A three-axis short period seismometer has been operating on the surface of Mars in the Utopia

Planitia region since September 4, 1976. During the first five months of operation approx. 640

hours of high quality data, uncontaminated by Lander or wind noise, have been obtained. The

detection threshold is estimated to be magnitude 3 to about 200 km and about 6.5 for the planet

as a whole. No large events have been seen during this period indicating that Mars is less seismically

active than Earth

Anderson, D. L.

Dainty, A. M.

Duennebier, F. K.

Knight, T. C. D.

Kovach, R. L.

Latham, G. V.

Lazarewicz, A. R.

Miller, W. F.

Nakamura, Y.

Toksoz, M. N.

Caltech Authors - Main

orbiters. The data were sel ected so as to 
obtain a uniform di stribution of peri aps i s 
longitudes over the surface of Mars, and both 
S- and X- band data were used where possible to 
elimi nate charged part i c l e effects. I nc lu sion 
of-the Vik ing data arcs altered the Mart i an 
geoid features, as defined by previous short-arc 
analysis techniques of Mariner 9 data, by about 
80 meters in the Southern Hemisphere 1 and about 
140 meters i n the Northern Hemisphere. 
J. Geophys. Res . , Red, Paper 750487 
6530 Gross properties of the planet s 
LANDER LOCATIONS , MARS PHYSICAL EPHEMERIS, AND 
SOLAR SYSTEM PARAMETERS; DETERMINATION FROM 
VIKING LANDER TRACKING DATA 
A. P . Mayo (NASA Langley Research Center, Mail 
Stop 40lB, Hampton, VA 23665) 
w. T . Blackshear, R. H . Tolson, W. H. Michael, 
Jr . , G. M. Kelly, J. P. Brenkle, and T. A. Komarek 
Radio Tracking data from the Viking l anders 
have been analyzed to determine the parameters 
of the Mars physical ephemeris, the radii of Mars 
at the landing sites, and the l ander locations . 
The orientation of the Mars rotation axis, re-
ferred to the 1950. 0 Earth mean equator, equinox, 
and epoch, was determined as 317.340 ± 0.003° 
right ascension and 52.710 ± 0. 002° declination . 
The planet's r otation period was determined as 
24 hr., 37 min . 22 . 663 ± 0.002 sec. Analyses 
indicate the determination of the motions of 
the Mars rotation axis will require additional 
tracking data. The Mars radii at the sites of 
landers 1 and 2 are 3389 .38 ± 0.06 km and 
3381.91 ± 0 . 08 km, respectively . The areocentric 
location of lander 1 is 22.272 ± 0.002° N, 
47.94 ± 0.2° W. The lander 2 location is 
47.670 ± 0.002° N, 225 . 71 ± 0 . 2° W. The 
areocentric right ascensions of the landers 
are determined as 227.314 ± 0 . 002° for lander 1 
and 99.546 ± 0 . 002° for lander 2 at Jan. 1 1 
0 hr., 1977 (Julian Date 2443144 . 5) . Possible 
determinations of relativity parameters , solar 
oblateness, asteroid mass , and variations of 
the universal gravitational constant, from their 
effects on the planetary motions 1 will require 
the additional t rac king data of the Viking ex-
~~n<h~~p~~~~ioR~S .(,V~~~~g Pa~~~d7Sb4't'~{s, rotation) 
6545 Interiors of planets 
SEISMOLOGY ON MARS 
D. L. Anderson (Seismological Laborator y , Calif. 
Inst. of Tech., Pasadena, Ca. 91125), W. F. 
Miller, G. V. Latham, Y. Nakamura, M. N. Toksoz, 
A. M. Dainty, F. K . Duennebier , A. R. Lazarewicz, 
R. L. Kovach, and T. C. D. Knight. 
A three-axis short period seismometer has been 
operating on the s urface of Mars in the Utopia 
Planitia region since September 4, 1976. During 
the first five months of operation approx. 640 
hours of high quality data, uncontaminated by 
Lander or wind noise, have been obtained . The 
detection threshold is estimated to be magnitude 
3 to about 200 km and about 6 . 5 for the planet 
as a whole. No large events have been seen during 
this period indicating that Mars is less seis-
mically active than Earth. Wind is the major 
source of noise during the day although the noise 
level was at or below the sensitivity threshold 
of the seismometer for most of the night during 
the early part of the mission. Winds, and there-
fore the seismic background, started to intrude 
into the night-time hour s starting on Sol 119 
(a Sol is a Martian day). The seismic background 
correlates well with wind velocity and is pro-
portional to (wind velocity) 2, as appropriate 
for turbulent flow. The seismic envelope power 
spectral density is proportional to frequency 
to the minus 0. 66 to 0. 90 power during windy 
periods. A possible local seismic event was 
detected on Sol 80 . No wind data was obtained 
at the time so a wind disturbance cannot be 
ruled out. However • this event has some unusual 
characteristics and is similar to local events 
recorded on Earth through a Viking seismometer 
system . If interpreted as a natural sei smic 
