. 

SCIENTIFIC RESULTS OF THE 

PROJECT ON 

MARS: EVQLUTION OF ITS 

CLIMATE AND AThaOSPHERE 

NASA23PONSORED STUDY 

MECA 

(NASA-@$- K~/~&?SCIENTXPIC EESULTS OF THE 

NBSA-SPCISORED SSEDY PBOJEC'L C6 EARS: 

EVCLUTICN OF IT2 CLIRAIE AHC A'ItCSPHERE 

(hASA) 36 F CSCL 03B Unclas 

18 9- 1 50 5 9 

G3/91 0170241 

LPI Technical Report Number WHO9 

LUNAR AND PLANETARY INSTITUTE 3303 NASA ROAD 1 HOUSTON, TEXAS 77058 
I SCIENTIFIC RESULTS OF THE NASA-SPONSORED STUDY PROJECT 

ON 

MARS: EVOLUTION OF ITS CLIMATE AND ATMOSPHERE 

Stephen M. Clifford 

Lunar and Planetary Institute 

3303 NASA Road 1 

Houston, TX 77058 

Ronald Greeley 

Department of Geology 

Arizona State University 

Tempe, AZ 85287 

Robert M. Haberle 

Mail Code 245-3 

NASA Ames Research Center 

Moffet Field, CA 94035 

Lunar and Planetary Inst it ut e 3303 NASA Road One 

LPI Technical Report Number 88-09 

Houston, Texas 77058-4399 I 

I 
Compiled in 1988 by the 

LUNAR AND PLANETARY INSTITUTE 

The Institute is operated by Universities Space Research Association under 

Contract NASW-4066 with the National Aeronautics and Space 

Administration. 

Material in this document may be copied without restraint for library, abstract 

service, educational, or personal research purposes; however, republication of 

any portion requires the written permission of the authors as well as appropriate 

acknowledgment of this publication. 

This report may be cited as: 

Clifford S. M., Greeley R., and Haberle R. M. (1988) Scientifi Results of the 

NASA-Sponsored Study Project on Mars: Evolution of its Climate and Atmosphere. 

LPI Tech. Rpt. 88-09. Lunar and Planetary Institute, Houston. 33 pp. 

Papers in this report may be cited as: 

Author A. A. (1988) Title of paper. In Scientific Results of the NASA-Sponsored 

Study Project on Mars: Evolution of its Climate and Atmosphere (S.M. Clifford, 

R. Greeley, and R. M. Haberle), pp. xx-yy. LPI Tech Rpt. 88-09. Lunar and 

Planetary Institute, Houston. 

This report is distributed by: 

ORDER DEPARTMENT 

Lunar and Planetary Institute 

3303 NASA Road One 

Houston, TX 77058-4399 

Mail order requestors will be invoiced for the cost of shipping and handling. 
Project Summary 

Science Report 

Appendix 1. Origin of MECA 

Appendix 2. MECA Membership List 

Appendix 3. MECA Bibliography 

1 

3 

13 

15 

21 
1 

Project Summary 

The principal scientific finding of the MECA study project is that Mars had a substantially “wetter” early history than previously thought. This realization is derived 

from several lines of evidence, including various geological arguments and geochemical 

models based on the composition of the SNC meteorites (which many investigators 

believe may be samples of Mars). 

The research suggests that Mars has outgassed the equivalent of a global Ocean of 

water 0.5-1.0 km deep. Previous estimates, based on the low measured abundance of 

atmospheric rare gas, suggested an inventory as small as 10-100 m. The discrepancy 

between these estimates is resolved if consideration is given to the various loss processes 

that may have affected the early atmosphere, such as hydrodynamic escape and atmospheric erosion by large impacts. 

Where does the surviving water reside? The only visible reservoirs are the martian 

polar caps and atmosphere, but their combined inventories fall far short of the suspected total. The “missing” water may be stored within the impact-generated regolith. 

Geologically reasonable estimates of the regolith’s total pore volume indicate that it 

may be sufficient to store a global Ocean of water as much as 1.5 km deep. 

cratered terrain suggests that the early martian climate may have differed markedly 

from that of today. Calculations indicate that an atmosphere of 1-5 bars of carbon 

dioxide would raise temperatures high enough to permit the flow of liquid water over 

the martian surface. Such conditions may have characterized the first half billion years 

of the planet’s climatic history, only to end as weathering processes depleted the atmospheric inventory of carbon dioxide faster than it could be replenished by global volcanism. If the early climate of Mars was indeed warm and wet, it clearly reopens the possibility that the planet may have evolved indigenous life. 

The diurnal, seasonal, and longer-term cycles of atmospheric water, carbon dioxide, 

and dust were also addressed during the MECA project. Evidence of the cyclical nature 

of the martian climate is visible in the layered stratigraphy of the perennial polar caps. 

This record is believed to reflect obliquity-driven changes in the formation of the seasonal carbon dioxide frost caps and the intensity of global dust storms. Complicating 

our understanding of this process is the recent discovery that the albedo of the seasonal 

caps is insolation dependent, a behavior that appears to explain why the current southern seasonal cap is able to survive throughout the southern summer. 

As an experiment in the management of a complex scientific program, MECA must 

be considered a success. Of particular note were the various MECA workshops, which 

brought together scientists of diverse backgrounds to discuss issues of common interest. 

The cross-discipline education and cooperative efforts that resulted from these meetings were major factors in the success of the program. Because many important issues in 

Mars climate research remain unresolved, we strongly recommended that a mechanism 

be established to continue this program of focused workshops. Given the success of this 

approach, we believe that the investigation of other complex problems in planetary 

science would benefit from the MECA model of science management. 

’ 

The presence of integrated networks of small valleys throughout the planet’s ancient 
3 

Science Report 

INTRODUCTION TABLE 1. MECA workshops. 

Mars has long fascinated scientists and the public. As 

a result, it has been the target of a number of ambitious 

spacecraft missions, the most recent being that of Vikings 

1 and 2 in 1976. Following an initial period of intensive 

study, it became clear by the late 1970s that the Viking 

data could still yield important clues about the nature and 

evolution of Mars. In recognition of this potential, NASA 

established the Mars Data Analysis Program (MDAP) in 

1979 to coordinate the funding and direction of Mars 

research. The first major investigation supported by MDAP 

was a focused three-year study project on the origin and 

evolution of martian volatiles. The project, entitled “Mars: 

Evolution of its Climate and Atmosphere” (MECA), was 

initiated in 1984 under the direction of the Lunar and 

Planetary Institute. 

In many respects, MECA was an experiment in science 

management. It combined elements of both a project 

approach and an approach involving research by independent investigators. From the project perspective, specific 

goals and objectives were defined, with administrative and 

logistical support provided through a central organization, 

the Lunar and Planetary Institute. However, investigators 

were funded individually and operated independently within 

the context of the study. To insure broad-based 

involvement, participation in the study project was open 

to all investigators who had research interests in the volatile 

and climate history of Mars, regardless of funding source. 

At the first meeting of the project, held in the spring 

of 1984, a science steering committee was elected and 

general guidelines for the project were defined. Three broad 

areas of study were identified: (1) the bulk chemical 

composition and outgassing history of Mars, (2) surface 

processes and climate history, and (3) seasonal cycles. 

a focus for research. A program of workshops was then 

organized to provide cohesion to the project and ensure 

that the project’s objectives would be addressed (Table 1). 

The results and ideas stimulated by this approach opened 

avenues of research that were unforeseen at the project’s 

outset. 

In this report, we review the scientific highlights of the 

MECA study project and discuss some of the important 

issues in martian climate research that remain unresolved. 

I 

I Within each area key questions were identified to provide 

Name of Workshop Date 

Water on Mars December 1984 

Dust on Mars I 

Clouds on Mars I 

Evolution of the Martian Atmosphere 

Dust on Mars I1 

Special Session on Martian Geomorphology 

and Its Relation to Subsurface Volatiles at 

LPSC XVII March 1986 

MECA Symposium on Mars: The Evolution of 

Its Climate and Atmosphere 

Atmospheric H2O Observations of the Earth 

and Mars September 1986 

Clouds on Mars I1 

Polar Processes on Mars 

Dust on Mars I11 

February 1985 

April 1985 

August 1985 

February 1986 

July 1986 

June 1987 

May 1988 

September 1988 

WATER ON MARS 

The principal conclusion of the MECA study project 

is that Mars had a substantially “wetter” history than 

previously thought. Although this conclusion is not 

accepted by all investigators, strong evidence has been 

rallied from several independent lines of study, including 

various geological arguments and geochemical 

considerations. 

Geological Evidence for Abundant Water 

With an atmospheric surface pressure of 6.1 mbar and 

a mean equatorial temperature of 220 K, the present 

martian climate precludes the stable flow of liquid water 

on the surface. However, there is evidence that a far 

different climate may have existed in the past. Integrated 

networks of small valleys, which resemble terrestrial runoff 

channels, dissect the planet’s ancient (-4 b.y. old) heavily 

cratered terrain, an indication that the early climate may 

have differed markedly from that of today. 

As discussed by Caw (1986), the clearest evidence of 

past water is provided by the outflow channels, which are 

broad, scoured depressions hundreds of kilometers long that 

PRECEDING PAGE BLANK NOT FTLMED 
4 MECAFidReport 

exhibit braided and streamlined forms within their beds. 

Most outflow channels originate within the cratered 

highlands just north of the great equatorial canyon system 

of Valles Marineris. The channels emerge abruptly from 

areas of collapsed and disrupted terrain, the apparent result 

of a massive and catastrophic release of groundwater. Carr 

estimates that the volume of water required to carve the 

channels was equivalent to a global Ocean some 50 m deep. 

Channel ages, inferred from the density of superposed 

craters, indicate several episodes of flooding; the oldest 

postdate most of the valley networks, while the youngest 

apparently formed within the last 1 to 2 b.y. 

There is little evidence of the fate of the water that 

eroded the channels. Initial examination of Mariner 9 and 

Viking images failed to reveal any indication of catchment 

areas. Their absence was attributed to the rapid vaporization 

of flood waters under conditions of low atmospheric 

pressure. However, the assumption that the flood waters 

were short -lived has been challenged recently by the 

discovery of possible remnants of ancient shorelines and 

sedimentary deposits in the low-lying northern plains. The 

evidence, derived from analysis of Viking images, suggests 

that large lakes and possibly even a shallow sea may have 

developed at the confluence of the major channels Uons, 

1984; Scott and Tamka, 1986; Parker et al., 1987; Greeky 

and Guest, 1987). 

Ancient shorelines and sedimentary deposits are not the 

only evidence that sizable bodies of water may have once 

existed on Mars. Horizontal, layered deposits up to 5 km 

thick are found in several branches of Valles Marineris. 

McCauky (1978) argued that these deposits are lake 

sediments that accumulated during an early epoch. Nedell 

et al. (1987) developed this idea further, suggesting that 

the lakes were formed when extensive groundwater seepage 

filled several of the enclosed canyons. 

Given the evidence of past water and the desiccated 

appearance of Mars today, the question arises: Where has 

all the water gone? Spacecraft measurements of the 

hydrogen escape flux from the martian atmosphere 

(Anderson and Hord, 1971) and kinetic theory calculations 

(Walk, 1977) indicate that Mars has lost -3 m of water 

by photodissociation and exospheric escape over the course 

of its geological history. Thus, most of the planet’s initial 

inventory of water should still reside in one of three 

reservoirs: the atmosphere, the perennial polar caps, or 

the regolith. The inventories of the first two reservoirs 

are readily assessed. Data obtained by the Viking Mars 

Atmospheric Water Detectors (MAWD) revealed that if 

all the water vapor present in the martian atmosphere were 

to condense on the surface it would form a global layer 

only 15 microns thick (Farmer et al., 1977). Similarly, the 

dimensions of the perennial polar caps are consistent with 

a quantity of water no greater than a global Ocean several 

tens of meters deep. The total size of these two reservoirs 

falls significantly short of the planetary inventory inferred 

from the abundant geomorphic evidence of past fluvial and 

periglacial activity (Caw, 1986). This evidence suggests that 

a considerable amount of water now resides within the 

regolith . How much water can the martian regolith hold? As on 

the Moon, the intense bombardment phase of early martian 

geologic history is thought to have resulted in the 

production of a blocky, porous megaregolith that extends 

to considerable depth (Fanuk, 1976; Caw, 1979). Studies 

of the seismic characteristics of the lunar crust suggest that 

it is brecciated to a depth of about 20 km. Gravitationally 

scaling this result to Mars suggests that the martian crust 

may retain significant porosity to a depth of 10 km and 

may possess a total pore volume sufficient to store a global 

layer of water 0.5-1.5 km deep (Clifford, 1987a). 

The possibility that the regolith represents a sizable 

volatile reservoir is supported by a long list of martian 

landforms whose morphology has been attributed to the 

presence of subsurface water (Rossbacher andJwdson, 1981; 

Carr, 1986). Many of these features resemble cold-climate 

features found on Earth; however, in other instances the 

morphologies appear unique to Mars. Of particular interest 

are rampart craters. Unlike craters found on the Moon, 

Mercury, and other bodies of the solar system, the ejecta 

surrounding many martian craters appears to have been 

emplaced in part as a ground-hugging fluidized flow. This 

fluidized appearance has led many investigators to conclude 

that rampart crater ejecta morphology originates from an 

impact into a water- or ice-rich crust (Caw et al., 1977; 

Gault and Greeky, 1978; Mouginis-Mark, 1987); however, 

laboratory cratering experiments indicate that interactions 

with the atmosphere may also play a role (Schultz and Gault, 

1979). If the water impact interpretation is correct, then 

the number and distribution of rampart craters indicates 

that the inventory of subsurface water on Mars, at the 

time of impact, was substantial. 

Geological estimates of the amount of water that Mars 

has degassed have varied over a wide range. By mapping 

the extent and thickness of the planet’s volcanic units, 

Gee4 (1987) has estimated that about 46 m of water 

may have been released by volcanism alone, given lava 

volatile contents comparable to Earth‘s. Can (1986) has 

taken a different approach. Based on his estimate of the 
Technical Report 88-09 5 

volume of water required to erode the outflow channels 

and the likely extent of its original source area, he estimates 

a global inventory of water in excess of 500 m, assuming 

the source region was representative of the rest of the 

planet. 

Mars Volatile Inventory: 

Geochemical Considerations 

Most early attempts at estimating the volatile inventory 

of Mars were based on comparisons of the relative 

abundance of various atmospheric constituents (e.g., the 

noble gases, carbon, and nitrogen) with the corresponding 

values found on Earth. These comparisons were made in 

the belief that they provided an accurate indication of 

the relative extent of outgassing that Mars had experienced. 

However, the inventory of water predicted by these models 

was invariably small (100 m or less) and clearly at odds 

with the geological evidence. This conflict may at last be 

reconciled as a result of knowledge gained from an unlikely 

source: the Shergotty, Nakhla, and Chassigny (SNC) 

meteorites. 

The SNCs are a group of eight stony meteorites that 

share at least two unique characteristics: a remarkably 

youthful crystallization age (-1.3 b.y.) and an embedded 

gas component that provides persuasive evidence of their 

origin. Based on age alone, the SNCs have attracted 

considerable attention, for they are half as old as the next 

youngest extraterrestrial sample found to date. Such recent 

crystallization requires a parent body that was geologically 

active for far longer than might be reasonably expected 

of the Moon or any asteroid. This consideration narrows 

the field of dynamically reasonable candidates to just one: 

Mars (Wasson and Wetherill, 1979; Wood and Ashwal, 1981). 

Virtual confirmation that Mars is the parent body of 

the SNC meteorites has come from the analysis of gas 

trapped within their shock-induced melt. The gas has an 

isotopic composition that is strikingly similar to the 

atmospheric samples analyzed by the Viking Landers 

(Bogard, 1982; Pepin, 1987). This similarity extends to an 

observed enrichment in "N, a compositional characteristic 

that is otherwise unique to Mars (Becker and Pepin, 1984). 

As probable samples of Mars, the SNCs provide clues 

to the planet's bulk composition and geochemical history 

(Dreibus and Wanke, 1985; McSween, 1985). When 

normalized to the abundances of such refractory elements 

as Si and La, the SNC meteorites are found to be several 

times richer in the moderately volatile elements (e.g., Na, 

K, and Br) than is generally inferred for Earth (Dreibus 

and Wiinke, 1985). This finding provides further support 

for the belief that Mars is a volatile-rich planet. 

Although a high volatile inventory appears difficult to 

reconcile with the low measured abundance of atmospheric 

rare gas, the discrepancy is readily explained if the martian 

atmosphere experienced a substantial mass loss early in its 

history. There are at least three processes by which such 

a loss may have occurred: hydrodynamic escape, atmospheric erosion by energetic impacts, and loss via the solar 

wind. 

Hydrodynamic escape, or the rapid thermally-driven loss 

of hydrogen from a planetary atmosphere, was probably 

most effective during the first few hundred million years 

of solar system history, when the atmospheres of the 

terrestrial planets may have still possessed a significant solar 

component and when the sun's ultraviolet output was 

1-2 orders of magnitude greater than it is today. One 

consequence of a vigorous flow of escaping hydrogen would 

be the enhanced loss of other light atmospheric constituents. As a result, an atmosphere that has undergone this 

process should exhibit a noticeable mass-fractionation of 

the lighter species; this is precisely what is observed in 

the present-day noble gas pattern of Mars (Hunten et al., 

1987; Pepin, 1987). 

At least two other processes may have contributed to 

the depletion of a dense early atmosphere. Calculations 

by Watkins and Lewis (1985) suggest that large impacts 

may have blasted a significant portion of the early 

atmosphere off into space. This process would have been 

particularly effective during the heavy bombardment 

period, when large impacting bodies were still prevalent 

in the solar system. The depletion of the atmosphere wa6 

probably further enhanced by the interaction of the solar 

wind with the martian ionosphere. Particle velocities within 

the resulting plasma flow likely exceeded the 5 km sel escape 

velocity of Mars. Calculations indicate that this process, 

alone could have reduced a dense early atmosphere to its 

present state in as little as a billion years (Perez-de-Tejadu, 

1987). 

Thus, lines of geological evidence and geochemical models 

based on the composition of the SNC meteorites suggest 

that a substantial amount of water was present on Mars 

thoughout much of its early history. The apparent 

discrepancy between this large inventory and the low 

measured abundance of atmospheric rare gas is readily 

explained if consideration is given to the various loss 

processes that are likely to have affected the early 

atmosphere. 
6 MECA Final Report 

EVOLUTION OF THE CLIMATE 

There are at least two schools of thought regarding the 

climatic conditions that prevailed on Mars at the time of 

valley network formation. The first is based on the idea 

that the networks resulted from precipitation and surface 

runoff (e.g., Masursky et al., 1977), a model that requires 

atmospheric pressures and surface temperatures far higher 

than those of today. Such conditions are possible if Mars 

had an early “greenhouse” environment. Estimates of the 

amount of carbon dioxide necessary to maintain surface 

temperatures above freezing range from 1 to 5 bars 

(Postawko and Kuhn, 1986; Kasting, 1987). Although this 

is two to three orders of magnitude greater than the present 

atmosphere, it is well within current estimates of the 

planet’s total volatile budget (Pepin, 1986). 

For the atmospheric inventory of carbon dioxide to 

decline from an initial value of several bars to its present 

level of 6.1 mbar implies a significant depletion process. 

Although atmospheric erosion may have played a role, an 

alternative explanation is that atmospheric carbon dioxide 

reacted with the regolith and liquid water to form carbonate 

rocks (Kahn, 1985; PolIack et al., 1987). The further 

development of the regolith by repeated impacts and 

weathering would have created an additional sink via 

adsorption (Fanale et ai., 1986). These processes may have 

ultimately modified the climate to the point where liquid 

water was no longer stable at the surface. Proponents of 

this model suggest that this transition occurred about 4 b.y. 

ago, marking the end of valley network formation. 

The second school of thought suggests that the early 

climate did not differ substantially from that of today. 

Advocates of this view find no compelling reason to invoke 

a warmer, wetter period to explain the origin of the valley 

networks. Rather, they cite evidence that the primary 

mechanism of small valley formation was groundwater 

sapping (Pieri, 1980; Brakenridge et al., 1985; Baker and 

Partridge, 1986), a process that does not require that liquid 

water exist in equilibrium with the atmosphere. If this 

analysis is correct, then small valleys could develop even 

under current climatic conditions (CUTT, 1983; Brakenndge 

et al., 1985). 

Yet if the early climate were similar to the present one, 

why are valley networks found almost exclusively in the 

oldest terrains? Several explanations are possible. First, it 

has been observed that many small valleys originate on 

or near the rims of large craters. This association led 

Brakenridge et al. (1985) to suggest a genetic relationship 

whereby the impact melt produced during the formation 

of large craters resulted in the establishment of local 

hydrothermal systems within the surrounding ice-rich crust; 

the discharge from these systems then formed the valleys. 

Because only large impacts would have produced sufficient 

melt to establish the necessary hydrothermal activity, the 

decline in valley network formation might then simply 

reflect a decline in the number of large impactors. 

Another possibility has been proposed by Jakosky and 

Carr (1985). They note that prior to the formation of the 

Tharsis volcanic complex, the obliquity of Mars periodically 

reached values as high as 45”. During these times, large 

quantities of water ice may have sublimed from the 

perennial polar caps. As the resulting vapor was transported 

toward the equator, cold nighttime temperatures could have 

led to saturation and snowfall at low latitudes, creating 

a snowpack that grew until the obliquity once again 

declined. Clow (1987) has shown that the absorption of 

sunlight within such a snowpack could lead to transient 

melting, even at pressures and temperatures only slightly 

in excess of those of today. The meltwater so produced 

may have then eroded the valleys. 

An interesting aspect of this proposal is that it is selfterminating. With the formation of Tharsis, the maximum 

obliquity of Mars declined to 35”, a figure too small to 

generate the high polar sublimation rates and low-latitude 

snowpack ascribed to the pre-Tharsis climate. Although 

the exact timing is not well constrained, present estimates 

indicate that the age of the Tharsis complex is about 3.5 b.y. 

Finally, recent geological mapping by Masursky et al. 

(1987) indicates that some small valleys may be considerably 

younger than previously thought, although it is unclear 

whether these valleys are volcanic or fluvial in origin. If 

subsequent investigation establishes that the valleys are 

indeed fluvial, then either our understanding of the middle 

course of martian climatic history, or the process involved 

in valley network formation, will likely need revision. 

Geomorphic Evidence of the Current Climate 

Although there is considerable uncertainty regarding the 

conditions that characterized the early martian climate, 

there is little debate that Mars has been cold throughout 

its recent history. Climatic models indicate that surface 

temperatures have probably not varied significantly from 

the current average of 220 K at the equator and 160 K 

at the poles. Atmospheric surface pressures have probably 

also been low, with obliquity-driven polar insolation changes 

causing oscillations between 0.1 to 15 mbar, a variation 

that reflects differences in the amount of carbon dioxide 
Technical Rewt 88-09 7 

adsorbed in the regolith and stored as ice in the seasonal 

polar caps (Fanale et al., 1982). 

