mirrored file at http://SaturnianCosmology.Org/ 
For complete access to all the files of this collection
	see http://SaturnianCosmology.org/search.php 
==========================================================
[1][LINK] 

[2]Home [3]Table of Contents [4]What's New [5]Image Index [6]Copyright
[7]Puzzles [8]Shopping [9]Search 

[10]Martian System 

_Mars Introduction_

_Where there is no vision, the people perish.
- Proverbs 29:18_

Table of Contents
Mars Introduction[11]Mars Statistics[12]Animations of Mars[13]Views of
Mars[14]Mars Moon Summary
Moons of Mars
[15]Deimos, [16]Phobos

Mars Science
[17]New Images Suggest Present-Day Sources of Liquid Water on
Mars[18]The Surface of Mars[19]Mars Pathfinder Mission[20]Water
History, Rock Composition[21]Life from Mars: The Discovery[22]Martian
Volcanoes[23]Martian Clouds[24]The Face on Mars and other Familiar
Features[25]No Evidence of Ocean Shorelines[26]Rootless Cones or
Pseudocraters[27]3-D View of Mars Reveals . . .[28]The Rationale for
Exploring Mars[29]Chronology of Mars Exploration[30]Project Viking
Fact Sheet[31]Magnetic Stripes Preserve Record of Ancient
Mars[32]Planetary Icosahedrons[33]Mars Image/Animation Gallery
Historical Books
[34]The Martian Landscape[35]Viking Orbiter Views of Mars[36]On Mars:
Exploration of the Red Planet

Mars Resources
[37]Mars Pathfinder Mission[38]Mars Global Surveyor[39]Mars
Missions[40]Mars Landing Site Catalog[41]Daily Martian Weather
Report[42]MSSS Viking Image Archive[43]Center for Mars Exploration.
[44]Uncovering the Secrets of the Red Planet,
by Paul Raeburn, National Geographic,
$28.00 Hardcover - 1998
[45]Life on Mars,
by Patrick Moore,
$4.50 Hardcover - 1996
[46]Mars: The Living Planet,
by Barry E. Digregorio,
$17.50 Hardcover - 1997
[47]Atlas of Volcanic Landforms on Mars,
by Carroll Ann Hodges,
$17.00 Hardcover - 1996
[48]The Hunt for Life on Mars,
by Donald Goldsmith,
$19.96 Paperback - 1997
[49]The NASA Atlas of the Solar System,
by Ronald Greeley,
$108.50 Hardcover - 1996

[50][LINK] 

Mars is the fourth planet from the Sun and is commonly referred to as
the Red Planet. The rocks, soil and sky have a red or pink hue. The
distinct red color was observed by stargazers throughout history. It
was given its name by the Romans in honor of their god of war. Other
civilizations have had similar names. The ancient Egyptians named the
planet _Her Descher_ meaning _the red one_.

Before space exploration, Mars was considered the best candidate for
harboring extraterrestrial life. Astronomers thought they saw straight
lines crisscrossing its surface. This led to the popular belief that
irrigation canals on the planet had been constructed by intelligent
beings. In 1938, when Orson Welles broadcasted a radio drama based on
the science fiction classic _War of the Worlds_ by H.G. Wells, enough
people believed in the tale of invading Martians to cause a near
panic.

Another reason for scientists to expect life on Mars had to do with
the apparent seasonal color changes on the planet's surface. This
phenomenon led to speculation that conditions might support a bloom of
Martian vegetation during the warmer months and cause plant life to
become dormant during colder periods.

In July of 1965, [51]Mariner 4, transmitted 22 close-up pictures of
Mars. All that was revealed was a surface containing many craters and
naturally occurring channels but no evidence of artificial canals or
flowing water. Finally, in July and September 1976, [52]Viking Landers
1 and 2 touched down on the surface of Mars. The three biology
experiments aboard the landers discovered unexpected and enigmatic
chemical activity in the Martian soil, but provided no clear evidence
for the presence of living microorganisms in the soil near the landing
sites. According to mission biologists, Mars is self-sterilizing. They
believe the combination of solar ultraviolet [53]radiation that
saturates the surface, the extreme dryness of the soil and the
oxidizing nature of the soil chemistry prevent the formation of living
organisms in the Martian soil. The question of life on Mars at some
time in the distant past remains open.

