The topics are presented in viewgraph form and include the following: mass and composition; photochemical processes; temperatures and winds; general circulation; and dust storms

Haberle, Robert M.

English

NASA Technical Reports Server

Topics:
THE MARTIAN LOWER ATMOSPHERE
Robert M. Haberle
National Aeronautics and Space Administration
Ames Research Center
Moffett Field, California 94035
N93-26894
- Mass and composition
- Photochemical processes
- Temperatures and winds
- General Circulation
- Dust storms
BASIC PFrOPERTIES'=OF MARS AND EARTH
==. =:?
PLANETARY PROPERTIES MARS EARTH
MASS, kg
RADIUS, m
ACCELERATION OF GRAVITY, m/see 2
ORBIT ECCENTRICITY
SPIN-AXIS INCLINATION, deg
LENGTH OF YEAR, Earth days
LENGTH OF SOLAR DAY, sec
SOLAR CONSTANT, W/m 2
6.46 x 1023 5.98 x 1024
3394 6369
3.72 9.81
0.093 0.017
25.2 23.5
687 365
88,775 86,400
591 1373
ATMOSPHERIC PROPERTIES MARS EARTH
PRINCIPAL CONSTITUENTS, by volume CO2 (95.3%) N 2 (78.1%1
N2 (2.7%) 0 2 (20.9%)
Ar 40 (1.6%) Ar 40 (0.9%)
02 (0.13%) CO 2 (0.03%)
44 29
2.4 x 1016 5.3 x 1018
6 1013
145-245 220-310
MEAN MOLECULAR WEIGHT
TOTAL MASS, kg
MEAN SURFACE PRESSURE, mbar
NEAR-SURFACE TEMPERATURE RANGE, K
39
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Jarosky, B.M. and Farmer, B., J. Geophys. Res., 87, 2999-3019, 1982, copyright by the
American Geophysical Union.
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Farmer, C.B. and Doms, P.E., J. Geophys. Res., 84, No. B6, 2881-2888, 1979, copyright by the
American Geophycial Union.
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45
Particles in
the
atmosphere
composition
density
sire distribution
concen_afion
Measurement Model
< 60% SiO2
1% magnetite
raogg: r = 0.1 - 10p.m
mean: r = 0.4 - 2.5 lam
N - NOx exp(-z/H)
where NO = 6 particles/era 3,
•t is the visible optical depth,
z is height (kin), and H = 10
km is an atmospheric scale
height.
Ideas
p = 2-3 gm/cm 3
Notes
SiO2 measurement based on
inferences from Mariner 9 IRIS
spectra - loosely constrained. Value
quoted is higher than Viking lander
soil elemental composition
measurements.
Based on typical silicate rock
densities. Considered a good
estimate.
Measurements based on inferences
from Mariner 9 IRIS spectra, and
Viking Lander Sun Diode images.
Considerable uncertainty in
concentrations of sub-micron
particles. Means are cross-mcfional
weighted.
Based on the Mariner 9 inferred
particle size distribution assuming r
= 2.5 lma and p = 3 gm/cm 3. See
Appendix A.
vertical
distribution
geographicM
distribution
seasonal
variability
'opfic_
properties
-ground visibility
_space-to-ground
visibility
Background dust
haze extends 30-70
km above the
surface. During great
dust storms,
panicles can reach
70 km.
Dust storm neriods!
regional to global.
Non-duststorm
_: localized
storms can occur
anywhere.
Maximum dust
loading occurs
during southern
spring and summer.
Solar optical depth
varies from 0 to 6 or
above.
No surface features
were visible from
orbit during the first
half of the 1971
storm.
Xvis/_ - 2
solar transmissivity ~
-1
(!+2_)
2_t
Visual Range (kin)~ lOlx
Backeround dust haze:
particles are unifromly
distributed with height.
Develooin2 storms: particles
are concenh'ated near the
surface in source regions;
aloft elswhere. Particles
with radii >> 5 I.tmfall out
quickly.
Maximum concentrations
tend to occur in tropical
regi_ms.
Consistent With twilight
observations and sky brightness
measurements. Loosely
constrained.
Highly variable.
Optical depth always > 0.2 at the
Viking lander sites. Solar
transmissivity is that for purely
scattering dust particles, and is
therclbre an approximation.
Visualrangefor distinguishing a
black target againsta diffuse white
background.
46
BLANK NOT FILMED
2_07 I _ I I I t
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18 X_- 4:13 PM U_tT
( _ULY_, 1_6
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9.-06 AM LMT _ /
140 -- SEPT. 3, 1976 _
- ¢-4 _-iN-
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TE..',APS.:_A TUR S (1<)
Seiff, A. and Kirk, D.B., J. Geophys. Res., 82, No. 28, 4364-4378, 1977, copyright by the
American I_leophysical Union.
DAILY AIR TEMPERAIURESAT VIKING LANDER1
25O
2_
220
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180
140
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VL-I SOLS
Ryan, J.A. and Henry, R.M., J. Geophys. Res., 84, No. B6, 2821-2829, 1979, copyright by the
American Geophysical Union.
47
Fig. I_
,1o I i . i I
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. _ J'+, . /+'-"
40
i
Pal, l_,
Fill. 18. D+utnal surl'mcetemperature meal1 and e,_lrem,'*/'or lhe primary Viking thermal model (A* - 0.25 and I -
6.5). The clashedlines indicate the s,'msonJlrange o1' the primary mission. (a) I_faximum lemlxtalures. (b) M;nimum
temperatures. (c) Mean temperatures.
Kelffer, H. et al., J. Geophys. Res., 82, No. 28, 4249-4291, 1977, copyright by the AmericanGeophysical Union.
48
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Hess, S.M., et al., J. Geophys. Res., 82, No. 28, 4559-4574, 1977, copyright by the American
Geophysical Union.
.==oI" i. 't
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Ryan, J.A. et al., J. Geophys. Res., 87, No. C9, 7279-7284, 1982, copyright by the American
Geophysical Union.
49
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Dust Storm Characteristics
- Require strong near-surface winds (> 30 m/s)
- Occur on a variety of scales
- Local dust storms
• last a few days
• spatially confined (< 25 km, < 10"'6 km**2)
• occur every year and probably in every season
• there are preferred locations, but can occur anywhere
• visible opacities vary: x ~ 1-6
-Regional dust storms
• last from days - months, cover large areas, extend to great heights
• start small then expand
• tend to occur during southern spring and summer
• may envelop much of the planet !
• visible opacities vary: x ~ 2-6
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The Martian lower atmosphere

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