An important characteristic of the current climate is 

that between the latitudes of *35”, mean annual 

temperatures exceed the frost point. Consequently, ground 

ice in this region is unstable and will eventually sublime 

away (Clifford and Hillel, 1983; Fanale et al., 1986). The 

vapor that results from the sublimation of equatorial ground 

ice is ultimately cold trapped at higher latitudes, thus 

enriching the ground ice content of the temperate and 

polar regolith. 

Evidence that the distribution of ground ice conforms 

to this theoretical expectation has been presented by 

Squyres and Caw (1986). They note that while crater rims, 

scarps, and ridges are all sharply defined at equatorial 

latitudes, these features exhibit more rounded and subdued 

profiles closer to the poles. Squyres and Carr propose that 

this “softened” appearance is the result of ice-enhanced 

creep, and they further note that the absence of softened 

terrain near the equator is consistent with the theoretical 

prediction that this latitude band is ice free. 

THE SEASONAL CYCLES OF CARBON DIOXIDE, 

WATER, AND DUST 

The rotational axis of Mars is currently inclined by 25”; 

thus the planet experiences seasonal change; In late fall, 

the reduction in insolation at high latitudes is sufficient 

to cause carbon dioxide to condense from the atmosphere. 

Surface pressure variations monitored by the Viking Landers 

indicate that as much as a fifth of the planet’s atmosphere 

freezes out during winter, forming a seasonal polar cap that 

extends toward the equator as far as 40” latitude. By 

midspring, the measured rise in surface pressure indicates 

that virtually all of the carbon dioxide has returned to 

the atmosphere. 

Because northern winter occurs very near perihelion, 

the seasonal cycle of carbon dioxide is not symmetric 

between the poles. As a consequence of its shorter season, 

the northern carbon dioxide cap is smaller than its southern 

counterpart. In addition, while the northern seasonal cap 

disappears entirely during summer, a remnant of the 

southern seasonal cap persists throughout the year. This 

year-round survival of carbon dioxide has been attributed 

to a polar cap albedo that is significantly higher in southern 

spring than observed during the equivalent season in the 

north (Paige and Ingersoll, 1985). A possible explanation 

for this disparity is that major dust storms on Mars occur 

at a time when the northern cap is forming, making it 

inherently dustier than its southern counterpart. However, 

the Viking mission found that global dust storms did not 

occur every year, and that the seasonal variation of 

atmospheric pressure showed little variability. This 

insensitivity of the carbon dioxide cycle to atmospheric 

dustiness may be related to the greater insolation of 

southern spring, which may cause dust grains entrained 

in the seasonal deposit to become hot and sink into the 

frost, producing a dramatic increase in the seasonal cap’s 

surficial reflectivity (Paige and Kieffer, 1986). 

There is a clear link between the seasonal cycle of carbon 

dioxide and the corresponding cycles for dust and water. 

When the seasonal cap sublimes in southern spring, the 

high mass flm from the cap and the sharp temperature 

contrast across the cap boundary often results in the 

generation of local dust storms. Closer to perihelion, larger 

storms frequently occur at the subsolar point. The actual 

manner in which dust is initially raised by these storms 

is unknown, but several mechanisms have been proposed. 

These mechanisms include impact ejection of dust particles 

by saltating sand grains, the entrainment of dust clumps 

or aggregates by low-speed surface winds, and dust 

fountaining due to the rapid desorption of carbon dioxide 

(Huguenin et al., 1986) or water (Greek and Leach, 1979) 

from the regolith. Dust devils, discovered recently on Viking 

Orbiter images by Thomas and Gierasch (1985), may be 

another mechanism for raising dust into the atmosphere. 

Perihelion dust storms frequently grow to global 

proportions. Two examples of this occurred during the first 

year observed by the Viking mission. However, while global 

dust storms may dominate the planet one year, they can 

be absent the next. This interannual variability may be 

linked to the dust cycle itself. For example, the transport 

of dust into the northern hemisphere during the winter 

of one year may ultimately weaken the Hadley circulation 

in the following year (Haberle, 1986). 

Pollack et al. (1979) have suggested that the fate of 

atmospheric dust is intimately tied to the formation of 

the seasonal polar caps. They propose that airborne dust 

particles serve as nucleation centers for the condensation 

of water ice. As either hemisphere enters the fall season, 

the suspended particles receive an additional coating of 

frozen carbon dioxide. This coating of carbon dioxide makes 

the particles heavy enough to precipitate from the 

atmosphere, contributing to the formation of the seasonal 

polar caps. In the spring, the carbon dioxide sublimes away; 

however, at high latitudes, it leaves behind a residual deposit 

of water ice and dust that adds to the perennial caps. 

Insolation changes, due to axial precession and periodic 
8 MECAFinnlRepxt 

variations in obliquity and orbital eccentricity, may alter 

the mixing ratio of ice to dust in the annual depositional 

layer. Such a scenario appears to explain the origin of the 

numerous horizontal layers that comprise the stratigraphy 

of both caps (Toon et al., 1980). This model of polar 

deposition has a potential problem, however. As noted by 

Jakosky and Martin (1987), Viking infrared observations, 

made at times of peak dust storm activity, indicate that 

the temperature of the polar atmosphere above the 

lowermost scale height often exceeds the frost point of 

carbon dioxide. Clearly, such an observation is difficult 

to reconcile with the condensation mechanism of Pollack 

et al. (1979). As a result, the process of polar deposition 

remains an active area of theoretical investigation. 

Mariner 9 radio occultation data indicates that the polar 

deposits may be anywhere from 1-6 km thick (Dzurisin 

and Blasius, 1975). If the larger estimates are accurate, 

calculations suggest that the deposits may be thick enough 

to undergo geothermal melting at their base (Clifford, 

1987b). In the north the deposits cover an area -lo00 km 

across, while in the south they have a diameter of 

approximately 1500 km. Because few craters with diameters 

greater than 300 m are visible within the deposits, they 

are believed to be relatively young (-10’ years; Pluut et 

al., 1988). Interestingly, elsewhere on the planet there are 

a number of older, but morphologically similar, deposits. 

Though they now appear devoid of ice, Schultz and Lutz 

(1988) have argued that these deposits may be evidence 

that the location of the poles has migrated over time due 

to changes in the planet’s moment of inertia. Such changes 

may have resulted from the filling of impact basins by flood 

basalts and the development of the Tharsis volcanic 

complex. 

Models of the martian atmospheric circulation have been 

constructed to study the transport processes involved in 

the formation of the polar deposits. Since much of the 

redistribution of dust is thought to occur during northern 

winter, most of the research has focused on the circulation 

at this time of year. Constraining the models are Viking 

observations showing a substantial warming of the polar 

atmosphere during the second global dust storm of 1977 

(Martin and Kiefier, 1979). The fact that the warming occurs 

well into the polar night indicates that it must be due 

to atmospheric dynamics, although the precise mechanism 

remains unclear. Early calculations with an inviscid zonally 

symmetric model were unable to reproduce the warming 

(Haberk et ai., 1982). More recently, however, Magalhaes 

(1987) and Barn and Hollingsworth (1987) have been able 

to reproduce some of its features, although the mechanisms 

they invoke are fundamentally different. Magalhaes, for 

example, retains zonal symmetry but invokes viscous mixing, 

while Barnes and Hollingsworth employ a planetary wave 

mechanism similar to that involved in the sudden warming 

of the Earth’s stratosphere. 

In each of these approaches, suspended dust particles 

play a key role by altering the thermal drive for atmospheric 

motions. Pollack et al. (1987) have begun to investigate 

this interaction with the aid of a general circulation model. 

Their first results show that the presence of atmospheric 

dust has a substantial effect: strengthening and expanding 

the Hadley circulation, enhancing the thermal tides, and 

changing the character of the midlatitude storms. One 

interesting result of their calculations is the steady increase 

in low-level winds (at the latitudes where dust storms 

originate) as the total dust in the atmosphere increases. 

However, if wind speeds continue to increase, what stops 

the dust-raising process? One possibility is that by increasing 

the atmospheric stability, dust in the atmosphere suppresses 

the turbulence that mixes momentum down to the surface. 

Calculations with a boundary layer model tailored for Mars 

have shown this to be the case, suggesting that a direct 

reduction in wind speeds is not necessary to shut off the 

dust-raising process (Haberk, 1987). 

Water, like dust and carbon dioxide, is cycled seasonally 

between its reservoirs. Measurements from both Earthbased instruments and the Viking MAWD experiment have 

shown that the distribution of atmospheric water vapor 

varies both seasonally and latitudinally. This variability is 

thought to result from a combination of atmospheric 

transport and exchange with surface and subsurface 

reservoirs (Jakosky, 1985). The most likely reservoirs are 

surface ice deposits and water adsorbed within the regolith. 

However, because of their similar response to solar 

insolation and because of the uncertain role of atmospheric 

transport, the relative contributions of these two sources 

are difficult to determine. 

Nevertheless, it is known that the residual north polar 

cap is composed of water ice and that it acts as a source 

of vapor during the summer (Kiefjer et al., 1976; Farmer 

et al., 1976). However, is the residual cap the only source 

of water at this season? Recent modeling calculations by 

Haberk and jakosky (1987) suggest that it is not. If it were, 

then the resulting vapor would have to be transported to 

lower latitudes rather quickly; otherwise, the polar regions 

would be saturated and covered with clouds, a condition 

that is not observed. Furthermore, calculations show that 

the high latitude circulation is too weak to move water 
Technical Report 88-09 9 

very far from the cap. Other sources of water must therefore 

exist. 

On an annual and zonally averaged basis, there is a 

gradient in atmospheric water vapor abundance from north 

to south. The cause of this asymmetry has been the subject 

of some debate.Jukosky (1983) has argued that the gradient 

is a reflection of the different composition of the remnant 

caps and that it implies a net north-to-south transport. 

However, asymmetries in global circulation patterns due 

to dust storms (Duuies, 1981) or the seasonal mass flux 

of carbon dioxide to and from the caps uumes, 1986) can 

also set up a gradient in water vapor with no net transport. 

Thus, the mass balance of the caps remains an open issue. 

SUMMARY 

The view of Mars that has evolved during the MECA 

study project is far different from that which existed shortly 

after the Viking mission. Mars is now recognized as a wetter 

and more complicated planet than previously thought; 

however, many questions about its evolution still remain: 

How much water did Mars inherit from the solar nebula, 

and how much of this was ultimately outgassed? Was there 

an additional late-stage input from comets and meteorites? 

What was the primordial composition of the atmosphere 

and to what extent was it affected by hydrodynamic escape 

and impact erosion? What conditions gave rise to the valley 

networks? How much confidence is there in the identification of various martian landforms as indicators of 

subsurface volatiles? What variables affect the current 

annual cycles of carbon dioxide, water, and dust? How have 

these cycles varied with time? These are just a few of the 

many questions that investigators have only begun to 

address. 

Some answers may be provided by the further analysis 

of data already in hand; this is the approach of the threeyear study project that succeeds MECA, entitled “Mars: 

Evolution of Volcanism, Tectonism, and Volatiles.” New 

data anticipated from Mars Observer (the next U.S. Mars 

mission, scheduled for launch in 1992) will be of critical 

importance. But ultimately our ability to answer many of 

the outstanding questions concerning the martian climate 

is contingent on the missions that follow Mars Observer. 

These will likely include rover investigations of the polar 

layered terrains, canyons, volcanos, outflow channels, and 

valley networks; the establishment of a global meteorological 

network to monitor the present climate; seismic and 

electrical investigations to determine the current state and 

distribution of subsurface volatiles; and the return of 

samples to Earth to allow researchers to bring to bear the 

full spectrum of modern analytical techniques to the 

investigation of martian mineralogy, geochemistry, and 

volatiles. 

As an experiment in the management of a major science 

program, MECA must be viewed as a success. Besides 

meeting its scientific goals, the study project clearly 

demonstrated the benefits of an interdisciplinary approach 

to the investigation of a complex and multifaceted topic. 

The success of this strategy was particularly evident during 

the study project’s various workshops, where terrestrial and 

planetary scientists were often brought together from 

seemingly disparate fields. Yet out of these meetings came 

discussions and collaborations that often produced 

significant advances in our understanding of the martian 

atmosphere and climate. The fruit of this effort is likely 

to benefit Mars research for many years to come. 

REFERENCES 

Anderson D. E. and Hord C. W. (1971) Mariner 6 and 7 ultraviolet 

spectrometer experiment: Analysis of hydrogen Lyman-alpha data. 1. 

Geophys. Res., 76, 6666-6673. 

Baker V. R. and Partridge J. B. (1986) Small martian valleys: Pristine 

and degraded morphology. J. Geophys. Res., 91, 3561-3572. 

Barnes J. B. and Hollingsworth J. L. (1987) Dynamical modeling of a 

planetary wave mechanism for a martian polar warming. Icm, 71, 

313-334. 

Becker R. H. and Pepin R. 0. (1984) The case for a martian origin 

of the shergottites: Nitrogen and noble gases in EETA 79001. Earth 

Planet. Sci. Lett., 69, 225-252. 

Bogdrd D. D. (1982) Trapped noble gases in the EETA shergottite. 

Meteoritics, 17, 185-186. 

Brakenridge G. R., Newsom H. E., and Baker V. R. (1985) Ancient hot 

springs on Mars: Origins and paleoenvironmental significance of small 

martian valleys. Geology, 13, 859-862. 

Carr M. H. (1979) Formation of martian flood features by release of 

water from confined aquifers. J. Geophys. Res., 84, 2995-3007. 

476-495. 

Carr M. H. (1983) Stability of streams and lakes on Mars. lcaruc, 56, 

Carr M. H. (1986) Mars: A water-rich planet? Icaws, 68, 187-216. 

Carr M. H., Crumpler L. S., Cutts L. A., Greeley R., Guest J. E., and 

Masursky H. (1977) Martian impact craters and the emplacement 

of ejecta by surface fl0w.J. Geophys. Res., 82, 4055-4065. 

Clifford S. M. (1987a) Mars: Crustal pore volume, cryospheric depth, 

and the global occurrence of groundwater. In MECA Symposium on 

MUSS: Evolution of its Climate and Atmosphere (V. Baker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

pp. 32-34. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Clifford S. M. (1987b) Polar basal melting on Mars, J. Geophys. Res., 

Clifford S. M., and Hillel D. (1983) The stability of ground ice in the 

92,9135-9152. 

equatorial region of Mars. J. Geophys. Res., 88, 2456-2474. 
10 MECA Final Report 

Clow G. D. (1987) Generation of liquid water on Mars through the 

Davies D. W. (1981) The Mars water cycle. Icam, 45, 398-414. 

Dreibus G. and Wanke H. (1985) Mars, a volatile-rich planet. Meteoritics, 

20, 367-381. 

Dzurisin D. and Blasius K. R. (1975) Topography of the polar layered 

deposits of Mars. J. Geophys. Res., 80, 3286-3306. 

Fanale F. P. (1976) Martian volatiles: Their degassing history and 

geochemical fate. Icam, 28, 179-202. 

Fanale F. P., Salvail J. R., Branerdt W. B., and Sunders R. S. (1982) 

Mars: The regolith atmosphere cap system and climate change. Icasus, 

50, 381-407. 

Fanale F. P., Salvia1 J. R., Zent A. P., and Postawko S. E. (1986) Global 

distribution and migration of subsurface ice on Mars. Im, 67, 1-18. 

Farmer C. B., Davies D. W., and LaPorte D. D. (1976) Northern summer 

ice cap-Water vapor observations from Viking 2. Science, 194, 

1339-1340. 

Farmer C. B., Davies D. W., Holland A. L., LaPorte D. D., and Downs 

P. E. (1977) Mars: Water vapor observations from the Viking Orbiters. 

J. Geophys. Res., 82, 4225-4248. 

Gault D. E. and Greeley R. (1978) Exploratory experiments of impact 

craters forrr’ed in viscous-liquid targets: Analogs for martian rampart 

craters? Icak, 34, 486-495. 

Greeley R. (1987) Release of juvenile water on Mars: Estimated amounts 

and timing associated with volcanism. Science, 236, 1653-1654. 

Greeley R. and Guest J. E. (1987) Geologic map of the eastern equatorial 

region of Mars. U.S. Geol. SUW. Misc. Inu. Map 1-1 802B. 

Greeley R. and Leach R. (1979) “Steam” injection of dust on Mars: 

Laboratory simulations. NASA T’M-80339, pp. 304-307. 

Haberle R. M. (1986) Interannual variability of great dust storms on 

Mars. Science, 234, 459-461. 

Haberle R. M. (1987) The influence of dust on the structure of the 

diurnally varying boundary layer on Mars. Bull. Am. As~T~. Soc., 

19, 815. 

Haberle R. M. and Jakosky B. M. (1987) Trai sport of water from the 

residual north polar cap on Mars. In LUMT and Planetary Science XVIIf, 

p. 378. Lunar and Planetary Institute, Houston. 

Haberle R. M., Leovy C. B., and Pollack J. B. (1982) Some effects of 

global dust storms on the atmospheric circulation of Mars. Icam, 

5 I, 322-367. 

Huguenin R. L., Harris S. L., and Carter R. (1986) Injection of dust 

into the martian atmosphere: Evidence from the Viking gas exchange 

experiment. Icam, 68,99-119. 

Hunten D. M., Pepin R. O., and Walker J. C. G. (1987) Mass fractionation 

in hydrodynamic escape. Icam, 69, 532-549. 

Jakosky B. M. (1983) The role of seasonal reservoirs in the Mars water 

cycle 11: Coupled models of the regolith, the polar caps, and atmospheric 

transport. Icam, 55, 19-39. 

Jakosky B. M. (1985) The seasonal cycle of water on Mars. Space Sci. 

Jakosky B. M. and Carr M. H. (1985) Possible precipitation of ice at 

low latitudes of Mars during periods of high obliquity. Nature, 315, 

559-561. 

Jakosky B. M. and Martin T. 2. (1987) Mars: North polar atmospheric 

warming during dust storms. Im, 72, 528-534. 

James P. B. (1986) The martian hydrologic cycle: Effects of carbon dioxide 

mass flux on global water distribution. Icm, 64, 249-264. 

melting of a dusty snowpack. Icam, 72, 95-127. 

Rw., 41, 131-200. 

Jons H. P. (1984) Sedimentary basins and mud flows in the northern 

lowlands of Mars. In Lunar and Planetary Science XV, p. 417. Lunar 

and Planetary Institute, Houston. 

Kahn R. (1985) The evolution of carbon dioxide on Mars. Icam, 62, 

175-190. 

Kasting J. F. (1987) Climatic effects of enhanced carbon dioxide levels 

in Mars’ early atmosphere. In MECA Symposium on Mars: Evoluti~n 

of its Climate and Atmosphere (V. Baker, Michael Carr, F. Fanale, 

R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), pp. 64-66. 

LPI Tech. Rpt. 87-01, Lunat and Planetary Institute, Houston. 

Kieffer H. H., Chase S. C., Jr., Martin T. Z., Miner E. D., and Palluconi 

F. D. (1976) Martian north pole summer temperatures: Dirty water 

ice. Science, 194, 1341-1344. 

Magalhaes J. A. (1987) The martian Hadley circulation: Comparison of 

“viscous” model predictions to observations. fcam, 70, 442-468. 

Martin T. 2. and Kieffer H. H. (1979) Thermal infrared properties of 

the martian atmosphere. 2. The 15 pm band measurements.]. Geophys. 

Res., 84,2830-2842. 

Masursky H., Boyce J. M., Dial A. L., Schaber G. G., and Strobell M. 

E. (1977) Formation of martian channels. J. Geophys. Res., 82, 

4016-4028. 

Masursky H., Chapman M. G., Davis P. A., Dial A. L., Jr., and Strobell 

M. E. (1987) Martian terrains. NASA TM-89810, pp. 545-547. 

McCauley J. F. (1978) Geologic map of the Coprates quadrangle of Mars. 

US. Geol. SUW. Mkc. Inu. Map 1-879. 

McSween H. Y., Jr. (1985) SNC meteorites: Clues to martian petrologic 

evolution? Rev. Geophys., 23, 391-416. 

Mouginis-Mark P. J. (1987) Water or ice in the martian regolith? Clues 

from rampart craters seen at very high resolution. Icancs, 71, 269-286. 

Nedell S. S., Squyres S. W., and Anderson D. W. (1987) Origin and 

evolution of the layered deposits in the Valles Marineris, Mars. Icam, 

70, 409-441. 

Paige D. A. and Ingersoll A. P. (1985) Annual heat balance of the martian 

polar caps: Viking observations. Science, 228, 1160-1168. 

Paige D. A. and Kieffer H. H. (1986) Nonlinear frost albedo feedback 

on Mars: Observations and models. In Workshop on the Evolution of 

the Martian Atmosphere (M. Carr, P. James, C. Leovy, R Pepin, and 

J. Pollack, eds.), pp. 33-34. LPI Tech Rpt. 86-07, Lunar and Planetary 

Institute, Houston. 

Parker T. J., Schneeberger D. M., Pieri D. C., and Sunders R. S. (1987) 

Geomorphic evidence for ancient seas on Mars. In MECA Symposium 

on Mass: Evolution of its Climate and Atmosphere (V. Baker, M. Carr, 

5. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

pp. 96-98. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Pepin R. 0. (1986) Volatile inventory of Mars. In LUMT and Planetary 

Science XVII, pp. 656-657. Lunar and Planetary Institute, Houston. 

Pepin R. 0. (1987) Volatile inventories of the terrestrial planets. Rev. 

Geophys., 25, 293-296. 

Perez-de-Tejada H. (1980) Plasma flow in the Mars magnetosphere. J. 

Geophys. Res., 92, 4713-4718. 

Pieri D. C. (1980) Martian valleys: Morphology, distribution, age, and 

origin. Science, 210, 895-897. 

PlautJ. J.,KahnR.,GuinessE.A.,andArvidson R.E. (1988)Accumulation 

of sedimentary debris in the south polar region of Mars and implications 

for climate history. Icm, in press. 
Technical Report 88-09 11 

Pollack J. B., Colburn D., Flasar F. M., Kahn R., Carlston C. E., and 

Pidek D. (1979) Properties and effects of dust particles suspended 

in the martian atm0sphere.J. Geophys. Res., 84, 2929-2945. 

Pollack J. B., Kasting J., and Richardson S. (1987) Partitioning of carbon 

dioxide between the atmosphere and lithosphere on early Mars. In 

MECA Symposium on Mars: Evolution of its Climate and Atmosphere 

(V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, 

and T. Maxwell, eds.), pp. 104-105. LPI Tech. Rpt. 87-01, Lunar 

and Planetary Institute, Houston. 

Postawko S. E. and Kuhn W. R. (1986) Effect of the greenhouse gases 

((202, H20, SO2) on martian paleoclimate. J. Geophys. Res., 91, 

431-438. 

Rossbacher L. A. and Judson S. (1981) Ground ice on Mars: Inventory, 

distribution, and resulting landforms. Icarus, 45, 39-59. 