even t it has a magnitude of 3 and a distance of 
llO km. Preliminary interpretation of later 
a rrivals in the signal suggest a crustal thick-
ness of 15 km at the Utopia Planitia Site which 
is within the range of crustal models derived 
from the gravity field. More events must be 
recorded before a firm interpretation can be 
.nade of seismicity of crustal structure. One 
firm conclusion is that the natural background 
noise on Mars is low and that the wind is the 
prime noise source. It will be possible to 
reduce this noise by a factor of 103 on futur e 
missions by removing the seismometer from the 
Lander • thus making it possible to operate an 
extremely sensitive seismometer on the surface. 
(Mars seismicity • Mars crust, Mars wi:nds, 
Viking Seismology) 
J. GeQphys. R~s. , Red, Paper 750408 
828 
6560 Meteoritics 
CORRELATED 0 AND Mg ISOTOPIC ANOMALIES IN ALLENDE 
INCLUSIONS: II. MAGNETISM 
G. J. Wasserburg (The Lunatic Asylum, Div. of 
Geological and Planetary Sciences, California 
Institute of Technology, Pasadena, California 91125) 
T. Lee and D. A. Papanastassiou 
Mg in two Allende Ca- Al rich inclusions s hows 
large isotopic, mass-dependent fractionation which 
enriched the heavier isotopes. After normaliza-
tion, Mg in these inclusions shows negative o2~g 
:~!~:t:p~:a~ ~~s~~~~!r~r~:e 2E~~s~:~:y ~f ~~~l:r 
mass frac tionation is correlated with distinct but 
smaller fractionation effects for 0 reported by 
Clayton and Mayeda for the same inclusions (see 
companion paper). The observation of distinctive 
but uniform Mg isotopic compos ition in different 
phases within single Allende inclusions indicates 
that nuclear effects i n 0 and Mg are not due to 
the entrapment of interstellar carrier grains as 
discrete entities, which are preserved as rem-
nants, but are instead due to a homogenized mix-
ture of components of extraordinary isotopic com-
position mixed with a component of ordinary solar 
sys tem material and subjected to isotopic frac-
tionation. The distinct 0 isotopic composition 
of different phases within a single inclusion is 
believed to be due to incomp l ete back-reaction of 
the higher temperature condensates with a cooler 
solar nebul a of "normal" composition. The pro-
cesses responsible for t he 0 and Mg nuclear ef-
fects and the astrophysical site of their occur-
rence remain undefined. 
Geophys . Res . Lett., Paper 710406 
6560 Heteoritics 
CORRELATED OXYGEN AND MAGNES IUM ISOTOPE ANOMALIES 
IN ALLENDE INCLUSIONS, I: OXYGEN 
Robert N. Clayton and Toshiko K. Mayeda ( Enrico 
Fermi Institute, University of Chicago, Chicago, 
Illinois 60637 ) 
Two Ca-Al-rich inclusions from the Allende 
meteorite have been found to have undergone large 
mass-fractionation of oxygen isotopes subsequent 
to incorporation of the nucleosynthetic 160-
anomaly found in other Allende inclusions. The 
magnitude of the oxygen isotope fractionations 
is in constant ratio to the magnesium isotope 
fractiona tions found in the same inclusions by 
Wasserburg, Lee and Papanastassiou . The obser-
vations support earlier theories of the addition 
of supernova ejecta into the solar nebula just 
prior to collapse and condensation . (Meteorites, 
oxygen isotopes, solar nebula, supernova ) . 
Geophys. Res. Lett . , Paper 710407 
6575 Surface of planets 
IPL PROCESSING OF THE VIKING ORBITER IMAGES OF 
MARS 
See 6590 Instruments and techniques 
6575 Surfaces of planets 
VIKING RADIO OCCULTATION MEASUREMENTS OF THE 
MARTIAN ATMOSPHERE AND TOPOGRAPHY; PRIMARY 
MISSION COVERAGE 
See 6510 Atmosphere of planet s 
6575 Surface of planets 
PROCESSING THE VIKING LANDER CAMERA DATA 
See 6590 Instruments and techniques 
6575 Surfaces of Planets 
MARS: WATER VAPOR OBSERVATIONS FROM THE VIKING 
ORBITERS 
See 6510 Atmos pheres of Planets 
-M~5 vr~J~Gc~r8io8fC~Lt~NVESTIGATION: GENERAL 
ASPECTS 
H.P. Klein (NASA Ames Research Center, Moffett 
Field, California 94035, U.S .A. 
The Viking biological investigation has tested 
four different hypotheses regarding the possible 
nature of Martian organisms . While significant 
results were obtained for each of t hese, tests 
of three of the hypotheses appear to indicate 
the absence of biology in the s amples used, 
while the fourth is consistent with a biological 
interpretation. The original assumptions for 
each experiment and the experimental procedur es 
that wer e utilized to t est these assumptions are 
reviewed . 
J. Geophys. Res. , Red, Paper 7S0439 
SS 75 Surface of p l anets 
PECULIARITIES OF THE GEOLOGICAL STRUCTURE OF 
THE MARS' SECTOR PHOTOGRAPHED BY AUTOMATIC 
STATIONS 
"MARS" (9 pp.) 
A. L. Sukhanov 