Other instruments found no sign of organic chemistry at either landing
site, but they did provide a precise and definitive analysis of the
composition of the Martian atmosphere and found previously undetected
trace elements.

Atmosphere

The atmosphere of Mars is quite different from that of Earth. It is
composed primarily of carbon dioxide with small amounts of other
gases. The six most common components of the atmosphere are:
* Carbon Dioxide (CO2): 95.32%
* Nitrogen (N2): 2.7%
* Argon (Ar): 1.6%
* Oxygen (O2): 0.13%
* Water (H2O): 0.03%
* Neon (Ne): 0.00025 %

Martian air contains only about 1/1,000 as much water as our air, but
even this small amount can condense out, forming clouds that ride high
in the atmosphere or swirl around the slopes of towering volcanoes.
Local patches of early morning fog can form in valleys. At the Viking
Lander 2 site, a thin layer of water frost covered the ground each
winter.

There is evidence that in the past a denser martian atmosphere may
have allowed water to flow on the planet. Physical features closely
resembling shorelines, gorges, riverbeds and islands suggest that
great rivers once marked the planet.

Temperature and Pressure

The average recorded temperature on Mars is -63° C (-81° F) with a
maximum temperature of 20° C (68° F) and a minimum of -140° C (-220°
F).

Barometric pressure varies at each landing site on a semiannual basis.
Carbon dioxide, the major constituent of the atmosphere, freezes out
to form an immense polar cap, alternately at each pole. The carbon
dioxide forms a great cover of snow and then evaporates again with the
coming of spring in each hemisphere. When the southern cap was
largest, the mean daily pressure observed by Viking Lander 1 was as
low as 6.8 millibars; at other times of the year it was as high as 9.0
millibars. The pressures at the Viking Lander 2 site were 7.3 and 10.8
millibars. In comparison, the average pressure of the Earth is 1000
millibars.

Mars Statistics
Mass (kg) 6.421e+23
Mass (Earth = 1) 1.0745e-01
Equatorial radius (km) 3,397.2
Equatorial radius (Earth = 1) 5.3264e-01
Mean density (gm/cm^3) 3.94
Mean distance from the Sun (km) 227,940,000
Mean distance from the Sun (Earth = 1) 1.5237
Rotational period (hours) 24.6229
Rotational period (days) 1.025957
Orbital period (days) 686.98
Mean orbital velocity (km/sec) 24.13
Orbital eccentricity 0.0934
Tilt of axis (degrees) 25.19
Orbital inclination (degrees) 1.850
Equatorial surface gravity (m/sec^2) 3.72
Equatorial escape velocity (km/sec) 5.02
Visual geometric albedo 0.15
Magnitude (Vo) -2.01
Minimum surface temperature -140°C
Mean surface temperature -63°C
Maximum surface temperature 20°C
Atmospheric pressure (bars) 0.007
Atmospheric composition
Carbon Dioxide (C02)
Nitrogen (N2)
Argon (Ar)
Oxygen (O2)
Carbon Monoxide (CO)
Water (H2O)
Neon (Ne)
Krypton (Kr)
Xenon (Xe)
Ozone (O3)
95.32%
2.7%
1.6%
0.13%
0.07%
0.03%
0.00025%
0.00003%
0.000008%
0.000003%

Animations of Mars

* [54]Rotating Mars Movie.
* [55]Mars Topography Movie.
* [56]Animation of Tharsis Tholus.
* [57]Animation of the Olympus Mons Caldera.
* [58]Mars Global Surveyor Animation.
* [59]Mars the Movie.
* [60]Flight over Valles Marineris.
* [61]Animation of Martian Poles.
* [62]Animation over Olympus Mons.
* [63]Hubble Telescope full-globe animation.