Schultz P. H. and Gault D. E.(1979) Atmospheric effects on Martian 

ejecta emplacement. J. Geophys. Res., 84, 7669-7687. 

Schultz P. H. and Lutz A. B. (1988) Polar wandering on Mars. Icarus, 

73,91-141. 

Scott D. H. and Tanaka K. L. (1 986) Geologic map of the western equatorial 

region of Mars. U.S. Geol. SUN. Misc. Jnu. Map J-1802A 

I 

Squyres S. W. and Carr M. H. (1986) Geomorphic evidence for the 

distribution of ground ice on Mars. Science, 231, 249-252. 

Thomas P. and Gierasch P. (1980) Dust devils on Mars. Science. 230, 

175-177. 

Toon 0. B., Pollack J. B., Ward W., Burns J. A., and Bilski K. (1980) 

The astronomical theory of climate change on Mars. Jcarus, 44, 

552-607. 

Walker J. C. G. (1977) Evolution of the Atmosphere. Macmillan Co., New 

York. 318 pp. 

Wasson J. T. and Wetherill G. W. (1979) Dynamical, chemical and isotopic 

evidence regarding the formation locations of asteroids and meteorites. 

In Asteroids (T. Gehrels, ed.), pp. 926-974. Univ. of Arizona Press, 

Tucson. 

Watkins H. and Lewis J. S. (1985) Loss of volatiles from Mars as the 

result of energetic impacts. In Workshop on Water on Mars (S. Clifford, 

ed.), pp. 93-95. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. 

Wood C. A. and Ashwal L. D. (1981) SNC meteorites: Igneous rocks 

from Mars? Proc. Lunar Planet. Sci. IZB, pp. 1359-1375. 
13 

- Appendix 1. Origin of MECA 

The Mars Data Analysis Program (MDAP) was initiated 

in FY-79 to provide support for the post-Viking analysis 

of Mars data. It was recognized by the scientific community 

that the amount of high-quality data acquired during the 

Primary and Extended Viking Mission (from June 1976 to 

August 1980) constituted a national resource, but that 

adequate support for continued analysis was not available 

from the existing Research and Analysis Program. 

3. 

4. 

What is the volcano-tectonic history of Mars? 

What are the major components of the atmospheric 

circulation and what processes are responsible for major 

atmospheric phenomena? 

Because of limited resources, the restructured Mars Data 

Analysis Program was unable to support research to address 

all of these questions concurrently. Rather, the approach 

climate first, and to defer the volcanic-tectonic research 

topics to a later time. 

A Space Science and Applications Notice entitled “The 

Volatile Evolution and Climate History of Mars” was 

released May 25, 1983. Proposals were received and 

reviewed later that year. AS stated in the notice: 

1 was to address problems dealing with atmosphere and 

TABLE Al. Ad hoc Mars Science Working Group, assembled March 

11, 1982 to define science goals for a Mars data analysis program. 

Members Affiliation 

R. Greeley, Chairman Arizona State University 

J. Boyce, ex officio 

M. Malin 

R. Batson 

S. Sunders 

S. Squyres 

E. Shoemaker 

L. Wilkening 

V. Baker 

M. Carr 

J. Pollack 

A. Albee 

F. Fanale 

D. Wilhelms 

D. Wise 

H. Kieffer 

NASA Headquarters 

Arizona State University 

US. Geological Survey 

Jet Propulsion Laboratory 

Cornell University 

US. Geological Survey 

University of Arizona 

University of Arizona 

US. Geological Survey 

NASA Ames Research Center 

Jet Propulsion Laboratory 

University of Hawaii 

US. Geological Survey 

University of Massachusetts 

US. Geological Survey 

An ad hoc Mars Working Group (Table Al) of planetary 

scientists met in 1981 and defined the key science questions 

for Mars that could be addressed with the available data. 

Representatives of the working group then met with NASA 

administrators and presented their findings. Four major 

scientific questions were identified for continued study of 

Mars: 

1. 

2. 

What is the volatile history of Mars? 

What is the climatic history of Mars and how have 

lithosphere/atmosphere/hydrosphere interactions affected 

the evolution of the martian surface? 

Plans for administering this study involve not only 

focusing the effort [science], but also introducing 

a novel method of coordinating the individual 

research tasks which are selected. The approach 

involves the establishment of a working group 

consisting of all investigators whose proposals are 

accepted and, through occasional meetings of the 

group, the coordination of the research efforts. 

The organized approach is not intended to coerce 

any of the participants to redirect their research, 

but rather to take advantage of the collective wisdom 

of the participants to guide the study, to identify 

important areas of research not addressed by 

proposals, and to encourage voluntary responses to 

the identified needs. 

Thus, in addition to having scientific goals, the program 

was also an experiment in science management that, in 

many respects, combined elements of a mission-oriented 

project while retaining the principal investigator’s individual 

goals and responsibilities. 

An organizational meeting of funded investigators and 

associates was held in March 1984 to refine the science 

objectives and to decide how to move forward on the threeyear program. A steering committee was elected (Table 

A2) and science questions were posed around three issues 

for Mars: (1) seasonal cycles, (2) surface processes/climate 

history, and (3) bulk chemical composition and outgassing 

history (Table A3). 

PRECEDING PAGE BLANK NOT FILMED 
14 MECAFinulReport 

TABLE A2. MECA Science Steering Committee. 

Member Affiliation Area 

Ronald Greeley Arizona State Chairperson 

Michael Carr US. Geological Surface Processes 

Fraser Fanale University of Hawaii Climate Change 

Robert Haberle NASA Ames Research Seasonal Cycles 

University 

Survey 

Center 

Robert Pepin University of Minnesota Bulk Chemistry 

Peter Schultz Lunar and Planetary Project Scientist 

Institute (to 1984) 

Stephen Clifford Lunar and Planetary Project Scientist 

Institute (1984 to 1988) 

Joseph Boyce NASA Headquarters Ex Officio 

Kevin Burke Lunar and Planetary Ex officio 

Pam Jones Lunar and Planetary Project 

Institute Administrator 

Institute 

TABLE A3. Major MECA study questions. 

hon cyckr 

0 What are the physical processes that control the present ~ea~onal 

0 How do the seasonal cycles change from year to year? 

0 How can models of the seasonal cycles be extended to long-term 

cycles of dust, water, and carbon dioxide? 

variations? 

Surfuce Processes and Climate History 0 What are the causative agents of climate change on Mars? 

0 How have the abundum of surface volatiles changed with time? 

What are the major volatile reserwirs, and how have they changed 

0 What has been the climatic history of Mars and how has it been 

0 What observations and modeling will help resolve the above questions? 

0 What is the range of possible absolute and relative abundances of 

the initial Mars volatile inventory? 

0 What evidence exists that the planet has undergone significant 

oxidation? Is the oxidation only on the surface? Are there plans to 

try to measure martian atmospheric DIH? Has the composition of 

degassed volatiles changed with styles of volcanism in time and space 

(inputs from climate history/ surface morphology)? 

0 What does the present atmosphere tell us about integrated outgassing 

modified by “loss processes” to the regolith and to space over-martian 

with time? 

affected by the agents, abundances, and reservoirs? 

Bufk Chemicul Composition and Outgassing History 

It was decided that the study project [named “Mars: 

Evolution of Its Climate and Atmosphere” (MECA)) would 

be open to all investigators who had a potnetial 

contribution, regardless of funding. A letter of invitation 

was mailed to more than 3500 individuals on the LPI 

distribution list. Eventual membership for the project grew 

to about 130 (see Appendix 2). Newsletters were issued 

regularly to keep the study group, NASA, and the 

community abreast of MECA activities. Figure A1 shows 

the relationship among NASA, the Working Group, and 

the Lunar and Planetary Institute. 

The scientific program of MECA was conducted through 

a series of symposia, special sessions, and workshops. For 

each of these activities, an organizing committee was formed 

to develop the program, solicit participants, and prepare 

summaries of the program. All activities were supported 

through LPI for logistics, including mailing and preparation 

of abstract volumes and technical reports. 

eologic time? Implications of isotopic signatures (15N/’*N, 

he/’32Xe, wAr/~Ar)? 
15 

Appendix 2. MECA Membership List 

Vincent J. Abreau 

SPRL 

2455 Hayward 

Ann Arbor, MI 48 105 

Mail Stop 695.0 

NASA Goddard Space Flight Center 

Greenbelt, MD 20771 

Arden L. Albee 

Division of Geological and Planetary Science 

Caltech 

Pasadena, CA 91 125 

Department of Geology 

San Jose State University 

San Jose, CA 95 192 

Duwayne M. Anderson 

Eust Bizell Hall, Room 305 

Texas A d M University 

College Station, TX 77843-1 I I2 

Department of Chemistry, B-017 

University of California, San Diego 

La Jolla, CA 92093 

McDonneU Center for the Space Sciences 

Washington Uniwrsity 

St. Louis, MO 63 130 

Department of Geosciences 

University of Arizona 

Tucson, A2 8572 1 

Mail Stop 239-12 

NASA Ames Research Center 

Moffett Field, CA 94035 

Department of Atmospheric Sciences 

Oregon State University 

Coruallis, OR 9733 1 

Institute of Geophysics and Planetary Physics 

University of California, Los Angeles 

Los Angeles, CA 90024 

Mail Code EL4 

NASA Headquarters 

Washington, DC 20546 

Department of Geological Sciences 

Wright State University 

Dayton, OH 45435 

Mario H. Acuna 

David W. Andersen 

James R. Arnold 

Raymond E. Arvidson 

Victor R. Baker 

Amos Banin 

Jeffrey R. Barnes 

Bruce Barraclough 

Joseph Boyce 

G. Robert Brakenridge 

Geoffrey Brigs 

Mail Code EL 

NASA Headquarters 

Washington, DC20546 

Mail Code EL 

NASA Headquarters 

Washington, DC 20546 

LUMT and Planetary lnstitute 

3303 NASA Road One 

Houston, TX 77058 

Mail Stop 183-301 

Jet Propulsion Laboratory 

4800 Oak Grwe Drive 

Pasadena,CA91109 

U.S. Geological Suruey 

345 Middlefield Road 

Menlo Park, CA 94025 

Mail Stop 245-3 

NASA Am Research Center 

Mofiett Field, CA 94025 

Beaumont Building 

Universitv of Sheffield 

Henry Brinton 

Kevin Burke 

Robert W. Carlson 

Michael H. Carr 

Patrick Cassen 

Peter Cattermole 

. __ bookhili 

Sheffield S3 7HF England 

Philip R. Christensen 

Deportment of Geology 

Arizona State University 

Tempe, AZ 85287 

Todd Clancy 

Laboratory for Atmospheric and Space Physics 

Campus Box 392 

University of Colorado 

Boulder, CO 80309 

LUM~ and Planetary lnstitute 

3303 NASA Road One 

Houston, 'D( 77058 

U.S. Geological Suruey 

345 Middkfild Road 

Menlo Park, CA 94025 

Mail Stop 245-3 

NASA Ames Research Center 

Moffett Field, CA 94035 

Stephen Clifford 

Gary D. Clow 

David Colburn 
16 MECA Final Report 

Lelia Coyne 

Department of Gology 

SanJose State University 

San Jose, CA 95 192 

Depa~tment of Geology and Geophysical Science 

Princeton University 

Pnnceton, NJ 08544 

Division of Geological and Planetary Science 

Caltech 

Pasadena, CA 91 125 

Richard Durham 

Department of Space Physics and AS~TOWIIIY 

P. 0. Box 1892 

Rice University 

Houston, TX 77251 

Thanasis E. Economou 

Laboratory for Astrophysics and space bearch 

Ensico Fermi Institute 

University of Chicago 

Chicago, IL 60637 

Mail Stop 183-701 

Jet Pr~jd~ion Laboratory 

4800 Oak Gwe Drive 

Pasadena, CA 91 IO9 

Laboratory for Atmospheric and Space Physics 

Cumpus Box 392 

University of Colorado 

Boulde~, CO 80309 

Planetary Geosciences Division 

Hawaii Institute of Geophysics 

2525 Correa Road 

Honolulu, HI 96822 

Department of Applied kience 

New York University 

New York, NY 10003 

Mail Code SN4 

NASA Johnson Space Center 

Hourton, TX 77058 

Geophysical Laboratory 

Cumegie Institute of Washingron 

2801 Upton St. NW 

Washington, DC 20008 

Mail Code SN2 

NASA Johnson Space Center 

Houston, TX 77058 

Department of Geology 

Arizona State University 

Tempe, AZ 85287 

D. Crerar 

G. E. Danielson 

170-25 

Charles Elachi 

L. W. Esposito 

Fraser P. Fanale 

Stuart Gaffm 

Everett K. Gibson, Jr. 

Kenneth A. Goettel 

James Gooding 

Ronald Greeley 

Edward A. Guinness 

McDonnell center for the space Sciences 

Washington University 

St. his, MO 63 130 

Robert M. Haberle 

Mail code 245-3 

NASA Ames Research Center 

Moffett Field, CA 94035 

Depmtment of Geology and Geophysical Science 

Princeton University 

Pnnceton, NJ 08544 

Department of Atmospheric and Oceanic Science 

University of Michigan, North Campus 

Ann Arbor, MI 48109 

Department of Geobgicaf Sciences 

&own University 

prouidence, RI 029 1 2 

Kenneth Herkenhoff 

I>lvirion of Geologkd and Planetary Science 

Caltech 

Pasadena, CA 91 125 

Department of Geobgicd Sciences 

&own University 

F’rwidence, RI 02912 

Department of Applied Science 

New York University 

Washington Square 

New York, NY 10003 

chemistry Department 

Arizona State University 

Tempe, AZ 85287 

Remote Sensing center 

302 Hasbrouck Lnboratory 

University of Massachusetts 

Amhmt, MA 01003 

Division of Geological and Planetary Science 

170-25 

Caltech 

Pacadena, CA 91 125 

Ekuce M. Jakosky 

Laboratory for Atmospheric and Space Physics 

University of Colorado 

hddm, CO 80309 

Physics Department 

University of Missouri, St. his 

St. his, MO 63 12 1 

R B. Hargraves 

Paul B. Hays 

James Head 

170-25 

Paul C. Hess 

Martin 1. Hoffert 

John R. Holloway 

Robert L. Huguenin 

Andrew P. lngersoll 

Philip B. James 
Technical Repost 88-09 17 

Fred Jaquin 

Space Scienca Building 

Cornell University 

Ithaca, NY 14853 

Heinr-Peter Jons 

Technische Universitat Clawtha 

Swn-Hedin Str. 19 

3000 Hannouer 5 I 

F. R. Gmny 

Department of Earth and Planetary Science 

Campus Box I 169 

Washington University 

St. Louis, MO 63 130 

Mail Stop 245-3 

NASA Ames Research Center 

Mofftt Field, CA 94035 

U.S. Geological Suwey 

2255 North Gemini Drive 

Fkstaff, AZ 86001 

Department of Atmospheric and Oceanic Science 

University of Michigan, North Campus 

Ann Arbor, MI 48109 

Ralph Kahn 

Jim Kasting 

Hugh H. Keiffer 

William R. Kuhn 

Steve Lee 

Department of Geology 

Arizona State University 

Tempe, AZ 85287 

Mail code AK-40 

University of Washington 

Seattle, WA 98195 

Planetary Sciences Department 

University of Arizona 

Tucson, AZ 8572 1 

Space Science and Engineering Center 

University of Wisconsin, Madica 

1225 W. Dayton Street 

Madison, WJ 53706 

U.S. Geological Survey 

Branch of Astrogeology 

2255 North Gemini Driue 

Fkzgstafi, AZ 86001 

Department of Geology 

Arizona State University 

Tempe, AZ 85287 

Laboratory for Atmospheric Research 

College of Engineering 

Washington State University 

Pullman, WA 99164-2730 

Conway Leovy 

John S. Lewis 

Sanjay S. Limaye 

Baerbel K. Lucchitta 

Michael Malin 

Hal G. Marshall 

Leonard Martin 

Lowell Observatory 

Box 1269 

Flagstaff, AZ 86002 

Jet Propulsion Laboratory 

4800 Oak Grow Drive 

Pasadena, CA 91 109 

Jet Propulsion Laboratory 

4800 Oak Grove Drive 

Pasadena, CA 91 IO9 

Terry Z. Martin 

John V. Martonchik 

Harold Masursky 

U.S. Geological Suwey 

2255 North Gemini Drive 

Flagstaff, AZ 86001 

Jet Propulsion Laboratory 

4800 Oak Grove Drive 

Pasadena, CA 91 109 

Daniel J. McCleese 

Thomas B. McCord 

Planetary Geosciences Division 

Hawaii Institute of Geophysics 

2525 Caea Road 

Honolulu, HI 96822 

Michael B. McElroy 

Pierce Hall, Room lOOE 

Hmard Uniuersity 

Cambridge, MA 02 138 

Albert E. Metzget 

Mail Stop 183-501 

Jet Propulsion Laboratory 

4800 Oak Grove Drive 

Pasadena, CA 91 109 

Center for Meteorite Studies 

Arizona State University 

Tempe, AZ 85287 

U.S. Geological Sinwy 

345 Middlefield Road 

Menlo Park, CA 94025 

Carleton B. Mmre 

Henry J. Moore 

Jeff Moore 

Geology Department 

Arizona State University 

Tempe, AZ 85287 

Mail Code SN4 

NASAJohnson Space Center 

Hcuston, TX 77058 

Department of Geology and Geophysical Science 

Princeton University 

Princeton, NJ 08544 

Richard V. Morris 

Bruce Moskowitr 
18 MECAFinalReport 

Peter Mouginis-Mark 

Planetary Geosciolces Division 

Hdi Institute of Geophysics 

2525 Correa Road 

Honduly HI 96822 

Division of Geological and Planetary Science 

Caltech 

Pasadena, CA 91 125 

Mail Stop 693.0 

NASA Gcddard Space Flight Center 

Geenbelt, MD 20771 

Division of Geological and Planetary Science 

Caltech 

Pasadena, CA 91 125 

Astronomy RoFam 

Department of Earth and Space Science 

State Univmity of New York, Stony Brook 

Stony Brook, NY 1 1794 

Duane 0. Muhleman 

170-25 

Michael J. Mumma 

Bruce Murray 

170-25 

Tobias Owen 

David A. Paige 

Division of Geological and Planemy Science 

170-25 

Gdtech 

Pasadena, CA 91 125 

Frank Palluconi 

Mail Stop 183-501 

Jet Propulsion Laboratory 

4800 Oak Gcve Drive 

Pasadena,CA91109 

Tim Parker 

Mail Stop 183-501 

Jet RopurSion Laboratory 

4800 Oak Grove Driw 

Pasadena, CA 91 109 

School of Physics and Astrmy 

Univmity of Minnesota 

Minneapolis, MN 55455 

Robert 0. Pepin 

Gordon H. Pettingill 

54-618 

Massachusetts Znstirute of Technology 

Cmnbndge, MA 02 139 

Department of Geological Sciences 

Southem Methodist Uniwrsity 

D&, TX 75275 

Roger Phillips 

David C. Pieri 

Mail Stop 183-501 

Jet Ropulsion Laboratory 

4800 Oak Grove Driw 

Pasadena, CA 91 109 

Richard J. Pike 

U.S. Geological Sumy 

345 Middlefild Road 

Menlo Park, CA 94025 

James B. Pollack 

Mail Stop 245-3 

NASA Am Research Center 

Moffett Field, CA 94035 

Department of Geology and Geophysical Science 

Princeton Uniwsity 

Princeton, NJ 08544 

Planetary Geosciences Division 

Hawaii Znstitute of Geophysics 

2525 bea Road 

Honolulu, HZ 96822 

Mail Code EL4 

NASA Headquarters 

Washington, DC 20546 

Beaumont Building 

Univmity ofShefFeld 

Brookhill 

Sheffield S3 7HF England 

.Earth Science Department 

California State Polytechnic University 

3801 West Temple Avenrce 

Pomona, CA 91 768 

Mail Stop 183-701 

Jet Propulsion Laboratory 

4800 Oak Grow Driw 

Pasadena, CA 91 109 

Znstitute of Geophysics and Planetary Physics 

University of California, Los Angeles 

Lac Angeles, CA 90024 

Department of Geological Sciences 

Brown Univmity 

Rh, RZ 02912 

Laboratory for Planetary Studies 

Comell Univmity 

Space Sciences Building 

Zthaca, NY 14853-0355 

Mail Stop 183-501 

Jet Propulsion Laboratory 

4800 Oak Orow Driw 

Pasadena, CA 91 109 

MailStop239-12 

NASA Ames hearch Center 

Moffett Field, CA 94035 

Jessica Posey Dowty 

Susan Postawko 

William Quaide 

Colin Reid 

Lisa Rossbacher 

Ladislav E. Roth 

Christopher T. Russell 

Malcolm J. Rutherford 

Carl Sagan 

Steve Sunders 

Thomas W. Scattergood 
Technical Report 88-09 19 

F. Peter Schloerb 

Astronomy Department 

Graduate Tower B 

University of Massachusetts 

Amherst, MA 01 003 

Department of Geological Sciences 

&own University 

Providence, RI 02912 

Mail code EL4 

NASA Headquarters 

Washington, DC 20546 

Plnnetmy Geosciences Division 

Hawaii Institute of Geophysics 

2525 Correa Road 

Honolulu, HI 96822 

Mail Stop 169-506 

Jet Propulsion Laboratorj 

4800 Oak Gw Drive 

Pasadena, CA 91 109 

U.S. Geological Suswy 

2255 North Gemini Drive 

Fkstaff, AZ 8600 I 

Mail Stop 245-3 

NASA Ames Rewarch Center 

Moffett Field, CA 94035 

Department of Artsogeophysics 

Uniwrsity of Colorado 

Boulder, CO 80302 

Mail Stop 180-402 

Jet Propulsion Laboratory 

4800 Oak Grm Drive 

Fasadena,CA91109 

National Center fcr Atmospheric Research 

P.O. Box 3000 

Boulder, CO 80307 

Department of Chemistry, B-017 

Uniwrsity of Califomia, San Diego 

La Jolln, CA 92093 

Department of Atmospheric Sciences 

Mail Stop AK-40 

University of Washington 

Seattle, WA 981 95 

Mail Stop 245-3 

NASA Ames Research Center 

Moflett Field, CA 94035 

Peter Schultz 

David Scott 

Robert B. Singer 

James A. Slavin 

L. A. Soderblom 

Steven W. Squyres 

A. Ian Stewart 

Robert Steinbacher 

Carol Stoker 

Hans E. Suess 

James E. Tillman 

Owen B. Toon 

Marsha R. Torr 

Center for Atmospheric and Space Sciences 

Utah State Uniwrsity, UMC4 1 

Logan, UT84322 

G. Leonard Tyler 

Center for Radar Astronomy 

Stanford Uniwrsity 

Stanford, CA 94305 

Mail Stop 245-3 

NASA Ames Research Center 

Moffett Field, CA 94035 

Department of Geological Sciences 

Michigan State Uniwrsity 

East Lansing, MI 48824- 1 1 15 

Department of Applied Science 

New York University 

26 Stuywsant Street 

New York, NY 10003 

Hampton Watkins 

P.O. Box 2370 

Cmnbndge, MA 02238 

Mail Stop 183-301 

Jet Propulsion Laboratory 

4800 Oak Grw Drive 

Pasadena, CA 91 109 

US. Geological Sunq 

345 Middlefield Road 

Menlo Park, CA 94025 

U.S. Geological sutwy 

2255 North Gemini Drive 

Fkstafl, AZ 86001 

Pierce Hall, Room 1 OOE 

H-d Uniwrsity 

Canbridge, MA 02 I38 

Planetmy Geosciences Division 

Hawaii Institute of Geophysics 

2525 Correa Road 

Honolulu, HI 96822 

Lunar and Planetmy Institute 

3303 NASA Road One 

Houston, TX 77058 

Mail Stop T- 1 I66 

Jet Proputsion Lahatoy 

4800 Oak Gw Driue 

Pasadena,CA91109 

Jose R. Valentin 

Michael Velbel 

Tyler Volk 

Robert A. West 

Don E. Wilhelms 

Sherman Wu 

John Yatteau 

Aaron P. Zent 

Jim Zimbelman 

Richard W. Zurek 
I 

21 

Appendix 3. MECA Bibliography 

What follows is a compilation of papers and abstracts authored by participants in the 

MECA program during the period 1984-1988. Notably absent from this listing are abstracts 

from the last two MECA workshops: Polar Processes on Mars (to be issued as a NASA 

Technical Memorandum) and Dust on Mars I11 (to be published as an LPI Technical 

Report), neither of which had gone to press by the time this summary was ready for 

publication. While every effort has been made to ensure that this bibliography is otherwise 

complete, a few abstracts and papers have undoubtedly slipped through the cracks. This 

possibility should be kept in mind when using the bibliography for research purposes. 