Geotect., No. 1, 1977 
6575 Surface of planets 
GEOCHEMICAL AND MINERALOGICAL INTERPRETATION OF 
.THE VIKING INORGANIC CHEMICAL RESULTS 
P. Toulmin, III (U.S. Geological Survey, 959 
National Center, Reston , VA 22092) 
A. K. Baird, B. C. Clark, K. Keil, H.J. Rose, J r. , 
R.P. Christian, P . H. Evans and W.C. Kellihe r 
The elemental analyses whose basis is described 
in the preceding two papers represent the compo-
sition of samples of Martian fines ; the only un-
determined major constituents thought to be pre-
sent are H2 0, C0 2 , Na 2 0, and possibly NOx. The 
samples are principally silicate particles , with 
some admixture of oxide and probably carbona te 
minerals; the fines appear to hax_e been indura-
ted to a variable degree by a sulfate-rich inter -
granular cement. The overall elemental composi-
tion is dissimilar to any single known mineral or 
rock type, and apparently represents a mixture of 
materials. Close chemical similarity among 
samples at each site, and between the two s i t es , 
indicates effective homogenization of the f i nes , 
presumably by planetary windstorms, and fur t her 
suggests that the samples analyzed represent the 
fine, mobilizable materials over a large par t o f 
the planet ' s surface. Low trace-element, alka-
li, and alumina contents suggest that the great 
preponderance of the materials in the mixtu r e i s 
of mafic derivation; highly differentiated, sa lic 
igneous rocks or their weathering products are 
insignificant components of the samples . Norma-
tive calculations, comparisons with refere nce 
libraries of analytical data, and mathematical 
mixture modeling have led to a qualitative min-
eralogical model in which the fines consist 
largely of iron- rich smectites (or their degra -
dation products), carbonates , iron oxides, pro-
bably in part maghemite, and sulfate minera l s 
concentrated in a surface duricrust. The origi-
nal smectites may have formed by interaction of 
mafic magma and subsurface ice, and the sulfates 
(and carbonates?) may have been concentrated in 
the surf&~ c rust by subsurface l eaching, up-
=~~:t~~=n~?~~~: a~=s ~~:~o~:~i~:f~!e!:~~r~~a~~~= r 
and competing models will accompany continui ng 
acquisition of samples and data, and r efinemen t 
of the analyses, particularly with respect t o t he 
critical light elements Mg , A, and Si. (Ma r s, 
J~eG;~~~Y~~mk~~ ~~ i~~d 'm~~~~~l7~b464ea t her in g) 
6575 Surface of Planets 
MARTIAN IMPACT CRATERS AND EMPLACEMENT OF EJECTA 
BY SURFACE FLOS . 
M.H. Carr (U.s . Ge ologiceJ. Survey, Menlo Park, 
California 94025 ) 
L. A. Crumpler, J.A. CUtts, R. Greeley, J . E. Guest 
and H. Ma sursky 
Several types of martia n impact craters have 
been recognized. The most c ommon type, t he 
rampart crater, is distinctively different from 
lunar and mercurian craters. It is typicall y 
surrounded by several layers of ejecta, each 
with a low ridge or escarpment at its outer edge . 
Outward flow of' ejecta eJ.ong the ground af'ter 
ballistic depositi on is suggested by flow lines 
around obstacles, the absence of ejecta on top 
and on the lee side of obstacles, and t h e l arge 
radial distance to which c ontinuous eject a i s 
found. The peculiar flow characteristics CJf the 
ejecta around these craters are tentatively 
attributed to entrained gases or to contained 
water, either liquid or vapor, in the ejecta as a 
\
result of impact melting of ground ice . Ej ecta 
of other craters lack flow features but have 
Ia marked radial pattern; still others have eject a 
tpatterns that resemble those around lunar and 
'mercurian craters . The internal features of 
martian craters, in genereJ., resemble thei r lunar 
and mercurian counterparts except that the 
transition from bowl-shaped to flat-floore d takes 
,place at about 5 krn diameter, a smaller size than 
for Mercury of the Moon. 
J. Geophys. Res., Red, Paper 7S0488 
6575 Surface of planets 
COMMENTS ON: " CHARACTERISTICS OF FRESH MARTIAN 
CRATERS AS A FUNCTION OF DIAMETER: COMPARISON 
WITH THE MOON AND MERCURY" BY M. J. CINTALA 
ET AL. 
C. F."" Florensky 1 A. T. Basilevsky , and V. P. 
Polosukhin (Vernadsky Institute of Geochemis try 
and Analytical Chemistry, USSR Academy of Sci-
ences, Moscow, USSR) 
Cintala et al. attempt to determine: (1) at 
what diamete"rSfresh martian c r aters begin t o 
ldevelop features such as central peaks, flat 
bottoms, terraces, etc. and (2) what determines 
the threshold diameters for various features. 
1
we argue that the r esults of Cintala ~ !l· are 
biased by the way in which they collect and 
organize data. 
Geophys. Res. Lett., P~per 7L0 122 
', 


