov
(UA,IKI)


System architecture and engineering
(CH, F, D, NL, RUS)

D
(MPICh)
CO-PI. R.Rider
Integration (+ RUS)
Power supply
GSE-digital part

RUS
(IRE, IKI)
CO-I. V.Linkin
Ant, Match unit,
Tx, Rx, GSE, Rad Contrl, Integration


NL
(ESA-SSD)
CO-I. Grard
Antenna Conf.
(Processor, A/D, Synth, Interface)

F
(CEPHAG/SA)
CO-I. Y.Barbin
Radiometer
System design

USA
CO-I.V.Raizer
Radiometer
System design



USA
(JPL)
Intergration,
Testing,Colibra
tion.

Science team, CO-I's
Finland France Germany Norway Russia USA United Kingdom
Data analysis

Instrument Engineer
(to be decided)


Implementation level

NASA

Satellite manufacturer

NASA level