Special thanks are due Mildred Dickey, who spent countless hours inputting and revising 

this bibliography, and to Stephen Tellier, of the Institute's Library Information Center, 

who compiled and maintains the Lunar and Planetary Bibliography Database from which 

many of these citations were originally obtained. 

Symbol notation: "'" MECA Principal Investigator, "*" Member MECA 

Study Group. 

Agresti D. G., Morris R. V.t, Newcomb J. A., and Lauer H. V., Jr. (1986) 

Spectral properties of selected soils from the dry valleys of Antarctica. 

In Lunar and Planetary Science XVII, pp. 3-4. Lunar and Planetary 

Institute, Houston. 

Agresti D. G., Newcomb J. A., and Morris R. V.t (1987) Mossbauer study 

of ultramicrocrystalline hematite. In Lunar and Planetary Science XVIII, 

pp. 7-8. Lunar and Planetary Institute, Houston. 

Ahrens T. J. (1986) Accretional constraints on Mars volatile budget. In 

MECA Workshop on the Evolution of the Martian Atmosphere (M. Carr, 

P. James, C. Leovy, R. Pepin, and J. Pollack, eds.), pp. 9-10. LPI Tech. 

Rpt. 86-07, Lunar and Planetary Institute, Houston. 

Anderson D. M.+ (1985) The present water cycle on Mars: Some 

thermodynamic considerations. In Workshop on Water on Mars, (S. 

Clifford, ed.), pp. 9-11. LPI Tech. Rpt. 85-03, Lunar and Planetary 

Institute, Houston. 

Anderson D. M.t and Brandstrom G. W. (1987) Evidence for glaciation 

in Elysium. In MECA Symposium on Mars: Evolution of its Climate 

and Atmosphere, (V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, 

C. Leovy, and T. Maxwell, eds.), pp. 15-17. LPI Tech. Rpt. 87-01, 

Lunar and Planetary Institute, Houston. 

Anderson D. M.t (1988) Water in the Martian regolith. In Workshop on Atmospheric HrO Observations of Earth and Mars. LPl Tech. Rpt., 

in press, Lunar and Planetary Institute, Houston. 

Arvidson R. E.t (1986) On the rate of formation of sedimentary debris 

on Mars. In MECA Workshop on Dust on Mars I1 (S. Lee, ed.), p. 

9. LPI Tech. Rpt. 86-09, Lunar and Planetary Institute, Houston. 

Arvidson R. E.t and Kahn R. (1985) The relative rates of aeolian and 

tectonic processes on Venus and Mars. In Lunar and Planetary Science 

XVI, pp. 17-18. Lunar and Planetary Institute, Houston. 

Baker V. R.t (1984) Problems in the paleohydrologic and hydroclimatolcgic 

interpretation of valley networks. In Workshop on Water on Mars (S. 

Clifford, ed.), pp. 4-5. LPI Tech. Rpt. 85-03, Lunar and Planetary 

Institute, Houston. 

Baker V. R.t (1984) Fluvial erosion of impact craters: Earth and Mars. 

Baker V. R.t (1985) Models of fluvial activity on Mars. In Models in 

Geomorphology (M. Woldenber, ed.), pp. 287-312. Allen & Unwin, 

Boston. 

NASA TM-86246, pp. 175-1 77. 

Baker V. R.t (1985) Paleohydrologic implications of valley networks on 

Baker V. R.t (1986) Evolution of small valley networks in the heavily 

Baker V. R.t (1986) Evolution of valleys dissecting volcanoes on Mars 

Baker V. R.t and Gulick V. C. (1987) Fluvial valleys on Martian volcanoes. 

Baker V. R.t and Gulick V. C. (1987) Valley development on Hawaiian 

volcanoes. NASA TM-898 IO, pp. 297-299. 

Baker V. R.' and Kochel F. R. C. (1984) Valley network development 

by spring sapping. Geol. Soc. Arner. Abst. with Prog., 16, 435. 

Baker V. R.' and O'Connor J. E. (1986) Flow modeling of cataclysmic 

flood discharges. NASA TM-88383, pp. 274-276. 

Baker V. R.t and Partridge J. B. (1984) Morphometry of small valley 

networks on Mars. In Lunar and Planetary Science XV, pp. 23-24. Lunar 

and Planetary Institute. 

Baker V. R.t and Partridge J. B. (1984) Pristine and degraded segments 

of small valley networks on Mars. In Lunar and Planetary Science XV, 

pp. 25-26. Lunar and Planetary Institute, Houston. 

Baker V. R.t and Partridge J. B. (1986) Small Martian valleys: Pristine 

and degraded morphology. .I. Geophys. Res., 91, 3561-3572. 

Banin A.t (1986) Constraining Mars-dust mineralogy on the basis of Viking 

biology simulations and Mars spectral reflectance. In MECA Workshop 

on Dust on Mars I1 (S. Lee, ed.), pp. 10-11. LPI Tech. Rpt. 86-09. 

Lunar a$ Planetary Institute, Houston. 

Banin A. , Margulies L., and Chen Y. (1984) Iron-montmorillonite: 

Spectral analogy to Mars soil. In Lunar and Planetary Science XV, pp. 

31-32. Lunar and Planetary Institute, Houston. 

Banin A.t, Margulies L., and Chen Y. (1985) Iron-montmorillonite: A 

spectral analog of Martian soil. Proc. Lunar P/anet. Sci. Gmf. 151h, 

in]. Geo hys Res 90, C771-C774. 

Barnes J. R. (1984) Linear baroclinic instability in the Martian atmosphere. 

I. Atmos. Sci., 41, 1536-1550. 

Barnes J. R.t (1985) Transient baroclinic eddies in the atmospheres of 

Mars and Earth. IAMAP/IAPSO.Ioint Assembly Abstracts, p. 95. 

Barnes J. R.' and Hollingsworth J. L. (1985) Dynamical modeling of a 

Martian plar warming. Bull. Arner. Astron. Soc., 17, 733. 

Barnes J, R. and Hollingsworth]. L. (1986) Implications of a polar warming 

for dust transport into the north polar region of Mars. In Workshop 

on Dust on Mars I1 (S. Lee, ed.) pp. 12-13. LPI Tech. Rpt. 86-09, 

Lunar and Planetary Institute, Houston. 

Mars. NASA TM-87563, pp. 313-315. 

cratered terrains of Mars. NASA TM-88383, pp. 271-273. 

and Earth. NASA TM-88383, pp. 414-416. 

NASA TM-89810, pp. 294-296. 

e . " 

PRBCES)ING PAGE BLANK NOT FILMED 
22 MECA Final Report 

Barnes J. R' and Hollingsworth J. L. (1987) Numerical simulations of 

dust transport into northern high latitudes during a Martian polar 

warming. In MECA Symposium on Ma: Evolution of its Climate and 

Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, 

C. Leovy, and T. Maxwell, eds.), pp. 18-19. LPI Tech. Rpt. 87-01, 

Lunar and Planetary Institute, Houston. 

Barnes J. Rt and Hollingsworth J. L. (1987) Dynamical modeling of a 

planetary wave mechanism for a martian polar warming. Icm, 71, 

313-334. 

Barnes J. R.t and Hollingsworth J. L. (1988) Transport of Mars atmospheric 

water into high northern latitudes during a polar warming. In Workshop 

on Atmospheric H2O Observations of Earth and Man. LPI Tech. Rpt., 

in press, Lunar and Planetary Institute, Houston. 

Becker R. H. and Pepin R. O.t (1984) The case for a martian origin 

of the shergottites: Nitrogen and noble gases in EETA 79001. Emth 

Becker R. H. and Pepin R. O.t (1985) Nitrogen and light noble gases 

in the Shergotty meteorite. In hr and Planetary Science XVI, 

Supplement A, p . 1 2. Lunar and Planetary Institute, Houston. 

distribution of subsurface volatiles, Aeolis Quadrangle, Mars. In MECA 

Special Session at LPSC XVII: Martian Gemphobgy and its Relation 

to Subsutface Volatikr (S. Clifford, L. A. Rossbacher, and J. R. 

Zimbelman, eds.), pp. 12-13. LPI Tech. Rpt. 87-02, Lunar and Planetary 

Institute, Houston. 

Brakenridge G. R.', Newson H. E., and Baker V. Rt (1985) Ancient 

hot springs on Mars: Origin and paleoevironmental significance of 

martian valleys. Geology, 13, 859-862. 

Brakenridge G. R!, Newson H. E., and Baker V. R' (1985) Hot springs 

on Mars: Origins and paleoenvironmental significance of small martian 

valleys. Geol. Soc. Amer. Abst. with Prog., 17, 530. 

Brandenburg J. E. (1987) The paleo-ocean of Mars. In MECA Symposium 

on Mms: Evolution of its Climate and Atmosphere (V. hker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

pp. 20-22. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Bruckenthal E. A. and Singer R. B.t (1987) Spectral effects of dehydration 

of phyllosilicates. In Lunm and Planetary Science XVIII, pp. 135-136. 

Lunar and Planetary Institute, Houston. 

Calvin W. M., Jakosky B. M.t, and Christensen P. R.' (1987) A model 

of diffuse radar scattering from martian surface rocks. NASA TMPlanet. Sci. Lett., 69, 225-242. 

Brakenridge G. R. P- (1987) Small valley networks and the past and present 

89810, p .245-247. 

Carr M. H. P (1984) Freezing of martian streams under different climatic 

conditions. NASA TM-86246, pp. 185-186. 

Carr M. H. (1984) Formation of martian valley networks as a consequence 

of large impacts. In Lunm and Planetary Science XV, pp. 131-132. Lunar 

and Planetary Institute, Houston. 

Carr M. H.t (1986) Water on Mars: History and current distribution. 

Roc. XXVl COSPAR, 149. 

Carr M. H.t (1986) Climatic implications of martian channels. In Workshop 

on the Evolution of the Martian Atmosphere (M. Carr, P. James, C. 

Leovy, R. Pepin, and J. Pollack, eds.), pp. 11-12. LPI Tech. Rpt. 86- 

07, Lunar and Planetary Institute, Houston. 

Carr M. H! (1986) Mars: A water-rich planet? Icancs, 68, 187-216. 

Carr M. H.' (1987) Water on Mars. Nature, 326, 30-35. 

Carr M. H.t (1987) Mars: A water-rich planet. In MECA Symposium 

on Mms: Evolution of its Climate and Atmosphere (V. Baker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

pp. 23-25. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Carr M. H.' (1987) Martian volcanism: A review. In MECA Symposium 

on Man: Evolution of its Climate and Atmosphere (V. Baker, M. Carr, 

F. Fanale, R Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

pp. 29-31. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Carr M. H.t (1987) The inventory and distribution of water on Mars. 

Carr M. H.t (1987) The Mapian surface. h. Geophys., 25, 285-292. 

Carr M. H?, Lovy C. B. , and Pepin R. O.', eds. (1985) Workshop 

on the Evolution of the Mastian Atmosphere. LPI Tech. Rpt. 86-07, 

Lunar and Planetary Institute, Hpton. 52 pp. 

Carroll M. R. and Rutherford M. J. (1985) Sulfide and sulfate saturation 

in hydrous silicate melts. Roc. Lunar Planet. Sci. ISth, inJ. Geophys. 

Res., 90, C601-C612. 

Chen R. C. (1988) The effect of global-scale divergent circulation of 

the atmospheric water vapor transport and maintenance. In Workshop 

on Atmospheric H20 Observations of Emth and Man. LPI Tech. Rpt., 

Lunar and PlanEtary Institute, Houston, in press. 

Christensen P. R. (1984) The origin of regional dust deposits on Mars. 

In hnm and Planetary Science XV, pp. 148-149. Lunar and Planetary 

Institute, Houstgn. 

Christensen P. R. (1984) Thermal emissivity of the martian surface: 

Evidence for compositional variations. In Lunar and Planetary Science 

XV, pp. 150-15!. Lunar and Planetary Institute, Houston. 

Christensen P. R. (1985) The origin of regional dust deposits on Mars. 

Christensen P. R. (1985) Regional dust deposits on Mars: Origin, age, 

and geologic history. In Workshop on Durt on Man (S. Lee, ed.), pp. 

1-2. LPI Tech. bpt. 85-02, Lunar and Planetary Institute, Houston. 

Christensen P. R. (1986) Albedo variations of the martian surface and 

atmosphere. EQS Trans. AGU, 67, 301. 

Christensen P. R. (1986) Dust deposition and erosion on Mars: Cyclic 

development of regional deposits. In Workshop on Dust on Mars ZI 

(S. Lee, ed.), pp. 14-16. LPI Tech. Rpt. 86-09, Lunar and Planetary 

Institute, Houston. 

Christensen P. R.* (1986) Regional dust deposits on Mars: Origin, age, 

and geologic histfry. NASA TM-88383, pp. 237-238. 

Christensen P. R. (1986) Regional dust deposits on Mars: Physical 

properties, age ?nd history. J. Geophys. Res., 91, 3533-3546. 

Christensen P. R. (1986) Seasonal variability of martian surface albedos: 

Implications for yearly dust deposition and removal. In Lunar and 

Planetary Science XVII, pp. 121-122. Lunar and Planetary Institute, 

Houston. 

Christensen P. R.* (1986) Surface albedo variations on Mars: Implications 

for yearly dust deposition and removal. In Wurkshop on Dust on MMS 

11 (S. Lee, ed.), pp. 17-19. LPI Tech. Rpt. 86-09, Lunar and Planetary 

Institute, Housgon. 

Christensen P. R. (1987) Variations of martian surface albedo: Evidence 

for yearly dust {eposition and removal. NASA TM-89810, pp. 167-169. 

Christensen P. R. (1987) Global albedo variations on Mars: Implications 

for active aeolian transport, deposition, and erosion. Submitted to J. 

Geophys. Res. 

Christensen P. R.* and Zurek R. W.t (1984) Martian north polar hazes 

and surface ice: Results from the Viking Survey/Completion Mission. 

J. Geophys. Res.,*89, 4587-4596. 

Christensen P. R. and Zurek R. W.t (1984) Martian north polar hazes 

and surface ice: Results from the Viking Surveylcompletion mission. 

J. Geophys. Res., 89, 4587-4596. 

Christensen P. R. and Zurek R. W? (1984) Mars water-ice clouds. In 

Workshop on Water on Mars (S. Clifford, ed.), pp. 14-16. LPI Tech. 

Rpt. 85-03, Lunp and Planetary Institute, Houston. 

Christensen P. R. , Kieffer H. H., and Chase S. (1985) Determination 

of martian surface composition by thermal infrared spectral observation. 

In LuMr and Planetary Science XVI, pp. 125-126. Lunar and Planetary 

Institute, Housgon. 

Christensen P. R. , Jaramillo L., and Greeley R! (1985) Water-ice clouds 

on Mars: Location and seasonal variation. NASA TM-87563, pp. 

389-390. 

Christensen P. R.*, Zurek R. W.', and Greeley R.' (1986) Mars waterice clouds. NASA TM-88383, pp. 512-514. 

Advances in Space Research, 7, 85-94. 

NASA TM-87S03s pp. 295-2%. 
Christensen P. R.', Zurek R. W.t, and Jaramillo L. L. (1986) Seasonal 

and diurnal variability of Mars water-ice clouds. In Lunar and Planetmy 

Science XWI, pp; 123-124. Lunar and Planetary Institute, Houston. 

Christensen P. R. , Zurek R. W.t, and Jaramillo L. L. (1988) Seasonal 

and diurnal variability of Mars water-ice clouds. In Workshop on 

Atmospheric H2O Observations of Earth and Mars. LPI Tech. Rpt., 

Lunar 'and Planeiary Institute, Houston, in press. 

Christiansen E. H. and Hopler J. A. (1987) Geomorphic evidence for 

subsurface volatile reservoirs in the Elysium region of Mars. In MECA 

Special Session at LPSC XWl: Martian Geomorphology and its Relation 

to Subsurface Volatiles (S. Clifford, L. A. Rossbacher, and J. R. 

Zimbelman, eds.), pp. 14-15. LPI Tech. Rpt. 87-02, Lunar and Planetary 

Institute, Houston. 

Clark B. C. (1987) Comets, volcanism, the salt rich regolith and cycling 

of volatiles on Mars. In MECA Symposium on Mars: Evolution of its 

Climate and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, 

R. Haberle, C. kovy, and T. Maxwell, eds.), pp. 29-31. LPI Tech. 

Rpt. 87-0.1, Lunar and Planetary Institute, Houston. 

Clark B. C. (1987) Comets, volcanism, the salt-rich regolith, and cycling 

of volatilespn Mars. kana, 71, 250-256. 

Clifford S. M. (1984) Do the martian polar caps have equilibrium profiles? 

EOS Tram. PGU, 56,979. 

Clifford S. M. , ed. (1985) Workshop on Water on Mars. LPI Tech. Rpt. 

85-03, Lunar and Planetary Institute, Houston. 105 pp. 

Clifford S. M.' (1985) Mars: Groundwater mound development in response 

to polar basal melting. In Workshop on Water on Mars (S. Clifford, 

ed.), pp. 17-19. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. 

Clifford S. M.' (1985) Mars: Permeability requirements for a global 

groundwater system driven by polar basal melting. In Workshop on 

Water on Mars (S. Clifford, ed.), pp. 20-22. LPI Tech. Rpt. 85-03, 

Lunar and Planetary Institute, Houston. 

Clifford S. M.' (1986) Mars: Where has all the water gone? Sky &Telescope, 

72, 20. 

Clifford S. M.' (1987) Polar basal melting on Mars. J. Geophys. Res., 92, 

9135-9152.. 

Clifford S. M. (1987) Theoretical equilibrium profiles of the martian 

perennial polar caps. In Lunm and Planetary Science XWII, pp. 189-190. 

Lunar and Pknetary Institute, Houston. 

Clifford S. M. (1987) Mars: Crustal pore volume, cryospheric depth, 

and the global Occurrence of groundwater. In MECA Symposium on 

Mars: Evolution of its Climate and Atmosphere (V. Baker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

pp. 32-34. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Clifford S. M.' (1988) The interpretation of data from the Viking Mars 

Atmospheric Water Detectors (MAWD): Some points for discussion. 

In Workrhop on Atmospheric H.70 Obsmatim of Earth and Mars. 

LPI Tech. Rpt., Lunar and Planetary Institute, Houston, in press. 

Clifford S. M. and Bartels C. J. (1985) MARSTHERM: A FORTRAN 

77 finite-difference thermal model available for general distribution. 

and Bartels C. J. (1986) The Mars Thermal Model 

(MARSTHERMI: A FORTRAN 77 finite-difference thermal model 

designed for general distribution. In LUMT and Planetary Science XWI, 

pp. 142-143; Lunar and Planetary Institute, Houston. 

Clifford S. M. and Fanale F. P.' (1985) The thermal conductivity of 

the martian crust. In Lunar and Planetary Science XVl, pp. 144-145. 

Lunar and Planetary Institute, Houston. 

Clifford S. M.' and Haberle R. M.t, eds. (1988) Workshop on Atmospheric 

H20 Observations of the Earth and Mars. LPI Tech. Rpt., Lunar and 

Planetary Institute, Houston, in press. 

Clifford S. M.' and Hillel D. (1986) Knudsen diffusion: The effect of 

small pore size and low gas pressure on gaseous transport in soil. Soil 

Sci., 141, 289-299. 

Bdl. Amer. @Ton. SIX., 17,738. 

Clifford S. M. 

Clifford S. M.' and Huguenin R. L.' (1988) Regolith water vapor sources 

on Mars: A historical bibliography. In Workshop on Atmospheric H20 

Observations ofthe Emth and Mars. LPI Tech. Lpt., Lunar and Planetary 

Institute, Hpuston, in press. 

Clifford S. M. , Rossbacher L. A:. and Zimbelman J. R.', eds. (1987) 

MECA Special Session at LPSC XWl: Martian Geomorphology and its 

Relation to Subsuljace Vdatiles. LPI Tech. Rpt. 87-02, Lunar and 

PlanetaryJnstitute, Houston. 51 pp. 

Clow G. D. (1984) Use of planetary boundary layer model for martian 

paleoclimates. In Lunar and Planetmy Science XV, pp. 176-177. Lunar 

and PlanEtary Institute, Houston. 

Clow G. D. (1985) Radiation-dominated snowmelt on Mars. In Workshop on Water on Man (S. Clifford, ed.), pp. 23-24. LPI Tech. Rpt. 85- 

03, Lunar and Planetary Institute, Houston. 

Clow G. D.' (1987) Generation of liquid water on Mars through the 

melting of a'dusty snowpack. lcacs, 72, 95-127. 

Colburn D. S. , Pollack J. , and Haberle R. M.t (1986) Influence of dust 

on water condensation at Mars. In MECA Workshop on Duct on Mars 

II (S. Lee, ed.) pp. 20-22. LPI Tech. Rpt. 86-09, Lunar and Planetary 

Institute, Hpuston. 

Colburn D. S. , Pollack J. , and Haberle R. M.' (1988) Factors governing 

water condensation in the martian atmosphere. In Workshop on 

Atmospheric H2O Observations of Earth and Man. LPI Tech. Rpt.. 