Seismology on Mars

A three-axis short-period seismometer has been operating on the surface of Mars in the Utopia Planitia region since September 4, 1976. During the first 5 months of operation, approximately 640 hours of high quality data, uncontaminated by lander or wind noise, have been obtained. The detection threshold is estimated to be magnitude 3 to about 200 km and about 6.5 for the planet as a whole. No large events

have been seen during this period, a result indicating that Mars is less seismically active than earth. Wind is the major source of noise during the day, although the noise level was at or below the sensitivity threshold of the seismometer for most of the night during the early part of the mission. Winds and therefore the seismic background started to intrude into the nighttime hours starting on sol 119 (a sol is a

Martian day). The seismic background correlates well with wind velocity and is proportional to the square of the wind velocity, as is appropriate for turbulent flow. The seismic envelope power spectral density is proportional to frequency to the -0.66 to -0.90 power during windy periods. A possible local seismic event was detected on sol 80. No wind data were obtained at the time, so a wind disturbance

cannot be ruled out. However, this event has some unusual characteristics and is similar to local events

recorded on earth through a Viking seismometer system. If it is interpreted as a natural seismic event, it

has a magnitude of 3 and a distance of 110 km. Preliminary interpretation of later arrivals in the signal

suggest a crustal thickness of 15 km at the Utopia Planitia site which is within the range of crustal models

derived from the gravity field. More events must be recorded before a firm interpretation can be made of

seismicity or crustal structure. One firm conclusion is that the natural background noise on Mars is low

and that the wind is the prime noise source. It will be possible to reduce this noise by a factor of 10^3 on

future missions by removing the seismometer from the lander, operation of an extremely sensitive

seismometer thus being possible on the surface

Anderson, Don L.

Toksöz, M. N.