Lunar and Planetary Institute, Houston, in press. 

Costard F. and Dollfus A. (1987) Ice lenses on Mars. In MECA Special 

session ar LPsc XWf: Martian ~eomorphobgy and its Refation to 

Subsurface Volatiles (S. Clifford, L. A. Rossbacher, and J. R. Zimbelman, 

eds.), pp. 16-17. LPI Tech. Rpt. 87-02, Lunar and Planetary Institute, 

Houston. 

Dale-Bannister M., Arvidson &', Snger R.t, and Bruckenthal E. A. (1985) 

Observed upper limits for clay minerals on Mars. In L~MT and Planetmy 

Science XW, pp. 787-788. Lunar and Planetary Institute, Houston. 

Dale-Bannister M., Arvidson R.t, Singer RSt, and Bruckenthal E. (1985) 

The search for igneous minerals at the Viking Lander Sites. In LUMT 

and Planetmy Science XW, pp. 161-162. Lunar and Planetary Institute, 

Houston. 

DeHon R. A. (1987) Ring furrows: Inversion of topography in martian 

highland terrains. kana, 71, 287-297. 

Donner L. J. (1988) Cumulus convection and the terrestrial water-vapor 

distribution. In Workshop on Atmospheric H2O Observations of Earth 

and Mars. LPI Tech. Rpt., Lunar and Planetary Institute, Houston, 

in press. 

Drake D. M., Feldman W. C., Reedy R. C., and Jakosky B. M.t (1987) 

Neutron mode of the Mars Observer Gamma Ray Spectrometer. In 

Lunar and Planetary Science XWIl, pp. 244-245. Lunar and Planetary 

Institute, Houston. 

Drake D. M., Muhleman D. O.', Berge G. L., and Jakosky B. M.' (1987) 

Martian neutron albedo spectra. Submitted toJ. Geophys. Res. 

Dreibus G. and Wanke H? (1985) Mars, a volatile-rich planet. Meteoritics. 

20,367-381. 

Dreibus G. and Wanke H! (1986) Comparison of CllBr and Br/I ratios 

in terrestrial samples and SNC meteorites. In MECA Workshop on 

the Evolution of the Martian Atmosphere (M. Carr, P. James, C. Leovy, 

R. Pepin, and J. Pollack, eds.), pp. 13-14. LPI Tech. Rpt. 86-07, Lunar 

and Planetary Institute, Houston. 

Dreibus G. and Wanke H! (1987) Volatiles on Earth and Mars: A 

comparison. lcacs, 7I,225-ZO40. 

Duxbury E. and Clifford S. M. (1987) Minimum rampart crater onset 

diameters in the equatorial region of Mars. EOS Tram. AGU, 68, 

344. 

Elfstrom A. and Rossbacher L.' (1985) Erosional remnants in the Baldakatj 

area, Lapland, northern Sweden: A terrestrial analog for martian 

landforms. Geografiska An&, 67, 167-176. 

Evans L. G. and Squyres S. W.' (1987) Investigation of martian volatiles 

via gamma-ray spectroscopy. J. Geophys. Res., 92,9153-9167. 
Fanale F. P!, Salvail J. R., Zent A. P.., and Postawko S. E.’ (1984) 

Mars: Astronomical effects on regolith HzO state. Bdl. Amer. Astron 

Soc., 16, 674. 

Fanale F. P.t, Salvail J. R., Zent A. P.*, and Postawko S. E.* (1984) 

Mars: Long term changes in the state and distribution of Hz0. In 

Workshop on Water on Man (S. Clifford, ed.), p. 25. LPI Tech. Rpt. 

85-03, Lunar and Planetary Institute, youston. 

Fanale F. P.t, Salvail J. R., Zent A. P. , and Postawko S. E.’ (1985) 

Mars: Long term changes in the state and distribution of H20. In 

Ices in the Solar System 0. Klinger, D. Benest, A. Dollfus, and R. 

Smoluchowski, eds.), pp. 535-564. D. $eidel, Dordrecht. 

Fanale F. P.t, Salvail J. R, Zent A. P. , and Postawko S. E.* (1985) 

Global distribution and migration of subsurface ice on Mars. In hnm 

and Planetary Science XVI, p. 231. Lunar and Planetary Institute, 

Houston. 

Fanale F. P.t, Postawko S. E.’, Zent A. P.., and Salvail J. R. (1986) 

Is regolith adsorption the explanation for the transition from early 

to present Mars climate? In MECA Symposium on Mars: Evolution of 

its Climate and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, 

R Haberle, C. Leovy, and T. Maxwell, eds.), pp. 21-22. LPI Tech. 

Rpt. 87-01, Lunar and Planetary Institpe, Houston. 

Fanale F. P!, Salvail J. R., Zent A. P. , and Postawko S. E.* (1986) 

Global distribution and migration of subsurface ice on Mars. Icaw, 

Fanale F. P.t, Postawko S. E.’, Zent A. P.*, and Salvail J. R. (1987) 

The role of regolith adsorption in the transition from early to late 

Mars climate. NASA TM-89810, pp. 161-164. 

Frey H. (1987) Pseudocracters as indicators of ground ice on Mars. In 

MECA Special Session at LPSC XVII: Martian Geomorphology and its 

Relation to Subsurface Volatikc (S. Clifford, L. A. Rossbacher, and J. 

R. Zimbelman, eds.), pp. 18-19. LPI Tech. Rpt. 87-02, Lunar and 

Planetary Institute, Houston. 

Garvin J. G., Ulaby F. T., Smith D. E., Frey H. V., Solomon S., and 

Zwally H. J. (1987) Martian surface physical properties to be derived 

by radar altimeter on the Mars Observer Spacecraft. In MECA 

Symposium on MMS, Evolution of its Climate and Atmosphere (V. Baker, 

M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, 

eds.), pp. 37-39. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. , Gibson E. K. , Jr. (1985) Sources and sinks of present day water within 

the martian regolith: Evidence from a terrestrial analog of Martian 

weathering processes-the dry valleys of Antarctica. In Workshop on 

Water on Mars (S. Clifford, ed.) pp. 26-28. LPI Tech. Rpt. 85-03, 

Lunar and Planetary Institute, Houston. 

Goettel K. A. (1986) Rigorous constraints on the bulk composition and 

volatile inventory of Mars. In MECA Workshop on the Evolution of 

the Martian Atmosphere (M. Carr, P. James, C. Leovy, R. Pepin, and 

J. Pollack, eds.), pp.15-16. LPI Tech. Rpt. 86-07, Lunar and Planetary 

Institute, Houston. 

Gooding J. L.* (1984) Do igneous rocks fall from Mars and beyond? 

Geotimes, 29, 29-30. 

Gooding J. L. (1985) Water and ice in the martian regolith: Dependence 

of stabilities on regolith mineralogy. In Workshop on Water on Mms 

(S. Clifford, ed.), pp. 29-31. LPI Tech. Rpt. 85-03, Lunar and Planetary 

Institute, Houston. 

Gooding J. L! (1986) Martian dust particles as condensation nuclei: A 

preliminary assessment of mineralogical factors. Icm, 66, 56-74. 

Gooding J. L.t (1986) Martian weathering products: Response to climate 

changes and effects on volatile inventories. In MECA Workshop on 

the Evolution of the Mmtian Atmosphere (M. Carr, P. James, C. Leovy, 

R. Pepin, and J. Pollack, eds.), pp. 17-18. LPI Tech. Rpt. 86-07, Lunar 

and Planetary Institute, Houston. 

Gooding J. L! (1986) Condensation of frosts on martian dust particles. 

In MECA Workshop on Duct on Mars 11 (S. Lee, 4.1, pp. 23-25. LPI 

Tech. Rpt. 86-09, Lunar and Planetary Institute, Houston. 

67, 1-18. 

Gooding J. L.’ 11987) Are SNO smoked or salted? Geotiw, 32, 10-11. 

Gooding J. L. (1987) Undercooled water in basaltic regoliths and 

implications for fluidized debris flows on Mars. Icmur, 72, 519-527. 

Gooding J. L.t (1987) Water-ice in the martian regolith: Experimental 

investigation of lithologic effects. In MECA Special Session at LPSC 

XVII: Martian Geomorphology and its Relation to SubsMface Volatikc 

(S. M. Clifford, L. A. Rossbacher, and J. R. Zimbelman, eds.), pp. 20-21. 

LPI Tech. Rpt. 87-02, Lunar and Planetary Institute, Houston. 

(1987) Non-equilibrium freezing of water-ice in sandy 

basaltic regoliths and implications for fluidized debris flows on Mars. 

Gooding J. L.t (1988) Possible significance of HzO-ice in the martian 

atmospheric water cycle. In Workshop on Atmospheric H20 Observations 

of Earth and Mms. LPI Tech. Rpt., in press, Lunar and Planetary 

Institute, +uston. 

Gooding J. L. and Muenow D. W. (1986) Martian volatiles in shergottite 

ERA 79001: New evidence from oxidized sulfur and sulfur-rich 

aluminosili*ates. Gemhim. Cosmochim. Acta, 50, 1049-1059. 

Gooding J. L. and Wentworth S. J. (1987) Calcium carbonate and calcium 

sulfate in martian meteorite EETA79001. NASA TM-89810, pp. 

158-159. 

Greeley R.t (1986) Aeolian activity as a planetary process. In Physics 

of Desertijication, (F. El-Baz and M.H.A. Hassan, eds.), pp. 159-190. 

Greeley R! (1986) Dust storms on Mars: Mechanisms for dust-raising. 

Greeley R.t (1986) Toward an understanding of the martian dust cycle. 

In Workshop on Dust on MUTS II (S. Lee, ed.), pp. 22-24. LPI Tech. 

Rpt. 86-09, Lunar and Planetary Institute, Houston. 

Greeley Rt (1986) Martian dust: The case for “para.” In Workshop on Dust on Mass I1 (S. Lee. ed.). pp. 25-27. LPI Tech. Rpt. 86-09, 

Lunar and Planetary Institute, Houston. 

Greeley R.t (1986) Water on Mars: Amounts and timing released in 

association with volcanism. EOS Trans. AGU, 67, 1074. 

Greeley Rt (1987) The martian dust cycle: A proposed model. In MECA 

Symposium on MMS: Evolution of its Climate and Atmosphere (V. Baker, 

M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, 

eds.), pp. 43-45. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Greeley R! (1987) Release of magmatic water on Mars: Estimated timing 

and vo1umes.h MECA Symposium on Mars: Evolution of its Climate 

and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, R Haberle, 

C. Leovy, and T. Maxwell, eds.), pp. 40-43. LPI Tech. Rpt. 87-01, 

Lunar and Planetary Institute, Houston. 

Greeley R.t (1987) Release of juvenile water on Mars: Estimated amounts 

and timing associated with volcanism. Science, 236, 1653-1654. 

Greeley Rt, Williams S., White B. R., Pollack J!, Marshall J., and Krinsley 

D. (1984) Abrasion by aeolian particles: Earth and Mars. NASA-CR3788, p. 50. 

Greeley R.t, Williams S. H., White B. R., Pollack J., and Marshall J. 

R. (1985) Wind abrasion on Earth and Mars. In Modek in Geomorphology 

(M. Woldenberg, ed.), pp. 373-422. Allen and Unwin, Boston. 

Guinness E. A:, Leff C. E., and Arvidson R. E! (1985) On the latitudinal 

distribution of debris in the northern hemisphere of Mars. In Workshop on Water on Mars (S. Clifford, ed.), pp. 32-34. LPI Tech. Rpt. 85- 

03, Lunar an$ Planetary Institute, Houston. 

Guinness E. A. , Arvidson R. E!, Dale-Bannister M. A., Singer R!,and 

Bruckenthal E. A. (1987) On the spectral reflectance properties of 

materials exposed at the Viking landing sites. J. Geophys. Res., 92, 

Gulick V. C. and Baker V. R.+ (1986) Evolution of valley networks on 

Mars: The Hawaiian analog. Geol. Soc. Ame~. Abst. with Prog., 18, 623. 

Gulick V. C. and Baker V. R.t (1987) Origin and evolution of valleys 

on martian volcanoes: The Hawaiian analog. In LWUT ad Planetary 

Science XVIII, pp. 376-377. Lunar and Planetary Institute, Houston. 

Gooding J. L. 

NASA TM-898 IO, pp. 305-306. 

NASA TM-88383, pp. 242-244. 

575-587. 
Tachnkal Report 88-09 25 

I 

Haberle R. M.' (1985) Hidden carbon dioxide on Mars. Natuze, 318, 

599-600. 

Haberle R. M? (1986) Interannual variability of great dust storms on 

Mars. Science, 234,459-461. 

Haberle R. M.' (1986) The development of global dust storms: The tole 

of the mean meridional circulation. In MECA Workshop on Dust on 

Mars II (S. Lee, ed.), pp. 32-33. LPI Tech. Rpt. 86-09, Lunar and 

Planetary Institute, Houston. 

Haberle R. M.t (1986) The climate of Mars. Sci. Am., 254, 54-62. 

Haberle R M.+ (1987) Interannual variability of global dust storms on 

Mars. In MECA Symposium on Mars: Evolution of its Climate and 

Atmosphere (V. Baker, M. Cart, F. Fanale, R. Greeley, R Haberle, 

C. Leovy, and T. Maxwell, eds.), p. 46. LPI Tech. Rpt. 87-01, Lunar 

and Planetary Institute, Houston. 

Haberk R. M.' (1988) On the vertical distribution of water vapor in 

the martian tropics. In Workhop on Atmospheric H20 Observatium 

of Earth and Mars. LPl Tech. Rpt., in press, Lunar and Planetary 

Institute, Houston. 

Haberle R. M.' and Herdtle T. (1985) Numerical simulation of the current 

water cycle on Mars. In Workhog on Water on Mars (S. Clifford, ed.), 

p. 35. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, Houston. 

Haberle R. M.? and Jakosky B. M.+ (1987) Transport of water from the 

residual north polar cap on Mars. In Lunm and Planetq Science XVIII, 

pp. 378-379. Lunar and Planetary Institute, Houston. 

HaleaErlich W. S. (1987) Implications for substrate kolatile distributions 

on Mars from complex crater morphology and morphometry. In MECA 

Special Session at LPSC XVII: Martian Geomorphobgy and its Relation 

to Subsurface Volatiks (S. M. Clifford, L. A. Rossbacher, and J. R. 

Zimbelman, eds.), pp, 22-23. LPI Tech. Rpt. 87-02, Lunar and Planetary 

Institute, Houston. 

Harris S. L, and Huguenin R. L.? (1987) Chemical frost weathering of 

olivine: Experimental study and implications. In MECA Symposium 

on Mats: Evolution of its Climate and Atmosphere (V. Baker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

pp. 47-49. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Hart H. M. and Jakosky B. M.+ (1985) Stability and composition of 

condensate at the Viking Lander 2 site on Mars, In Workshop on Water 

on Mars (S. Clifford, ed.), pp. 36-37. LPI Tech. Rpt. 85-03, Lunar 

and Planetary Institute, Houston. 

Hart H. M. and Jakosky 8. M.t (1986) Composition and stability of the 

condensate observed at the Viking Lander 2 site on Mars. Icaw, 66, 

Hart H, M. and lakosky 8. M.t (1987) Vertical distribution of water 

vapor in the atmosphere of Mars: Error analysis and preliminary results. 

In Lunar and Pfanetary Science XVIII, pp. 387-388. Lunar and Planetary 

Institute, Hquston. 

Herkenhoff K. (1986) Dust scattering at the martian terminator during 

the Mariner 9 Mission. In MECA Workshop on Duct on Mms (S. Lee, 

ed.), pp. 34-36. LPI Tech. Rpt. 86-09, Lunar and Planetary Institute, 

Houston. 

Horner V. M. and Greeley R.t (1987) Effects of elevation and plains 

thicknesses on martian crater ejecta morphologies for the ridged plains. 

In MECA Special Session at LPSC XWl: Martian Geomorphology and 

its Relation to Subsurfnce Vdatiles (S. M. Clifford, L. A. Rossbacher, 

and J. R. Zimbelman, eds,), pp. 24-25. LPI Tech. Rpt. 87-02, Lunar 

and Planetary Institute, Houston. 

Horner V. M. and Greeley R> (1987) Effects of elevation and ridged 

plains thickness on martian crater ejecta morphology. J. Geophys. Res., 

Horner V. M. and Zimbelman J. R.* (1986) Viking IRTM studies of the 

Crater Curier. In LUWT and Planetaq Science XVII, pp. 360-361. Lunar 

and Planetary Institute, Houston. 

134-142, 

92,561-569. 

Huguenin R. L.' (1985) Mars: Mineralogical constraints on volatile 

evolution. In Workshop on Water on Mms (S. Clifford, ed.), pp. 38-40. 

LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, Houston. 

Huguenin R. L.? (1987) Mars low albedo regions: Possible map of nearsurface H20. In MECA Symposium on Mars: Evolution of its Climate 

Md Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, R Haberle, 

C. Leovy, and T. Maxwell, eds.), pp. 50-52. LPI Tech. Rpt. 87-01, 

Lunar and Planetary Institute, Houston. 

Huguenin R. L.+ (1987) Photochemical weathering and contemporary 

volatile loss on Mars. In MECA Symposium on Mars: Evolution of its 

Climate and Atmosphere (V. Baker, M, Garr, F. Fanale, R. Greeley, 

R. Haberle, C. Leovy, and T. Maxwell, eds.), pp. 53-56. LPI Tech. 

Rpt. 87-01, Lunar and Planetary Institute, Houston. 

Huguenin R. L! (1987) The silicate component of martian dust. la, 

Huguenin R. L? and Harris S. L. (1986) Accreted HzO inventory on 

Mars. In MECA Wmkshop a tk Evolution of the Mattian Atmosphere 

(M. Carr. P, James, C. Leovy, R. Pepin, and 1. Pollack, eds.), pp. 19-22. 

LPI Tech. Rpt. 86-07, Lunar and Planetary Institute, Houston. 

Huguenin R. L.f, Harris S., and Carter R (1985) Freezehhaw injection 

of dust into the martian atmosphere, In Lunm and Planetary Science 

XW, pp. 376-377. Lunar and Planetary Institute, Houston. 

Huguenin R. L?, Harris S. L., and Carter R. (1986) Injection of dust 

into the martian atmosphere: Evidence from the Viking gas exchange 

experiment. Icancs, 68,99-119. 

Hunt G. E. andJames P.t (1985)Martian cloud systems: Current knowledge 

and future observations. Adv. in Space Res., 5, 93-99. 

Hunten D. M., Pepin R. O.+, and Walker J. C. G. (1987) Mass-fractionation 

in hydrodynamic escape. Icarus, 69,532-549. 

Iversen J. D. and Greeley R.' (1984) Martian crater dark streak lengths: 

Explanation from wind tunnel experiments. Jcaw, 58,358-362. 

lwasaki K., Saito Y., and Akabane T. (1987) Interannual differences in 

the regressions of the polar caps of Mars. In MECA Symposium on 

Urns: Evolution of its Climate and Atmosphere (V. Baker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

pp. 57-59. LPI Tech, Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Iakosky B. M.' (1984) The seasonal cycle of water on Mars. EOS Truns. 

AGU, 65,979. 

Jakosky B. M.' (1985) The seasonal cycle of water on Mars. Space Si. 

Jakosky B. M.' (1985) Thermal properties of martian fmes. In Workshop 

on Dust on Mars (S. Lee, ed.), p. 6. LPI Tech. Rpt. 85-02, Lunar 

and Planetar Institute, Houston. 

Jakosky B. M. (1986) On Mars: Remote sensing examines surface. 

Jakosky B. M.+ (1986) On the thermal properties of the martian fines. 

Iakosky B. M? (1986) Remote sensing examines surface. Cieotims, 31, 

Jakosky 8. M? (1987) Sublimation of water from the residual notth polar 

cap on Mats. In LuMt and Planetary Science XVIII, p, 455. Lunar and 

Planetary Institute, Houston. 

Jakosky €3. M.t (1987) Sudace-atmosphere interactions on Mars. Internat. 

Union Geod. Geophys., 1 95. 

Jakosky B. M.+( 1988)The behavior of water vapor in the Mars atmosphere. 

In worksh.Jp on Amp& H20 Observations of bh and Mms. 

LPI Tech. Rpt., in press, Lunar and Planetary Institute, Houston. 

Jakosky B. M.' and Barker E. S. (1984) comparison of ground-based and 

Viking Orbiter measurements of martian water vapor: Variability of 

the seasonal cycle. Jcmus, 57,322-334. 

Jakosky B. M.+ and Carr M, H.t (1984) Mars at high obliquity: Possible 

precipitation of ice at low latitudes. BuU. AM. Astron. Soc., 16, 673. 

70, 162-188. 

Reu., 41, 131-200. 

Y 

Grntimes, 3 I, 28-30. 

ICUW, 66, 117-124. 

28-30. 
26 MECA Final Report 

Jakosky B. M.t and Carr M. H.' (1985) Possible precipitation of ice at 

low latitudes of Mars during periods of high obliquity. Nature, 315, 

559-561. 

Jakosky B. M.' and Christensen P. R.* (1984) Duricrusts on Mars: Evidence 

from thermal, radio, and radar data. In LUMT and Planetary Science 

W, pp. 397-398. Lunar and PlanetaJy Institute, Houston. 

Jakosky B. M.t and Christensen P. R. (1985) Interpretation of remotesensing observations of Mars. In Lunar and Planetary Science XVI, pp. 

392-393. Lunar and Planetary Instipte, Houston. 

Jakosky B. M.' and Christensen P. R. (1985) Global duricrust on Mars: 

Analysis of remote sensing data. In workshop on Dust on Mars (s. 

Lee, ed.), p. 7. LPI Tech. Rpt. 85-02, Lunar and Planetary Institute, 

Houston. 

Jakosky B. M.t and Christensen P. R.* (1986) Are the Viking Lander 

sites representative of the surface of Mars! In MECA Workshop on 

Dust on Mars II (S. Lee, ed.), pp. 37-38. LPI Tech. Rpt. 86-09, Lunar 

and Planetary Institute, Houston. 

Jakosky B. M.' and Christensen P. R.' (1986) Are the Viking landing 

sites representative of the surface of Mars? Icasus, 66, 125-133. 

Jakosky B. M.+ and Christensen P. R. (1986) Global duricrust on Mars: 

Analysis of remote sensing data. j. C+phys. Res., 91, 3547-3560. 

Jakosky B. M.t and Christensen P. R. (1986) Thermal properties of the 

martian surface. EOS Trans. AGU, 16, 301. 

Jakosky B. M.t and Lindner B. L. (1984) Mars atmospheric photochemistry, 

surface reactions, and climate change. In LUMT and Planetary Science 

XV, 399-400. Lunar and Plan$tary Institute, Houston. 

Jakosky B. M.t and Martin T. Z. (1987) Mars: North-Polar atmospheric 

warming during dust storms. Icarus, 72, 528-534. 