A-2 
SIGNATURES OF INTERNALLY GENERATED LANDER VIBRATIONS 
One of the disadvantages of placing the Viking seismometer on the Lander was 
that large amounts of noise were expected from mechanical vibrations of Lander 
machinery and electrical cross talk. It was important to identify these noise 
sources so that.they would not be confused•with externally generated events. 
The following figures A-5 through A-11 show examples of internal noise sources 
that have been identified. In addition, figures A-12, A-13, and A-14 show 
examples of noise generated within the seismic package itself. 
FIGURE A-1. 
FIGURE A-2. 
FIGURE A-3. 
FIGURE A-4. 
FIGURE A-5. 
APPENDIX FIGURE CAPTIONS 
Crustal thickness map of Mars from orbital gravity data. This 
map (from Phillips and Tiernan, 1977) assumes an_ average crus-
tal thickness of 100 km and a density contrast of 0.3 gm/cm3 • 
Change in calibration pulse amplitude versus time. · Decrease 
of temperature within the lander is believed to have caused an 
increase in sensitivity of the calibration and transducer coils 
by decreasing their resistance. All components still are 
matched within 5%. 
Schematic top view of the lander showing the location of the 
seismometer and the axis of rotation inferred from the coher-
ence of signals observed by the seismometer. 
Schematic side view of the lander in a plane perpendicular to 
the axis of rotation. Seismic motion implies that the lander 
tends to rotate around an axis through footpads 1 and z . 
. Soil Sampler motions. The sample arm is the noisiest device on 
the lander. The example of sampler activity shown (in Event 
mode) covers a period when the arm is extended, stopped, and 
retracted. The nearly exponential amplitude decay near the 
middle of the record occurred when the sample arm was stopped 
near full extension. As the back towards the 
'-[\.Qoi y{fi/'"''\"-f) .. '{ .C' rl. / ,r,,.e 
, I c< ~ fl ,5 -
FIGURE A-6, 
FIGURE A-7. 
lander the increase in resonant frequency is reflected in the 
increase in zero crossings. When extended, the arm resonates at 
a frequency of from 2 - 4 Hz, depending on the extension, and 
with a Q of about 250, When the arm is not being used it il; 
retracted and does not vibrate, Since the arm is only used 
for short periods of time, its vibrations do not seriously 
affect the acquisition of seismic data, The collector head 
vibrator on the sample arm operates at 8.8 and 4.4 Hz. Both 
of these signals are clearly visible on seismic records when 
the vibrator operates, 
S-Band antenna motions. The S-Band antenna is a large dish 
antenna on a 2 meter pole attached to the lander about 10 cm 
from the seismometer. When in use, the antenna is rotated to 
track the Earth. The sample shown in the figure is Event mode 
data showing the initial slew of the antenna from its parked 
position to its Earth-pointing position followed by periodic 
steps of the drive motor while following Earth (every 30 sec), 
The frequency observed by the seismometer is 7.6 Hz with a Q 
of about 25, Since the antenna is seldom in use, its effect 
on seismic data is negligible. However, it is probable that 
Martian winds are coupled to the lander through the antenna. 
S-Band antenna operation recorded in normal mode, Note that 
the amplitudes recorded are much lower than in Event mode, 
FIGURE A-8, 
FIGURE A-9. 
FIGURE A-10, 
FIGURE A-11. 
This is due to the difference in response of 
these two modes; the Event mode being more sensitive to high 
frequencies. 
Camera motion. The Viking cameras make vertical scans of the 
area to be photographed and rotate slowly to complete a scene. 
The seismometer in Event mode records this operation as a low-
level amplitude and a frequency of 7.1 Hz. Since the lander 
tape recorder is running continuously while the camera is 
operating, the noise seen by the seismometer could be caused 
by the tape recorder, 
X-ray Experiment Sample dump. When the X-ray Fluorescence 
Experiment clears its sample chamber, the vibrations of the 
trap door are visible as low level signals on the amplitude. 
traces and about 5 Hz signals on the axis crossing traces, 
Tape recorder motion, When the Lander Data Storage Memory 
(DSM) buffer is full, it is dumped to the lander tape recorder, 
This operation is observed by the seismometer as bursts of 
noise at 7.3 Hz lasting for about 15 sec, 
Cross talk with Meteorology Experiment, Each time a sample 
is obtained by the Meteorology Experiment, an electrical pulse 
is registered by the seismometer usually causing a one bit 
signal on each axis in the E'vent mode, In the sample shown, 
Meteorology is taking samples every 8 seconds. The noise pro-
duced is most easily seen on the Y component axis crossing trace. 