Jakosky B. M.', LaPointe M. R., and Zurek R. W.' (1987) The observed 

day-to-day variability of Mars water vapor. In MECA Symposium on 

Mars: Evolution of its Climate and Atmosphere (V. Eiaker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

p. 60. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, Houston. 

Jakosky B. M.', Thomas G. E., Rusch D. W., Barth C. A., Lawrence 

G. M., Oliver0 J. J., Clancy R. T., Sanders R. W., and Knapp B. G. 

(1988) Solar mesosphere explorer observations of stratospheric and 

mesospheric water vapor. In WorkshoponAtmosphericH20 Observations 

of hrth and Man. LPI Tech. Rpt., in press, Lunar and Planetary 

Institute, Houston. 

Jakosky B. M.', Zurek R. W.t, and LaPointe M. R. (1988) The observed 

day-to-day variability of Mars atmospheric water vapor. Icancs, 73, 

80-90. 

James P. B.t (1984) Martian local dust storms. In Recent Advances in 

Planetary Meteorology (G.E. Hunt, ed.), pp. 85-99. Cambridge Univ. 

Press, Cambridge. 

James P. B. (1985) Hydrologic cycle on Mars: Effects of COz mass flux 

on global water distribution. In Workshop on Water on Mms (S. Clifford, 

ed.), p. 44. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. 

James P. B.' (1986) The martian hydrologic cycle: Effects of COz mass 

flux on global water distribution. Icasus, 64, 249-264. 

James P. B.t (1987) The direction of water transport on Mars: A possible 

pumping mechanism. In MECA Symposium on Man: Evolution of its 

Climate and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, 

R. Haberle, C. Leovy, and T. Maxwell, eds.), pp. 62-63. LPI Tech. 

Rpt. 87-01, Lunar and Plane\ary Institute, Houston. 

(1986) Interannual variability in Mars 

south polar recessions and possible correlations with major dust storms. 

In MECA Workshop on Dust on Man I1 (S. Lee, ed.), pp. 29-40. LPI 

Tech. Rpt. 86-09, Lunar andFlanetary Institute, Houston. 

James P. B.' and Martin L. J. (1988) Circumpolar hoods and clouds 

and their relation to the martian Hz0 cycle. In Workrhop on Atmospheric 

H20 Obsmations of Emth and Man. LPI Tech. Rpt., in press, Lunar 

and Planetary Institute, Houston. 

James P. B.t and Martin L. J. 

James P. B.', Pierce M., and Martin L. 1.' (1987) Martian north polar 

cap and circumpolar clouds: 19751980 telescopic observations. Icasus, 

71, 306-312. 

James P. B.t, Malolepszy K. M., and Martin L. I.* (1988) Interannual 

variabijty of Mars south polar cap. lcancs, 71, 298-305. 

Jaquin F. (1986) The vertical distribution of aerosols during the growth 

phase of a global dust storm. In MECA Workshop on Dust on Mars 

I1 (S. Lee, ed.), p. 41. LPI Tech. Rpt. 86-09, Lunar and Planetary 

Instituge, Houston. 

Jaquin F. (1988) Very high elevation water ice clouds on Mars: Their 

morphology and temporal behavior. In Workshop on Atmospheric H2O 

Observations of Earth and Mars. LPI Tech. Rpt., in press, Lunar and 

Planet$ry Institute, Houston. 

Jaquin F. , Gierasch P., and Kahn R.* (1986) The vertical structure of 

limb hazps in the martian atmosphere. Icaw, 68, 442-461. 

Jons H.-P. (1984) Orcus Patera and its surroundings: A squeezed zone 

between two Mega-Aureoles? In LUMT and Planetary Science XV, pp. 

415-416. Lunar and Planetary Institute, Houston. 

Jons H.-P.* (1984) Sedimentary basins and mud flows in the northern 

lowlands of Mars. In LUMT and Planetary Science XV, pp. 417-418. 

Lunar aFd Planetary Institute, Houston. 

Jons H.-P. (1985) Late sedimentation and late sediments in the northern 

lowlands on Mars. In Lunar and Planetary Science XVI, pp. 414-415. 

Lunar a:d Planetary Institute, Houston. 

Jons H.-P. (1987) Arcuate ground undulations, gelifluxion-like features 

and "front tori" in the northern lowlands on Mars-What do they 

indicate? InMECASpecialSessionat LPSCXVII: MmtianGeomorphology 

and its Relation to Subsurface Volatiles (S. M. Clifford, L. A. Rossbacher, 

and J. R. Zimbelman, eds.), pp. 26-27. LPI Tech. Rpt. 87-02, Lunar 

and Planetary Institute, Houston. 

Kahn R.* (1984) The spatial and seasonal distribution of Martian clouds 

and ?me meteorological implications. J. Geophys. Res., 98, 6671-6688. 

Kahn R. (1985) Observational constraints on the global-scale wind systems 

of Mars. In Workshop on Water on Mars (S. Clifford, ed.), pp. 45-47. 

LPI Tzch. Rpt. 85-03, Lunar and Planetary Institute, Houston. 

Kahn R. (1985) The evolution of COz on Mars. lcasus, 62, 175-190. 

Kahn R. (1986) The evolution of COz on Mars. In MECA Workshop on the Evolution of the Martian Atmosphere (M. Carr, P. James, C. 

Leovy, R. Pepin, and J. Pollack, eds.), p. 23. LPI Tech. Rpt. 86-07, 

Lunarand Planetary Institute, Houston. 

Kahn R. (1986) The varying properties of Martian aerosols. In MECA 

Workshop on Dust on Mars I1 (S. Lee, ed.), p. 42. LPI Tech. Rpt. 

86-09,Lunar and !lanetary Institute, Houston. 

Kahn R. , Guiness E. , and Arvidson R.+ (1986) Loss of fine-scale surface 

texture in Viking Orbiter images and implications for the inferred 

distribution of debris mantles. Icancs, 66, 22-38. 

Kahn R. , Guinness E. , and Arvidson R.' (1986) Loss of fine-scale surface 

texture in Viking Orbiter images due to atmospheric obscuration, and 

a reassessment of latitudinal debris mantling on Mars. In MECA 

Workshop on the Evolution of the Martian Atmosphere (M. Carr, P. 

James, C. Leovy, R. Pepin, and J. Pollack, eds.), pp. 24-25. LPI Tech. 

Rpt. 86-07, Lunar and Planetary Institute, Houston. 

Kargel J.S. (1987) Morphologic variations of martian rampart crater ejecta 

and their dependencies and implications. In MECA Special Session at 

LPSC XWI: Martian Geomorphology and its Relation to Subsurface 

Volatile (S. M. Clifford, L. A. Rossbacher, and J. R. Zimbelman, eds.), 

pp. 28-29. LPI Tech. Rpt. 87-02, Lunar and Planetary Institute, 

Houston. 

Kasting J. F. (1987) Climatic effects of enhanced COz levels in Mars 

early atmosphere. In MECA Symposium on Man: Evolution of its Climate 

and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, 

C. Leovy, and T. Maxwell, eds.), pp. 64-66. LPI Tech. Rpt. 87-01, 

Lunar and Planetary Institute, Houston. 
i Technical Report 88-09 27 

Kasting 1. E.* and Toon 0.. (1987) Climate evolution on the terrestrial 

planets. In Proceedings of the Conference on Origin and Evolution of 

Planetary and Satellite Atmospheres, March 10-14. Univ. of Ariz. Press, 

Arizona. , Kasting J. F. , Toon O., and Pollack J. B.* (1988) How climate evolved 

on the terrestrial planets. Sci. ,$mer., 258, 90-97. 

Kieffer H. H.t and Paige D. A. (1987) Influence of polar-cap albedo 

on past and current martian climate. In MECA Symposium on Mars: 

Evolution of its Climate and Atmosphere (V. Baker, M. Carr. F. Fanale, 

R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), pp. 69-70. 

LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, Houston. 

Kochel R. C. and Howard A. D. (1985) Groundwater sapping and ancient 

valley networks on Mars. In Workshop on Water on Man (S. Clifford, 

ed.), pp. 48-50. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. 

Kochel R. C. and Piper 1.0. (1987) Morphology of large valleys on Hawaii: 

Implications for groundwater sapping and comparisons to Martian 

valleys. In MECA Special Session at LPSC XWI: Martian Geommphology 

and its Relation to Subsurface Volatiles (S. M. Clifford, L. A. Rossbacher, 

and J. R. Zimbelman, eds.), pp. 30-31. LPI Tech. Rpt. 87-02, Lunar 

and Planetary Institute, Houston. 

Krinsley D. and Greeley R.t (1985) Individual particles and martian aeolian 

action-a review. Sedimentary Ge?logy, 47, 167-189. 

Laul 1. C., Smith M. R., Wanke H. , Jagoutz E., Dreibus G., Palme H., 

Spettel B., Burghele A., Lipschutz M. E., and Verkouteren R. M. (1985) 

Chemical systematics of Shergotty. In Lunar and Planetary Science XVJ, 

pp. 17-18. Lunar and Planetary Institute, Houston. 

Laul J. C., Smith M. R., Wanke H.*, Jagoutz E., Dreibus G., Palme H., 

Spettel B., Burghele A., Lipschutz M. E., and Verkouteren R. M. (1986) 

Chemical systematics of the Shergotty meteorite and the composition 

of its paient body (Mars). Geochim. Cosmochim. Acta, 50, 909-926. 

Lee S. W. (1984) Albedo features in the Solis PlanumlSinai Planum 

region of Mars: Seasonal and secular changes. But Am. AS~TOTL Soc., 

16, 672, 

Lee S. W. (1984) Mars: Eolian dust transport at high altitudes and low 

pressures. Geol. Soc. Amer. Abst. with Prog., 16, 573. 

Lee S. W.* (1984) Mars: Wind streak production as related to obstacle 

type and size. Icaw, 58, 339-357. 

Lee S. W.* (1985) Influence of atmospheric dust loading and water vapor 

content on settling velocities of martian dustlice grains: Preliminary 

results. In Workshop on Water on MMS (S. Lee, ed.), pp. 51-52. LPI 

Tech. !pt. 85-02, Lunar and Planetary Institute, Houston. 

Lee S. W. (1985) Seasonal and secular variation of the Solis Lacus albedo 

feature: Relation to the martian dust-transport cycle. In LUMT and 

Planetary Science XVJ, pp. 483-484. Lunar and Planetary Institute, 

Houstp. 

Lee S. W. (1985) Aeolian dust transport at heh altitudes and low pressures 

on Mars. In Workshop on Duct on Mms (S. Lee, ed.), pp. 8-9. LPI 

Tech. Rgt. 85-02, Lunar and Planetary Institute, Houston. 

Lee S. W. , ed. (1985) Workshop on Dust on Mars LPI Tech. Rpt. 85- 

02, Lunar and Planetary Institute, Houston. 23 pp. 

Lee S. W.* (1985) IRTM Observations of Syrtis Major: An area of active 

aeolian transport. Bull. Amer. AS~TOTL Soc., 17, 736-737. 

Lee S. W.' (1986) IRTM thermal and albedo observations of Syrtis Major. 

In Lunar and Planetary Science XVII, pp. 470-471. Lunar and Planetary 

Institute, Houston. 

Lee S. W.* (1986) Viking observations of regional sources and sinks of 

dust on Mars. In MECA Workshop on Dust on Mms II (S. Lee, ed.), 

pp. 44-45. LPI Tech. Rpt. 86-09, Lunar and Planetary Institute, 

Houston. 

Lee S. W.*, ed. (1986) MECA Workshop on Duct on Mms II. LPI Tech. 

Rpt. 86;09, Lunar and Planetary Institute, Houston. 79 pp. 

Lee S. W. (1986) Regional sources and sinks of dust on Mars: Viking 

observations of Cerberus, Solis Planum, and Syrtis Major. In MECA 

Symposium on Mars: Evolution of its Climate and Atmosphere (V. Baker, 

M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, 

eds.), pp. 57-58. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houstoni 

Lee S. W. (1986) Dust transport at high altitudes and low pressures 

on Mars: Aeolian activity on the Tharsis Montes. NASA TM-88383, 

Lee S. W.* (1987) Regional sources and sinks of dust on Mars: Viking 

observations of Cerberus, Solis Planum, and Syrtis Major. In NASA 

(1985) The general circulation of Mars: Models and 

observations, Advances. In Issues in Atmospheric and Oceanic Modeling, 

Part A Climate Dynamics (S.K. Manabe, ed.), Advances in Geophys., 

28A, pp. 327-346. Academic, New York. 

Leovy C. B.* (1986) Martian dust storms and climate change. In MECA 

Workshop on the Evolution of the Martian Atmosphere (M. Carr, P. 

James, C. Leovy, R. Pepin, and J. Pollack, eds.), pp. 26-27. LPI Tech. 

Rpt. 86-07, Lunar and Planetary Institute, Houston. 

pp. 251-253. 

~~-898 r 0, pp. 259-260. 

Leovy C. B. 

Leovy C. B. c1987) Planetarypospheres. Rev. Geophys., 25, 297-303, 

Leovy C. B. , Tillman J. E. , Guest W. R., and Barnes 1. R.* (1985) 

Interannual variability of martian weather. In Recent Developments in 

Planetary Meteorology (G. E. Hunt, ed.), pp. 69-84. Cambridge Univ. 

Press, Caybridge. 

Leovy C. B. , Hitchman M., and McCleese D.* (1988) Flux of water 

vapors in the terrestrial stratosphere and in the martian atmosphere. 

In Workshop on Atmospheric H2O Observatias of Earth and Mms. 

LPI Tech. Rpt., in press, Luna: and Planetary Institute, Houston. 

Leshin L. A. and Zimbelman J. R. (1986) Thermal inertias for the Elysium 

and Aeolis quadrangles of Mars. In LU~T and Planetary Science XVII, 

pp. 474-475. LUMI and Plan5tary Institute, Houston. 

Lewis J. S.+ and Watkins G. H. (1986) Early volatile element inventories 

on Mars. In MECA Workshop on the Evolution of the Martian Atmosphere 

(M. Carr, P. James, C. Leovy, R. Pepin, and J. Pollack, eds.), p. 28. 

LPI Tech. Rpt. 86-07, Lunar and Planetary Institute, Houston. 

Lindner B. L. and Jakosky B. M.+ (1985) Martian atmospheric 

photochemistry and composition during periods of low obliquity. ]. 

Geophys. Res., 90, 3435-3440. 

Lucchitta B. K. (1984) Ice and debris in the fretted terrain, Mars. PTK. 

Lunar Planet.oSci. Coni 14th, in]. Geophys. Res., 89, W-B418. 

Lucchitta B. K. (1984) A late climatic change on Mars. In Lunar and 

Planetary Science XV, pp. 493-494. Lunar and Planetary Institute, 

Houston. 

Lucchitta B. K.' (1984) Small-scale polygons on Mars. NASA TM-86246, 

pp. 205-207. 

LucchittaB. K.* (1984)Permafrost on Marsand Earth. In27thIntemotional 

Geological co?gress, 8, August 4-14. Moscow. 

Lucchitta B. K. (1984) Valles Marineris basin beds: A complex story. 

NASA TM-8!563, pp. 506-508. 

Lucchitta B. K. (1985) Groundwater in the equatorial region of Mars: 

Evidence from landslides. In Workthop on Water on Mnrs (S. Clifford, 

ed.), pp. 53-55. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. 

Lucchitta B. K.* (1985) Geomorphologic evidence for ground ice on Mars. 

In Ices in the Solar System 0. Klinger, D. Benest, A. Dollfus, and R. 

Smoluchowski, eds.), pp. 583-604. D. Reidel, Dordrecht. 

Lucchitta B. K.' (1985) Ice-laden debris in outflow channels and northern 

lowland plains, Mars. Geol. Soc. Ame~. Abst. with Prog., 17, 647. 

Lucchitta B. K. (1987) Water and ice on Mars: Evidence from Valles 

Marineris. In MECA Symposium on MIITS: Evolution of its Climate and 

Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, 

C. Leovy, and T. Maxwell, eds.), pp. 73-75. LPI Tech. Rpt. 87-01, 

Lunar and Planetary Institute, Houston. 

Lucchitta B. K.* (1987) Ice-formed landscapes on Mars. Inter-Nord, Int. 

Joud of Arc$ and Nordic Studies, in press. 

Lucchitta B. K. (1987) Valles Marineris, Mars: Wet debris flows and 

ground ice. Icmus, 72,411-429. 
28 MECA Final Report 

Lucchitta B. K.*, Ferguson H. M., and Summers C. A. (1986) Northern 

sinks on Mars(?). In Lunar and Planetmy Science XVII, pp. 498-499. 

Lunar and Plpetary Institute, Houston. 

Lucchitta B. K. , Ferguson H. M., and Summers C. A. (1986) Sedimentary 

deposits in the northern lowland plains, Mars. PTK. Lunar Planet. Sci. 

Cmf 174 i:J. Geophys. Res., 91, E166-El74. 

Lucchitta B. K. , Ferguson H. M., and Summers C. A. (1986) An ancient 

Ocean on Mars? NASA TM-88383, pp. 450-453. 

Lumme K. and James P. B.’ (1984) Some photometric properties of the 

martian south polar cap during the 1971 apparition. Icancs, 58,363-377. 

Marshall H. G.*, Walker J. C.G., and Kuhn W. R.t (1985) Cloud properties 

in past martian climates. In Workshop on Water on Man (S. Clifford, 

ed.), p. 56. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston., 

Martin L. J. (1984) Clearing the martian air: The troubled history of 

dust story Im, 57, 317-321. 

Martin L. J. and James P. B.’ (1985) The possible role of water in the 

recession of Mars polar caps. In Workshop on Water on Mms (S. Clifford, 

ed.), p. 56. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston., 

and James P. B.t (1986) Major dust storm activity and 

variations in the recessions of Mars south polar cap. In MECA Workshop 

on the Evolution of the Martian Atmosphere (M. Carr, P. James, C. 

Leovy, R. Pepin, and J. Pollack, eds.), pp. 29-30. LPI Tech. Rpt. 86- 

07, Lunar and Planetary Institute, Houston. 

Martin L. 1. and James P. B.+ (1986) Dust clouds of a different nature. 

In MECA Workshop on Dust on Mass II (S. Lee, ed.), pp. 46-47. LPI 

Tech. Rpt; 86-09, Lunar and Planetary Institute, Houston. 

Martin L. J. and James P! (1987) The great dust storm of 1986(?). 

In MECA Symposium on Mass: Evolution of its Climate and Atmosphere 

(V. Fhker, M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and 

T. Maxwell, eds.), pp. 76-77. LPI Tech. Rpt. 87-01, Lunar and Planetary 

Institute, Houston. 

Martin T. 2.’ (1986) Infrared opacity of dust from Mars atmosphere. 

Martin L. J. 

In MECA Workshop on ht on Mms II (S. Lee, ed.), pp. 48-49. LPI 

Tech. Rpt,86-09, Lunar and Planetary Institute, Houston. 

Martin T. 2. (1986) Thermal infrared opacity of the Mars atmosphere. 

Martin T. Z.* and Kieffer H. H.’ (1985) Improved access to martian 

infrared radiometry/spectroscopy datasets. In LUMT and Planetary 

Science XVI, p. 523. Lunar and Planetary Institute, Houston. 

Masursky H.’ (1986) Ages of rocks and channels in prospective martian 

landing sites of Mangala Vallies region. In Lunar and Planetary Science 

XVII, pp. 529-521. Lunar and Planetary Institute, Houston. 

McCleese D. J. and Schofield J. T. (1988) Measurement of the vertical 

profile of water vapor abundance in the martian atmosphere from 

Mars Observer. In Workshop on Atmospheric H20 Observations of hth 

and Man. LPI Tech. Rpt., in press, Lunar and Planetary Institute, 

Houston. 

McCleese D. J.’ and West R. A.’ (1986) Observations of dust from Mars 

Observer. In MECA Workshop on Dust on Mms II (S. Lee, ed.), pp. 

50-52. LPI Tech. Rpt. $49, Lunar and Planetary Institute, Hpuston. 

McKay C. P., Clow G. D. , Wharton R. A., and Squyres S. W. (1985) 

‘Thickness of ice on perennially frozen lakes. Nature, 313, 561-562. 

McSween H. Y., Jr. (1985) SNC meteorites: Clues to martian petrologic 

evolution? Reu. Geophys., 23, 391-416. 

Michelangeli D. V., Zurek R. W.’, and Elson L. S. (1987) Barotropic 

instability of midlatitude zonal jets on Mars; Earth and Venus. J. 

Miller J. S., Marshall J. R., and Greeky R.’ (1987) Wind ripples in low 

Moore H. J.’ (1985) Sublimation rates required for steady-state glaciers, 

Mars. In Workshop on Water on Mms (S. Clifford, ed.), pp. 59-61. 

LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, Houston. 

I-, 66, 1-21. 

I 

Atl~~~pheric Sci., 44,2031-2041. 

, density atmospheres. NASA Th4-89810, pp. 268-270. 

Moore H. 1.’ (1985) Local dust storm of SOL 1742, Mars. In Lums and 

Planetary Science XVI, 571-572. Lunar and Planetary Institute, Houston. 

Moore H. J.+ (1986) The martian dust storm of SOL 1742. PTOC. LUMT 

Planet. Sci. Cmf. 16th, inJ. Geophys. Res., 90, D163-Dl74. 

Moore H. (1986) Martian miniature slope failures, Mutch Memorial 

Station. In MECA Workshop on Dust on Mms II (S. Lee, ed.), pp. 

53-55. LPI Tech. Rpt. 86-09, Lunar and Planetary Institute, Houston. 

Moore H. J! and Davis P. A. (1987) Ablation of martian glacier. In 

MECA Symposium on Mars: Evolution of its Climate and Atmosphe 

(V. Beker, M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and 

T. Maxwell, eds.), pp. 78-80. LPI Tech. Rpt. 87-01, Lunar and Planetary 

Institute, Houston. 

Morris R. V.’ (1985) Determination of optical penetration depths from 

reflectance and transmittance measurements on albite powders. In 

Lunar and Phnetary Science XVI, pp. 581-582. Lunar and Planetary 

Institute, Houston. 

Morris R. V.’ and Lauer H. V., Jr. (1984) Spectral properties of annealed 

(Fe.Al1.~)203 gels with applications to Mars. In Lunar and Planetary 

Science XV, pp. 571-572. Lunar and Planetary Institute, Houston. 

Morris R. V.’ and Mendell W. W. (1984) Scattering coefficients and 

optical penetration depths for powders of San Carlos olivine. In Lunar 

and Pkmetary Science XV, pp. 573-574. Lunar and Planetary Institute, 

Houston. 

Morris R. V.’, Lauer H. V., Jr., Lawson C. A., Gibson E. K., Jr.’, Nace 

G. A., and Stewart C. (1985) Spectral and other physicochemical 

properties of submicron powders of hematite (a-Fezq), maghemite 

(y-FezOj), magnetite (FejO,), goethite (a-FeOOH), and lepidocrocite 

(y-FeOOH). J. Geophys. Res., 90, 3126-3144. 

Morris R. V.t, Lauer H. V., Jr., Agresti D. G., and Newcomb ].A. (1986) 

Spectral properties of “dust” produced in the dry valleys of Antarctica: 

A martian analogue? In MECA Workshop on Duct on Man I1 (S. Lee, 

4.1, pp. 56-57. LPI Tech. Rpt. 86-09, Lunar and Planetary Institute, 

Houston. 

Morris R. V?, Lauer H. V., Jr., Murali A. V., Agresti D. G., and Newcomb 

J. A. (I 987) Ultramicrocrystalline hematite: Properties and occurrence 

on the martian surface. In Lunar and Planetary Science XVIII, pp. 

668-669. Lunar and Planetary Institute, Houston. 

Morris R. V!, Agresti D. G., Lauer H. V., Jr., Newcomb J. A., and Murali 

A. V. (1987) Ultramicrocrystalline hematite: Properties and occurrence 

on Mars and the Earth. Submitted toJ. Geophys. Res. 

Mouginis-Mark P. J. (1985) Volcanolground ice interactions in Elysium 

Planitia, Mars. IT, 64,265-285. 

Mouginis-Mark P. J. (1985) Identification of lava flow-permafrost 

interactions on Mars. In L~MT and Planetmy Science XVI, pp. 591-592. 

Lunar and Planettry Institute, Houston. 

Mouginis-Mark P. J. (1987) Ice or liquid water in the Martian regolith? 

Morphologic indicators from rampart craters. In MECA Symposium 

on Mms: Evolution of its Climate and Atmosphere (V. Ekker, M. Cam, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell,, eds.), 

pp. 81-83. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Mouginis-Mark P. 1. (1987) Water or ice in the Martian regolith?: Clues 

from rampart cratzrs seen at very high resolution. Iumcs, 71, 268-286. 

Mouginis-Mark P. J. (1987) Martian rampart craters: Morphologic clues 

for the physical state of the target at time of imuact. NASA TM898 IO, pp. 420-42.2. - 

Mouginis-Mark P. J. and Zimbelman J. R.’ (1987) Channels on Alba 

Patera, Mars: Evidence for polygenic eruptions. In Lunar and Planetary 

Science XVII, pp. 6.72-673. Lunar and Planetary Institute, Houston. 

Mouginis-Mark P. J. , Wilson L., Head J. W., Brown S. H., Hall J. L., 

and Sullivan K. D. (1984) Elysium Planitia, Mars: Regional geology, 

volcanology, and evidence for volcano-ground ice interactions. Earth, 

Moon, and Planets, 30, 149-113. 

Muenow D. W. and GoodingJ. L. (1985) “Martian” volatiles in shergottite 

EETA 79001: Possible significance of secondary minerals. In Lunar and 

i 
~ 

Technical Report 88-09 29 

I 

Planetary Science XVJ, pp. 593-594. Lunar and Planetary Institute, 

Houston. 

Muhleman D. O., Clancy R. T., Schloerb F. P., Riley L., and Wilson 

W. G. (1985) Mapping of the water vapor distribution on Mars; a 

microwave spectrometer and radiometer for MG/CO. In Workshop 

on Water on Mars (S. Clifford, ed.), pp. 62-63. LPI Tech. Rpt. 85, 

03, Lunar and Planptary Institute, Hpuston. 

Murphy J., Leovy C. , and Tillman J. (1987) Seasonal wind variations 

in the martian subtropics. In MECA Symposium on Mas: Evolution 

of its Climate and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, 

R. Haberle, C. Leovy, and T. Maxwell, eds.), p. 84. LPI Tech. Rpt. 

87-01, Lqar and Planetary Iytitute, Houston. 

Murray B. C. , Herkenhoff K. E. ,and Landry B. M. (1985) Frost variations 

within the south polar residual cap of Mars. Bull. Am. AStTon. Soc., 

17, 734. 

Narumi Y. (1987) Optical thickness of the Olympus cloud. In MECA 

Symposium on Mars: Evolution of its Climate and Atmosphere (V. Baker, 

M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, 

eds.), pp. 85-87. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Nedell S. S. and Squyres S. W.* (1985) Geology of the layered deposits 

in the Valles Marineris. In Workshop on Water on Mars (S. Clifford, 

ed.), pp. 64-65. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. 

Nedell S. S. and Squyres S. W.* (1987) Formation of the layered deposits 

in the Valles Marineris, Mars. In MECA Symposium on Mars: Evolution 

of its Climate and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, 

R. Haberle, C. Leovy, and T. Maxwell, eds.), pp. 88-90. LPI Tech. 

Rpt. 87-01, Lunar and Pla:etary Institute, Houstop. 

Nedell S. S., Squyres S. W. , and Anderson D. W. (1987) Origin and 

evolution of the layered deposits in the Valles Marineris, Mars. Icancr, 

70,409-441. 

Newsom H. E. and Graup G. (1987) The role of fluidization in the 

emplacement and alteration of the suevite impact melt deposit at the 

Ries Crater, West Germany. In MECA Special Session at LPSC XVJJ: 

Martian Geomurphobgy and its Relation to Subsurface Volatiles (S. M. 

Clifford, L. A. Rossbacher, and J. R. Zimbeltnan, eds.), pp. 34-35. 

LPI Tech. Rpt. 87-02, Lunar and Planetary Institute, Houston. 

Oliver0 1. 1. (1988) Measurement of H2O in the terrestrial mesosphere 

and implications for extra-terrestrial sources. In Workshop on 

Atmospheric H2O Observations of Earth and Mars. LPI Tech. Rpt., 

in prey, Lunar and Planetary Institute, Houston. 

Owen T. (1986) Update of the Anders-Owen model for martian volatiles. 

In MECA Workshop on the Evolution of the Martian Atmosphere (M. 

Carr, P. James, C. Leovy, R. Pepin, and J. Pollack, ed.), pp. 31-32. 

LPI Tegh. Rpt. 86-07, Lunar and Planetary Institute, Houston. 

(1987) Could icy impacts reconcile Venus with Earth and 

Mars? In MECA Symposium on MUTS: Evolution of its Cfimare nnd 

Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, 

C. Leovy, and T. Maxwell, eds.), p. 91. LPI Tech. Rpt. 87-01, Lunar 

and Planetary Institute, Houston. 

Page T. (1987) Seismic exploration for water on Mars. In MECASymposium 

on Mms: Evolution of its Climate and Atmosphere (V. Baker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), 

p. 92. LP! Tech. Rpt. 87.01, Lunar and Planetary Institute, Houston. 

Paige D. A. (1986) Dust in the spring season polar atmospheres: A northsouth comparison. In MECA Workshop on Dust on Man 11 (S. Lee, 

ed.), pp. 58-60. LPI Tech. Rpt. 86-09, Lunar and Planetary Institute, 

Houston; 

Paige D. A. and lngersoll A. P.' (1985) Annual heat balance of martian 

polar caps: Viking observations. Science, 228, 1160-1 168. 

Paige D. A. and Kieffer H. H.' (1986) Non-linear frost albedo feedback 

on Mars: Observations and models. In MECA Workshop on the Evolution 

of the Martian Atmosphere (M. Carr, P. James, C. Leovy, R. Pepin, 

Owen T. 

and J. Pollack, eds.), pp. 33-34. LPI Tech. Rpt. 86-07, Lunar and 

Planetary Institute, Houston. 

Paige D. A. and Kieffer H. H.+ (1987) The thermal properties of martian 

surface materials of high latitudes: Possible evidence for permafrost. 

In MECA Symposium on Mars: Evolution of its Climate and Atmosphere 

(V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and 

T. Maxwell, eds), pp. 93-95. LPI Tech. Rpt. 87-01, Lunar and Planetary 

Institute, !-louston. 

Paige D. A. , Herkenhoff K. E.', and Murray B. C.' (1987) Mariner 

9 observations of the south residual polar cap of Mars: Evidence for 

residual COJ frost, in prepaytion. 

Pallaconi F. D. and Albee A. L. (1985) The Mars Gewience/Climatology 

Observer (MGCO) Mission. In Workshop on Man (S. Clifford, ed.), 

p. 66. LPiTech. Rpt. 85-03, Lunar and Planetary Institute, Houston. 

Parker T. J. and Schneeberger D. M. (1986) Longitudinal depth profile 

for Nirgal pllis. Nq TM-88383, pp. 462-467. 

Parker T. J. , Pieri D. , and Saunders R. (1986) Morphology and 

distribution of sinuous ridges in central and southern Argyre. NASA 

Parker T. J. , Schneeberger D. M., Pieri D. C.', and Saunders R. S.' 

(1987) Geomorphic evidence for ancient seas on Mars. In MECA 

Symposium on Mars: Evolution of its Climate and Atmosphere (V. Baker, 

M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, 

eds.), pp. 96-98. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston., 

Parker T. J. , Schneeberger D. M., Pieri D. C.', and Saunders R. S.' 

(1987) Curvilinear ridges and related features in southwest Cydonia 

Mensae, Y,,,. NASA TM-898 IO, pp. 502-504, 

Parker T. J. , Schneeberger D. M., Pieri D. C. , and Saunders R. S.' 

(1987) Geomorphic evidence for ancient seas in west Deuteronilus 

Mensae, Mars-I: Regional geomorphology. NASA TM-89810, pp. 

Parker T. J. , Schneeberger D. M., Pieri D. C.', and Saunders R. S.' 

(1987) Geomorphic evidence for ancient seas in west Deuteronilus 

Mensae, Mars-11: From very high resolution Viking Orbiter images. 

TM-88382, pp. 468-470. 

319-321. 

NASA TM-89810, pp. 322-324. 

Pepin R. 0.: (1985) Evidence of martian origins. Nature, 317,473-475. 

Pepin R. 0. (1987) Volatile inventory of Mars. In MECA Special Session 

at LPSC XVJI: Martian Geomurphobgy and its Relation to Subsurface 

Volatiles (S. M. Clifford, L. A. Rossbacher, and J. R. Zimbelman, eds.), 

pp. 36-37. LPI Tech. Rpt. 87-02, Lunar and Planetary Institute, 

Houston. 

Pepin R. 0. (1987) Volatile inventory of Mars-11: Primordial sources 

and fractionating processes. In MECA Symposium on Mars: Evolution 

of its Climate and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, 

R. Haberle, C. Leovy, T. Maxwell, eds.), pp. 99-101. LPI Tech. Rpt. 

87-01, Luvar and Planetary Institute, Houston. 

Pepin R. 0. (1987) Volatile inventories of the terrestrial planets. Reu. 

Geophys., <5, 293-296. 

Pepin R. 0. and Becker R. H. (1984) Galactic-cosmic-ray exposure 

histories of the Antarctic shergottite EE'TA 79001. In Lunar and 

Planetq Science XV, pp. 637-638. Lunar and Planetary Institute, 

Houston. 

Peterfreund A. R. (1985) Local dust storms and global opacity on Mars 

as detected by the Viking IRTM. In Workshop on Dust on Mars (S. 

Lee, ed.), pp. 10-14. LPI Tech. Rpt. 85-02, Lunar and Planetary 

Institute, Houston. 

Philip J. R. (1988) Atmospheric heat engines, and H20 in the martian 

regolith. In Workshop on Atmospheric H20 Observations of Earth and 

Man. LPI Tech. Rpt., in press, Lunar and Planetary Institute, Houston. 

Phillips R. J.' (1987) Martian tectonics: A review. In MECA Symposium 

on Mms: Ewlution of its Climate and Atmosphere (V. Beker, M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. laovy, and T. Maxwell, &.I, 

pp. 102-103. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 
~ 

30 MECA Final Report 

Plaut J. J., Kahn R.*, Guinness E. A:, Arvidson R. E! (1988)Accumulation 

of sedimentary debris in the south polar region of Mars and implications 

for climate. history. Icarus, in press. 

Pollack J. B. (1986) Longevity of a dense carbon dioxide atmosphere 

on Mars. In MECA Workshop on the Evolution ofthe Martian Atmosphere 

(M. Carr, P. James, C. Leovy, R. Pepin, and J. Pollack, eds.), p. 37. 

LPI Tech. Rpt. 86-07, Lunar and Planetary Institute, Houston. 

Pollack J. B.., Haberle R. M.t, White J., and Bilski K. (1985) New GCM 

simulations of transport into the polar regions. In Workshop on Water 

on Mars (S. Clifford, ed.), p. 67. LPI Tech. Rpt. 85-03, Lunar and 

Planetary institute, Houston. 

Pollack J. B, , Haberle R. M.', Barnes I.*, Schlesinger M., Zurek R.+, 

Leovy C. , White J., Schaeffer J., and Bilski K. (1986) Influence of 

dust on the general circulation of the martian atmosphere. In MECA 

Workshop on Duct on Mars 11 (S. Lee, ed.), pp. 61-62. LPI Tech. Rpt. 

86-09, Lunar and Plapetary Institute, Houston. 

Pollack J. B.., Kasting J. , and Richardson S. (1987) Partitioning of carbon 

dioxide between the atmosphere and lithosphere on early Mars. In 

MECA Symposium on Mars: Evolution of its Climate and Atmosphere 

(V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and 

T. Maxwell, eds.), pp. 104-105. LPI Tech. Rpt. 87-01, Lunar and 

Planetary fnstitute, HousLon. 

Pollack J. B. , Kasting 1. F. , Richardson S. M., and Poliakoff K. (1987) 

The case for a wet, warm climate on early Mars. NASA TM-89810, 

Pollack 1. B.., Kasting 1. F.*, Richardson S. M., and Poliakoff K. (1987) 

The case for a warm, dense COz atmosphere on early Mars. Icarus, 

71,203-224, 

Posey-Dowty J. , Tanenbaum L.B., Moskowitz B. M.*, Crerar D. A., and 

Hargraves R.t (1985) Controls on precipitation of various iron oxides 

and hydroxides: Relevance to Mars. In Workshop on Water on Mars 

(S. Clifford, ed.), pp. 68-70. LPI Tech. Rpt. 85-03, Lunar and Planetary 

Institute, Hotston. 

Posey-Dowty J. , Moskowitz B.*, Crerar D., Hargraves R., Tanenbaum 

L., and Dowty E. (1986) Iron oxide and-hydroxide precipitation from 

ferrous solution and its relevance to martian surface mineralogy. Icarus, 

Postawko S. E. and Kuhn W. R.* (1984) Sulfur dioxide and martian 

temperature.*EOS Trans. AGU, 55, 980. 

Postawko S. E. and Kuhn W. R. (1985) Sulfur dixoide and martian 

surface temperature. In Lunar and Planetary Science XVI, pp. 673-674. 

Lunar and Plpetary Institute, Hyston. 

Postawko S. E. and Kuhn W. R. (1986) Effect of greenhouse gases 

(COz, HzO, SOz) on martian paleoclimate. Proc. Lunar Planet. Sci. 

Gmf. 16th, iyJ. Geophys. Res., 91, D4!1-D438. 

Postawko S. E. and Mouginis-Mark P. (1987) Possible origin of some 

channels on Alba Patera, Mars. NASA TM-89810, pp. 303-304. 

Rao A. S. P. (1987) Implications of isotopic signatures of noble gases 

for the origin and evolution of terrestrial atmospheres. In MECA 

Symposium on Mars: Evolution of its Climate and Atmosphere (V. Baker, 

M. (srr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, 

eds.), pp. 106-108. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Rhodes D. D. and Rossbacher L. A.* (1985) The surface of Mars. In 

Himmel ochJord: Ymer (Yearbook, Swedish Geographical Society), 105, 

Rossbacher L. A.* (1984) Curvilinear ground on Mars: The search for 

terrestrial analogs. In Abstracts of the 27th International Geological 

Rossbacher L. A. (1985) The problem of scale in planetary megageomorphology: Global megageomorphology. NASA conference Publication 

p. 160. 

66, 105-116.. 

7-29. 

Congres~, 7, 302-304. 

~~ 

2312, pp.76-18. 

ground. NASA TM-87563, pp. 329-331. 

Rossbacher L. A. (1985) Terrestrial analog studies for Martian patterned 

Rossbacher L. A.* (1985) Ground ice models for the distribution and 

evolution of curvilinear landforms on Mars. In Models in Geomorphology 

(M. Woldenberg, ed.), pp. 343-372. Allen and Unwin, Boston. 

(1985) Quantitative analysis of Martian polygonal 

ground. In Lunar and Planetary Science XVI, pp. 710-711. Lunar and 

Planetary Instipte, Houston. 

Rossbacher L. A. (1986) Ground patterns on Earth and Mars. In Lunar 

and Planetary Science XVII, pp. 726-728. Lunar and Planetary Institute, 

Houston. 

Rossbacher L. A.* (1987) Ground patterns on Earth and Mars. In MECA 

Special Session at LPSC XVII: Martian Geomorphology and its Relation 

to Subsurface Volatiks (S. M. Clifford, L. A. Rossbacher, and J. R. 

Zimbelman, eds.), pp. 38-39. LPI Tech. Rpt. 87-02, Lunar and Planetary 

Institute, Houston. 

Rossbacher L. A. (1987) The G-scale and planetary megageomorphology: 

How big is it really? In MECA Special Session at LPSC XVII: Martian 

Geomorphology and its Relation to Subsurface Volatiks (S. M. Clifford, 

L. A. Rossbacher, and J. R. Zimbelman, eds.), pp. 40-41. LPI Tech. 

Rpt. 87-02, Lungr and Planetary Institute, Houston. 

and Rhodes D. D. (1987) Planetary analogs for 

geomorphic features produced by catastrophic flooding. In Catastrophic 

Flooding (L. Mayer and D. Nash, eds.), pp. 289-304. Binghamton 

Symposiup in Geomorphology: IntemntioMl Series, 18. 

Roth L. E. and Sunders R. S.* (1984) Microwave reflectivity of the 

multi-layer models of the martian surface. In Lunar and Planetmy Science 

XV, pp. $93-694. Lunar an$ Planetary Institute, Houston. 

Roth L. E. , Sunders R. S. , and Schubert G. (1984) Radar and the 

detection of liquid water on Mars. In Workshop on Water on Mars 

(S. Clifford, ed.), p. 63. LPI Tech. Rpt. 85-03, Lunar and Planetary 

Institute, Houston. 

Roth L. E. , Sunders R. So, and Schubert G. (1985) Mars: Seasonally 

variable radar reflectivity. In Lunar and Planetary Science XVI, pp. 

712-713. Lunar and Planetary Institute, Houston. 

Roth L. E.*, Sunders R. S.', and Schubert G. (1986) Mars: Seasonally 

variable radar reflectivity 11. In hr and Planetary Science XVII, p. 

730. Lupar and Planetay Institute, Houston. 

Roth L. E. ,Sunders R. S. , and Thompson T. W. (1986) Radar reflectivity 

of a variable dust cover. In MECA Workshop on Duct on Mars II (S. 

Lee, ed.), pp. 63-65. LPI Tech. Rpt. 86-09, Lunar and Planetary 

Institutel Houston. 

Roth L. E. , Sunders R. S., and Thompson T. W. (1987) Modification 

styles of the martian impact craters. In Lunar and Planetary Science 

XVIII, pp. 852-853. Lu?ar and Planetary Institute, Houston. 

Roth L. E. ,Sunders R. S. ,and Thompson T. W. (1987) Mars: Seasonally 

variable radar reflectivity. NASA TM-89810, pp. 248-250. 

Roush T. L. and Singer R! (1985) Carbonates on Mars: Searching the 

Mariner 6 and 7 IRS Measurements. In Lunar and Planetarj Science 

XVI, pp. 714-715. Lunar and Planetary Institute, Houston. 

Roush T. L., Singer R.t, and McCord T. (1986) The spectral reflectance 

of mafic silicates and phyllosilicates from 0.6-4.6 pm. EOS Trans. AGU, 

67, 1271. 

Roush T. L., Singer R.+, and McCord T. (1987) Reflectance spectra of 

selected phyllosilicates from 0.6-4.6 pm. In Lunar and Planetary Science 

XVIII, pp. 858-859. Lunar and Planetary Institute, Houston. 

Roush T. L., Singer R.t, and McCord T. (1987) The spectral reflectance, 

0.6-4.3 pm, of particulate mineral-water ice mixtures. In Lunar and 

Phtary Science XVIII, pp. 856-857. Lunar and Planetary Institute, 

Houston. 

Rudy D. J., Muhleman D. O., Berge G. L., Jakosky B. M.t, and Christensen 

P. R. (1987) Mars: VLA observations of the northern hemisphere 

and the north polar region at wavelengths of 2 and 6 cm. Icarus, 

Rusch p. W., Jakosky B. M!, Clancy R. T.*, Barth C. A., Stewart A. 

I. F. , Lawrence G. M., McClintock W. E., and Paxton L. J. (1986) 

The Mars atmosphere spectrometer for Mars Observer. In MECA 

Rossbacher L. A. 

Rossbacher L. A. 

71, 159-177. 
Workshop on Duct on Mars II (S. Lee, ed.), pp. 66-68. LPI Tech. Rpt. 

86-09, Lunar apd Planetary Institute, Houston. 

Rutherford M. J. and Carroll M. R. (1985) The influence of HzO on 

volcanic degassing of aerosol forming elements S, CI, and F. In Workshop 

on Water on Mars (S. Clifford, ed.), pp. 74-75. LPI Tech. Rpt. 85- 

03, Lunar apd Planetary Institute, Houston. 

Saunders R. S. and Blewett D. T. (1987) Mars north polar dunes: Possible 

formation from low-density sediment aggregates. Solar System Res., 2 I, 

113-1 17. 

Saunders R. S.* and Parker T. J.* (1986) Distribution possible sources 

of dune-like material at the martian poles. NASA TM-88383, pp. 

Saunders R. S.', Parker T. I.', Stephens J., Laue E. G., and Fanale F. 

P.' (1985) Sediment-water deposition and erosion in the martian polar 

regions. In Workshop on Water on Mars (S. Clifford, ed.), pp. 76-78. 

LPI Tech. Ret. 85-03, Lunar and Planetary Institute, Houston. 

Saunders R. S. , Parker T. J.', Stephens J., Laue E. G., and Fanale F. 

P.' (1985) Transformation of polar ice sublimate residue into Martian 

circumpolar pd. NASA Rj-87563, pp. 3GO-302. 

Saunders R. S. , Parker T. J. , Stephens J., Laue E. G., and Fanale F. 

P? (1985) Filamentary sublimation residues from dispersions of siliceous 

particles in ice. In Lunar and Planetary Science XVI, pp. 730-731. Lunar 

and Planetary Institute, Houston. 

Saunders R. S. , Fanale F. P.', Parker T. I.*, Stephens J., and Sutton 

S., (1986) Properties of filamentary sublimation residues from dispersions 

of clay in icp. Icaw, 66, 94-104. 

Schultz P. H. (1985) Polar wandering on Mars and the distribution of 

water-ice through time. In Workshop on Water on Mars (S. Clifford, 

ed.), pp. 79-81. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. , Schultz P. H.. (1985) Polar wandering on Mars. Sci. Amer., 253, 94-102. 