Because of the low level of this int.erference, it is not con-
sidered ser.ious. 
FIGURE A-12. Electrical transient noise produced in the seismometer package. 
The noise observed correlates well with the time of the beg.inning 
of each record. It is most serious in High Data Rate when a 
record lasts only 4 seconds, Because this noise is exactly 
reproducible, it could easily be removed from the data. 
FIGURE A-13. Gain change transient, 0-30 db. When the seismometer gain is 
changed, an electrical pulse from the amplifier is passed 
through the system. This pulse is an instrument characteristic 
and is easily recognized. 
FIGURE A-14. Gain change transient from 36 db to 0 db. Case must be taken 
when the instrument is in normal mode when the triggers are 
enabled because this transient will cause the system to 
trigger into the Event mode. 
FIGURE A-15. 'I' event in High Data Rate, 'I' (or Impulsive) events are 
believed to be generated by sharp motions of the lander, 
possibly related to relief of thermal stress, 
FIGURE A-16. 'I' event in the High Data Rate. This event differs from 
n,;s ,j A·· I/, (l\C 
l[V\9Je 611,( (\ru ,1. < 
r.• 
l 
I 
\I 
( ..... 
1.e . . .J ./( '1 /,r, ) 
FIGURE A-17. 
FIGURE A-18. 
FIGURE A-19. 
FIGURE A-20. 
the previous one in that motion is almost completely confined 
to the Y-direction, while in the above event motion was in the 
X-Y plane. This observation shows that 1 1 1 events can originate 
in different parts of the lander. 
'I' events recorded in the Event mode. These events show 
similar properties from one event to the next, indicating 
that they all came from the same source. Although their 
source is most likely in the lander, it is not yet identified. 
Correlation of wind speed with seismic noise on Sol 10. Wind 
gusts of 8 - 9 m/sec produced seismic amplitudes of 8 - 10 DU. 
Detailed correlations are difficult because the seismic 
amplitudes are 1 second averages and the wind speeds are 
widely spaced point samples. 
Correlation of wind speed with smoothed amplitude of Event 
mode seismic data. The solid line shows the expected slope if 
the seismic amplitude is proportional to the square of the 
wind speed. The high degree of correlation is in agreement 
with this relationship. 
Correlation of wind speed with high data rate seismic amplitude, 
In the high data rate, where no averaging is involved, seismic 
noise also correlates with the square of the wind speed. 
FIGURE A-21. 
FIGURE A-22. 
FIGURE A-23. 
FIGURE A-24. 
Axis Crossing histogram for Sol 133 event. The number of 
events is related to the amount of signal at that frequency. 
Because the shape of the histogram reflects the response of 
the system it can be assumed that the wind noise produces a 
nearly flat spectrum and lander resonan.ces are not important. 
Axis Crossing histogram for Sol 139 event. This event is 
similar to the 133 event but slightly richer in high frequencies. 
Spectral estimates of Event mode amplitude for Sol 131 during 
a 51-minute period starting at 20:15:34. The slow decrease 
in power with increase in frequency is typical of wind noise. 
The numbers to the right of the figure are the actual spectral 
estimates with the 32 values for the X axis in the top two rows. 
Sol 12, 16:50 LLT event. This event, and those in the 5 fot-
lowing figures, were chosen as possible marsquakes when first 
observed (also Figures 21 and 22 in text). Chosen mainly for 
their impulsive beginnings, these events were believed to 
have characteristics expected for marsquakes. However, all 
but two have been correlated with wind gusts. This event 
occurred-at a time when no wind data was available. The high 
background level and its occurrence at a time of day when wind 
gusts are common make it highly probable, however, that this is 
a wind generated event. Additional information on ~hese 
events is found in Table 3 in the text. 
FIGURE A-25. 
FIGURE A-26. 
FIGURE A-27. 
FIGURE A-28. 
FIGURE A-29. 
Sol 23 15:15 LLT event. This event correlates with a 12 m/sec 
wind gust. 
Sol 42 15:54 LLT event. This event correlates .with a 11· m/sec 
wind gust. 
Sol 49 13:45 LLT event. Thi-s event correlates with a 12 m/sec 
wind gust. 
Sol 49 14:35 LLT event. This event correlates with an 8 m/sec 
wind gust. 
Sol 49 15:48 LLT event. This event correlates with a 10 m/sec 
wind gust. 
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Mg in two Allende Ca-Al rich inclusions shows large isotopic, mass-dependent fractionation which

enriched the heavier isotopes. After normalization, Mg in these inclusions shows negative δ^(26)Mg which appears to require the presence of nuclear effects in Mg distinct from ^(26)Al decay

Seismology on Mars

Abstract

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