Schultz P. H. (1986) The martian atmosphere before and after the Argyre 

impact. In MECA Workshop on the Evolution of the Martian Atmosphere 

(M. Carr, P. James, C. Leovy, R. Pepin, and J. Pollack, eds.), pp. 38-39. 

LPI Tech. Fpt. 86-07, Lunar and Planetary Institute, Houston. 

Schultz P. H. (1987) Crater ejecta morphology and the presence of water 

on Mars. In MECA Symposium on Mars: Evolution of its Climate and 

Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, 

C. Leovy, and T. Maxwell, eds.), pp. 109-111. LPI Tech. Rpt. 87- 

01, Lunar 2nd Planetary Institute, Houston. 

Schultz P. H. (1987) Crater ejecta morphology and the presence of water 

on Mars. YASA TM-89810, pp. 423-425. 

Schultz P. H. and Britt D. (1987) Early changes in gradation styles and 

rates on Mars. In MECA Special Session at LPSC XVJI: Martian 

Geomorphology and its Relation to Subsurface Volatiks (S. M. Clifford, 

L. A. Rossbacher, and J. R. Zimbelman, eds.), pp. 42-43. LPI Tech. 

Rpt. 87-OZbLunar and Planetary Institute, Houston. 

Schultz P. H. and Gault D. E. (1984) On the formation of contiguous 

ramparts around martian impact craters. In Lunar and Planetary Science 

XV, pp. 73;-733. Lunar and Planetary Institute, Houston. 

Schultz P. H. and Lutz A. (1988) Polar wandering of Mars. Icancc, 73, 

91-141. 

Schultz P. H.' and Rogers J. (1984) Evolution of erosional styles of martian 

impact basins. In Lunar and Planetary Science XV, pp. 734-735. Lunar 

and Planetay Institute, Houston. 

Schultz P. H. and Simon J. F. (1985) Mangala Valles outflow region: 

Characterization of the source and associated terrains. In Lunar and 

Planetary Science XVI, pp. 779-780. Lunar and Planetary Institute, 

Houston. 

Schultz P. H. , Rogers J., and Haber S. (1985) Erosion of martian impact 

basins and the changing water cycle. In Workshop on Water on Mars 

(S. Clifford, ed.), pp. 82-84. LPI Tech. Rpt. 85-03, Lunar and Planetary 

Institute, Houston. 

Schultz P. H.*, Simon J., and Clifford S. M.' (1985) Ice-embedded 

unconformable deposits as a possible source for outflow channels. In 

260-262. 

Lunar and Planetary Science XW, 744-745. Lunar and Planetary 

Institute, Houston. 

Simon J. F., Jr. and Schultz P. H.' (1985) Mangala Valles outflow region: 

Characterization of the source and associated terrains. In Lunar and 

Planetary Science XVI, pp. 779-780. Lunar and Planetary Institute, 

Houston. 

Singer R.' (1985) Spectroscopic observation of Mars. Adv. Space Res., 

59-68. 

Singer R.', Owensby P. D., and Clark R. N. (1984) First direct detection 

of clay minerals on Mars. Bull. Am. Astron. Soc., 16., pp. $79-680. 

Singer R.', Cloutis E., Rousb R. L., Mouginis-Mark P. J. , Hawke B. 

R., and Christensen P. R. (1984) Multispectral analysis of the Kasei 

Valles-Lunae Planum region of Mars. In L~MI and Planetary Science 

XV, pp. 794-795. Lunar and Planetary Institute, Houston. 

Singer R.', Owensby P. D., and Clark R. N. (1985) Observed upper limits 

for clay minerals on Mars. In Lunar and Planetary Science XVI, pp. 

787-788. Lunar and Planetary Institute, Houston. 

Singer R.', Owensby P. D., and Clark R. N. (1985) Direct detection 

of minor clay mineralogy on Mars. In MECA Workshop on Water on 

Mars. (S. Clifford, ed.), pp. 85-87. LPI Tech. Rpt. 85-03, Lunar and 

Planetary Institute. Houston. 

Singer R.', Bruckenthal E. A., Roush T. L., and Lucey P. G. (1986) 

Mars: Spatially resolved spectrophotometry from 2.2--4.2 pm. Bull. 

Amer.Astron. Soc., 18, p. 806. 

Singer R.', Roush E. A., Roush T. L., and Lucey P. G. (1987) Mars: 

Spatially resolved spectrophotometry from 2.2-4.2 pm, in preparation. 

Singer S. F.' (1987) Phobos and Deimos: A base for sampling the martian 

past. In MECA Symposium on MMS: Evolution of its Climate and 

Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, R. Haberle, 

C. Leovy, and T. Maxwell, eds.), p. 112. LPI Tech. Rpt. 87-01, Lunar 

and Planetary Institute, Houston. 

Spencer J. R. and Croft S. K. (1986) Valles Marineris as karst: Feasibility 

and implications for martian atmospheric evolution. In MECA 

Workshop on the Evolution of the Martian Atmosphere (M. Carr, P. 

James, C. Leovy, R. Pepin, and J. Pollack, eds.), pp. 40-41. LPI Tech. 

Rpt. 86-07, Lunar and Planetary Institute, Houston. 

Squyres S. W.* (1984) The history of water on Mars. Ann. Rev. Earth 

Planet. Sci., !2, 83. 

Squyres S. W. (1985) The problem of water on Mars. In Lunar &ws 

and Space A&& in the 2lst Century (W. Mendell, ed.). pp. 817-823. 

Lunar and Planetary Institute, Houston. 

SquyresS. W. and Carr M. H.' (1984) Distribution of ground ice features 

on Mars. EQS Trans. AGU, 65,979. 

Squyres S. W. and Carr M. H.' (1985) The distribution of ground ice 

features on Mars. In Workshop on Water on Mars (S. Clifford, ed.), 

pp. 88-89. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. 

Squyres S. W.* and Carr M. H.+ (1986) Geomorphic evidence for the 

distribution*of ground ice on Mars. Science, 23 1, 249-252. 

Squyres S. W. and Evans L. G. (1986) Investigation of martian volatiles 

via gamma-ry spectroscopy. Bull. Amer. Astron. Soc., 18, 807. 

Squyres S. W. and Evans L. G. (1987) Investigation of martian HzO 

and COz viapmma-ray spectroscopy. NASA TM-89810, pp. 184-186. 

Squyres S. W. and Moosman A. C. (1984) Numerical simulation of 

volcano-ground ice interaction on Mars. In Lunar and Planetmy Science 

XV, pp. 816917. Lunar and Pkpetary Institute, Houston. 

Squyres S. W. , Wilhelms D. E. , and Moosman A. C. (1985) Largescale volcano-ground ice interactions on Mars. Bull. Amer. Astron. Soc., 

17, 735. 

Squyres S. W.', Wilhelms D. E.*, and Moosman A. C. (1987) Largescale volcano-ground icp interactions on *Mars. Jmuc, 70, 385-408. 

Stephens J., Parker T. J. , Sunders R. S. , Laue E. G., and Fanale F. 

P.' (1985) Properties of filamentary sublimation residues from 

dispersions of clay in ice. NASA TM-87563, pp. 440-442. 
32 MECA Final Report 

Summers C. A. and Lucchitta B. K.' (1986) Polygonal ground in the 

northern hpisphere of Mars. NASA TM-88383, pp. 488-490. 

Tanaka K. L. (1985) Ice-lubricated gravity spreading of Olympus Mons 

aureole depits. Icarus. 62, 19;-206. 

Tanaka K. L. and Scott D. H. (1987) The youngest channel system 

on Mars. In MECA Special Session at LPSC XVII: Martian Geomorphology 

and its Relation to Subsurface Vdatikc (S. M. Clifford, L. A. Rossbacher, 

and J. R. Zimbelman, eds.), pp. 44-45. LPI Tech. Rpt. 87-02, Lunar 

and Planetary Institute, Houston. 

Thomas P. (1985) Dust streaks and related phenomena: Photometry and 

mapping. In workshop on Dust on Mars (s. Lee, ed.), pp. 15-17. LPI 

Tech. Rpt. 85-02, Lunar and Planetary Institute, Houston. 

Thompson T. W., Jurgens R. F., Roth L. ,and Robinett L. (1986) Possible 

Goldstone radar observations of Mars: 1986 and 1988 oppositions. In 

MECA Workshop on Dust on Mars II (S. Lee, ed.), pp. 69-71. LPI 

Tech. Rpt. 86-09, Lunar and Planetary Institute, Houston. 

Tillman J. E.* (1984) The Viking Mission to Mars. Proceedings of the 

National Pcme Users Goup Gmference, pp. 92-101, Orlando, FL. 

Tillman J. E. (1985) Martian meteorology and dust storms from Viking 

observations. In The Case for Mars 11, Science and Technology, 62 (C.P. 

McKay ed;), pp. 333-342. American Astronautical Society. 

Tillman J. E. (1986) Martian atmospheric dust processes over three years 

as inferred from Lander meteorology measurements. In MECA 

Workshop on Dust on Mars JI (S. Lee, ed.), p. 72. LPI Tech. Rpt. 

86-09, Lunar and Planetary Institute, Houston. 

Tillman J. E. (1987) Mars global atmospheric oscillations: Transients 

and dust storm relations. In MECA Symposium on Mars: Evolution of 

its Climate and Atmosphere (V. Baker, M. Carr, F. Fanale, R. Greeley, 

R. Haberle, C. Leovy, and T. Maxwell, eds.), p. 113. LPI Tech. Rpt. 

87-01, Lunar and Planetary Institute, Houston. 

Tyler A. L. and Hunten D. M. (1987) Vertical 03 distribution as a 

diagnostic for eddy diffusion profile. In MECA Sym@sium on Mars: 

Evolution of its Climate and Atmosphere (V. Beker, M. Carr, F. Fanale, 

R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, eds.), pp. 114-116. 

LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, Houston. 

Walker J. C. G. (1986) Early evolution of the terrestrial atmosphere. 

In MECA Workshop on the Evolution of the Martian Atmosphere (M. 

Carr, P. James, C. Leovy, R. Pepin, and J. Pollack, eds.), p. 42. LPI 

Tech. Ret. 86-07, Lunar and Planetary Institute, Houston. 

Wanke H. (1987) Chemistry and accretion of Earth and Mars. Bull. 

De Lo Societe Geologique De France, 3, 13-19, Lunar and Planetary 

Institute, Houston. 

and Dreibus G. (1984) Chemistry and accretion of Earth 

and Mars. In L~MT and Planetmy Science XV, pp. 884-885. Lunar 

and Planztary Institute, Houston. 

and Dreibus G. (1985) The degree of oxidation and the 

abundance of volatile elements on Mars. In Lunar and Planetary Science 

XU, pp. 28-29. Lunar and Planetary Institute, Houston. 

Wanke H.* and Dreibus G. (1985) Volatiles on Mars. In Workshop on 

Water on Mars (S. Clifford, ed.), pp. 90-92. LPI Tech. Rpt. 85-03, 

Lunar and Planetary Institute, Houston. 

Wanke H.' and Dreibus G. (1986) Can a high abundance of moderately 

volatile and even some highly volatile elements on Mars be reconciled 

with its low abundance of primordial rare gases! In MECA Workshop 

on the Evolution of the Mmtian Atmosphere (M. Carr, P. James, C. 

Leovy, R. Pepin, and J. Pollack, eds.), pp. 43-45. LPI Tech. Rpt. 86- 

07, Luny and Planetary Institute, Houston. 

Wanke H. and Dreibus G. (1987) Water on Mars. In MECA Symposium 

on Mms: Evolution of its Climate and Atmosphere (V. Baker. M. Carr, 

F. Fanale, R. Greeley, R. Haberle, C. hvy, and T. Maxwell, eds.), 

pp. 117-119. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Warren P. H. (1987) Mars regolith versus SNC meteorites: Evidence for 

abundant crustal carbonates? In MECA Symposium on Mms: Evdution 

of its Climate and Atmosphere (V. Baker, M. Carr, F. Fanale, R Greeley, 

Wanke H. 

Wanke H. 

R. Haberle, C. Leovy, and T. Maxwell, eds.), pp. 120-122. LPI Tech. 

Rpt. 87-01, Lunar and Planetary Institute, Houston. 

Watkins H.* and Lewis J. S.' (1985) Loss of volatiles from Mars as the 

result of energetic impacts. In Workshop on Water on Mars (S. Clifford, 

ed.), pp. 93-95. LPI Tech. Rpt. 85-03, Lunar and Planetary Institute, 

Houston. 

Watkins G. H.' and Lewis J. S.' (1986) Evolution of the atmosphere 

of Mars as the result of asteroidal and cometary impacts. In MECA 

Workshop on the Evolution of the Martian Atmosphere (M. Carr, P. 

James, C. Leovy, R. Pepin, and J. Pollack, eds.), pp. 46-47. LPI Tech. 

Rpt. 86-07, Lunar and Planetary Institute, Hpston. 

Weins R. C., Becker R. H., and Pepin R. 0. (1986) The case for a 

martian origin of the shergottites, 11. Trapped and indigenous gas 

components in EETA 79001 glass. In Earth Planet. Sci. Lett., 77,149-158. 

Wilhelms D. E.* (1986) Lava-ice interactions on Mars. In LUMT and 

Planetmy Science XVII, pp. 946-947. Lunar and Planetary Institute, 

Houston. 

Wilhelms D. E.* and Baldwin R. J. (1986) Relation between gullying and 

crater degradation in the martian-uplands. In LMT and Planetary Science 

XVII, pp. 948;949. Lunar and Planetary Institute, Houston. 

Wilhelms D. E. and Hayden C. J. (1986) Areas of gullied terrain and 

possible volcanic deposits in the martian uplands. In Lu~~and Planetary 

Science XVII, pp. 950-951. Lunar aFd Planetary Institute, Houston. 

Wilhelms D. E. and Squyres S. W. (1985) Lava-ice interaction along 

Mars upland-lowland scarp. EOS Trans. AGU, 66,946. 

Williams S. H. and Greeley R! (1986) Wind erosion on Mars: Impairment 

by poor saltation cloud development. In Lunm and Planetary Science 

XVII, pp. 952-953. Lunar and Planetary Institute, Houston. 

Williams S. H. and Greeley R.' (1987) Mass transport by aeolian saltation 

on Earth, Mars and Venus: The effects of saltation cloud development 

and choking. NASA TM-89810, pp. 274-275. 

Wu S. S. C. (1985) Mars topographic maps. In Workshop on Water on 

Mars (S. Clifford, ed.), pp. 96-97. LPI Tech. Rpt. 85-03, Lunar and 

Planetary Institute, Houston. 

(1985) Mars: Effect of water vapor 

abundance on atmospheric oxidation state. In Workshop on Water on 

Mars (S. Clifford, ed.), p. 98. LPI Tech. Rpt. 85-03, Lunar and Planetary 

Institute, Houston. 

Yatteau J. H. and McElroy M.' (1986) Mars: Atmospheric escape of major 

volatiles. In MECA Workshop on the Evolutionofthe Martian Atmosphere 

(M. Cam, P. James, C. Leovy, R. Pepin, and J. Pollack, eds.), p. 48. 

LPI Tech. Rpt. 86-07, Luntr and Planetary Institute, Houston. 

Zahnle K. J. and Kasting J. F. (1986) Mass fractionation during transonic 

escape and implications for loss of water from Mars and Venus. Icm, 

68,462-480. 

Zent A. P.' and Fanale F. P.' (1985) Possible Mars brines: Kinetics and 

chemistry. Bull. Amer. Asiron. Soc., 17, 734. 

Zent A. P.' and Fanale F. P.' (1985) Solis Lacus brines: Possible chemistry 

and kinetics. In L~MT and Planetary Science XU, pp. 930-931. Lunar 

and Planztary Institute, Houston. 

Zent A. P. and Fanale F. P.' (1986) Possible Mars brines: Equilibrium 

and kinetic considerations. Proc. hMr Planet. Sci. Gmf 16th, in J. 

Geophys.oRes., 91, D439-D445. 

Zent A. P. and Fanale F. P.' (1986) Adsorption of H20 and COz on 

Mauna Kea plagonites. In Lunar and Planetmy Science XVII, p. 962. 

Lunar and Planetary Institute, Houston. 

Zent A. P.' and Fanale F. P.' (1986) Mars: A quantitative estimate of 

total H20 exchange between the regolith and the atmospherelcap 

system over obliquity timescales. In MECA Workshop on the Evolution 

of the Martian Atmosphere (M. Carr, P. James, C. hvy, R. Pepin, 

and J. Pollack, eds.), pp. 49-50. LPI Tech. Rpt. 86-07, Lunar and 

Planetary Institute, Houston. 

Zent A. P. , Fanale F. P?, and Salvail J. R. (1984) Seasonal cycles of 

diffusion and phase partitioning of water within the Martian regolith. 

Bull. Am. Astron Soc., 16,674. 

Yatteau J. H. and McElroy M. 
~~~~~ ~ 

Technical Repurt 88-09 33 

Zent A. P.', Fanale F. P.+, and Salvail J. R. (1985) Short term water 

cycles within the Mars regolith. In Workshop on Water on Mar (S. 

Clifford, ed.), pp. 99-101. LPI Tech. Rpt. 85-03, Lunar and Planetary 

InstitutebHouston. 

Zent A. P. , Fanale F. P?, Salvail J. R., and Postawko S. E.' (1986) 

Distribution and state of Hz0 in the high latitude shallow subsurface 

of Mars. !cm, 67, 19-36. 

Zent A. P. , Fanale F. P.t, and Postawko S. E.' (1987) Adsorption on 

the martian regolith: Specific surface area and missing COz. In MECA 

Symposium on Man: Evolution of Its Climate and Atmosphere (V. Baker, 

M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, 

eds.), pp. 123-125. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houstoni 

Zent A. P. , Fanale F. P.t, and Postawko S. E.* (1987) Mars: Detection 

of regolith H20 sources from space. In Lunar and Pfunetary Science 

XVIII, pg 1120-1 121. Lunar and Planetary institute, Houston. 

Zent A. P. , Fanale F. P.t, and Postawko S. E. (1987) COz: Adsorption 

on palagtnite and the martian regolith. NASA,TM-89810, pp. 181-183. 

Zent A. P. , Fanale F. P?, and Postawko S. E. (1987) Carbon dioxide: 

Adsorption on palagonite and partitioning in the martian regolith. 

Icarus, 75 241-249. 

Zent A. P. , Fanale F. P.t, and Postawko S. E.' (1988) Atmospheric 

HzO and the search for martian brines. In Workshop on Atmospheric 

H20 Observations of Earth and Mass. LPI Tech. Rpt., in press, Lunar 

and Planetary Institute, Houston. 

Zimbelman J. R. ( 1985) Surface properties of Ascraeus Mons: Dust deposits 

on a Tharsis volcano. In Workshop on Dust on Mars (S. Lee, ed.), 

pp. 14-16. LPI Tech. Rpt. 85-02, Lunar and Planetary Institute, 

Houston. 

Zimbelman J. R.* (1986) Physical properties of aeolian features in the 

Elysium-Amazonis region of Mars. In Workshop on Dust on Mars II 

(S. Lee, ed.), pp. 73-75. LPI Tech. Rpt. 86-09, Lunar and Planetary 

Institute, Hoyon. 

Zimbelman J. R. (1986) Spatial resolution and the geobc interpretation 

of martian morphology. In LUMT and Planetmy Science XVII, pp. 63-964. 

Lunar and Plaqetary Insitute, Houston. 

Zimbelman J. R. (1986) Surface properties of the Pettit wind streak 

on Mars: Impli$ations for sediment transport. Icm, 66, 83-93. 

Zimbelman J. R. (1986) On the Red Planet: Does landscape show 

subsurface voitiles? Geotimes, 31, 18-20. 

Zimbelman J. R. (1987) Thermal properties of channels in the Aeolis 

quadrangle: Topographic traps for aeolian materials. In MECA 

Symposium on Mms: Evolution of Its Climate and Atmosphere (V. Baker, 

M. Carr, F. Fanale, R. Greeley, R. Haberle, C. Leovy, and T. Maxwell, 

eds.), pp. 126-128. LPI Tech. Rpt. 87-01, Lunar and Planetary Institute, 

Houston. 

Zimbelman J. R.' (1987) Spatial resolution and the geologic interpretation 

of martian morphology: Implications for subsurface volatiles. Icarus, 

Zimbelman J. R.' (1987) Old channels on Mars spark new ideas. Geotimes, 

Zimbelman 1. R.' (1987) Martian geomorphology and subsurface volatiles 

discussed at LPSC XVII. In MECA Special Session at LPSC XVII: Martian 

Geomorphology and its Relation to Subsurface Volatiles (S. M. Clifford, 

L. A. Rossbacher, and J. R. Zimbelman, eds.), pp. 5-7. LPI Tech. Rpt. 

87-02, Lunar 2nd Planetary Institute, Houston. 

Zimbelman J. R. (1987) New information on puzzling channels. Geotimes, 

32,. 13-14. 

Zimbelman J. R.' and Leshin L. A. (1986) Comparisons between high 

resolution thermal inertias and Mars consortium data for the Elysium 

and Aeolis quadrangles of Mars. In Lunar and Planetary Science XVII, 

pp. 965-966.@nar and Planetary Institute, Houston. 

Zimbelman J. R. and Leshin L. A. (1987) A geologic evaluation of thermal 

properties for the Elysium and Aeolis quadrangles of Mars. PTOC. Lunar 

Planet. Sci. Cmf 17th, in]. Geophys.oRa.. 92. E588-ES96. 

Zurek R. W.t and Christensen P. R. (1983) Mars north polar hazes: 

Estimating opacity and temperature with a 8-Eddington Code. Bull. 

k. htron. &., 15,847-848. 

Zurek R. W.+ (1985) Surface winds inferred from models of the planetaryscale circulation. In Workshop on Dust on Mms (S. Lee, ed.), p. 23. 

LPI Tech. Rpt. 85-01, Lunar and Planetary Institute, Houston. 

Zurek R. W.t (1986) Atmospheric tidal forcing of the zonal mean 

circulation: The martian dusty atmosphere. J. Atmos. Sci., 43, 652-670. 

Zurek R. W.t (1988) The interannual variability of atmospheric water 

vapor on Mars. In Workshop on Atmospheric H20 Observations of Earth 

and Mms. LPI Tech. Rpt., in press, Lunar and Planetary Institute, 

Houston. 

Zurek R. W.t (1988) The martian atmospheric water cycle as viewed 

from a terrestrial perspective. In Workshop on Atmospheric H20 

Observations of Earth and Mars. LPI Tech. Rpt., in press, Lunar and 

Planetary Institute, Houston. 

Zurek R. W.t and Haberle R. M? (1986) Cross-equatorial transport during 

a martian great dust storm. In MECA Workshop on Duct on Mars 

11 (S. Lee, ed.), p. 79. LPI Tech. Rpt. 86-09, Lunar and Planetary 

Institute, Houston. 

71 I 257-267. 

32, 13-14.