Views of Mars

[64]Ingterior of Mars _The Interior of Mars_
The current understanding of the interior of Mars suggests that it can
be modeled with a thin crust, similar to Earth's, a mantle and a core.
Using four parameters, the Martian core size and mass can be
determined. However, only three out of the four are known and include
the total mass, size of Mars, and the moment of inertia. Mass and size
was determined accurately from early missions. The moment of inertia
was determined from Viking lander and Pathfinder Doppler data, by
measuring the precession rate of Mars. The fourth parameter, needed to
complete the interior model, will be obtained from future spacecraft
missions. With the three known parameters, the model is significantly
constrained. If the Martian core is dense (composed of iron) similar
to Earth's or SNC meteorites thought to originate from Mars, then the
minimum core radius would be about 1300 kilometers. If the core is
made out of less-dense material such as a mixture of sulfur and iron,
the maximum radius would probably be less than 2000 kilometers.
_(Copyright 1998 by Calvin J. Hamilton)_
[65]Topography Map of Mars _Topography Map of Mars_
This image is a newly released topographic map of Mars. The full range
of topography on Mars is about 19 miles (30 kilometers), one and a
half times the range of elevations found on Earth, The most curious
aspect of the map is the striking difference between the planet's low,
smooth Northern Hemisphere and the heavily cratered Southern
Hemisphere," which sits, on average, about three miles (five
kilometers) higher than the north. _(Courtesy GSFC/NASA)_
[66]Schiaparelli Hemisphere of Mars _Schiaparelli Hemisphere_
This image is a mosaic of the Schiaparelli hemisphere of Mars. The
center of this image is near the impact crater Schiaparelli, 450
kilometers (280 miles) in diameter. The dark streaks with bright
margins emanating from craters in the Oxie Palus region, upper left of
image, are caused by erosion and/or deposition by the wind. Bright
white areas to the south, including the Hellas impact basin at extreme
lower right, are covered by carbon dioxide frost. _(Courtesy USGS)_
[67]Valles Marineris _Valles Marineris_
This image is a mosaic of the Valles Marineris [VAL-less
mar-uh-NAIR-iss] hemisphere of Mars. It is a view similar to that
which one would see from a spacecraft. The center of the scene shows
the entire Valles Marineris canyon system, more than 3,000 kilometers
(1,860 miles) long and up to 8 kilometers (5 miles) deep, extending
from Noctis Labyrinthus, the arcuate system of graben to the west, to
the chaotic terrain to the east. Many huge ancient river channels
begin from the chaotic terrain and north-central canyons and run
north. Many of the channels flowed into a basin called Acidalia
Planitia, which is the dark area in the extreme north of this picture.
The three Tharsis volcanoes (dark red spots), each about 25 kilometers
(16 miles) high, are visible to the west. Very ancient terrain covered
by many impact craters lies to the south of Valles Marineris.
_(Courtesy USGS)_
[68]Candor Chasm _Central Candor Chasm - Oblique View_
This image shows part of Candor Chasm in Valles Marineris. It is
centered at Latitude -5.0, Longitude 70.0. The view is from the north
looking into the chasm. Candor Chasm's geomorphology is complex,
shaped by tectonics, mass wasting, wind, and perhaps by water and
volcanism. _(Courtesy USGS)_
[69]Candor Chasm _West Candor Chasm (Enhanced Color)_
This picture (centered at latitude 4° S, longitude 76° W) shows areas
of central Valles Marineris, including Candor Chasm (lower left),
Ophir Chasm (lower right), and Hebes Chasm (upper right). Complex
layered deposits in the canyons may have been deposited in lakes, and
if so, are of great interest for future searches for fossil life on
Mars. The pinkish deposits in Candor Chasm may be due to hydrothermal
alterations and the production of crystalline ferric oxides.
_((Geissler et al., 1993, Icarus 106,380). Viking Orbiter Picture
Numbers 279B02 (violet), 279B10 (green), and 279B12 (red) at 240
meters/pixel resolution. Picture width is 231 kilometers. North is 47°
clockwise from top.)_
[70]Ophir Chasma _Ophir Chasma_
Ophir Chasma is a large west-northwest-trending trough about 100 km
wide. The Chasma is bordered by 4 km high walled cliffs, most likely
faults, that show spur-and-gully morphology and smooth sections. The
walls have been dissected by landslides forming reentrants; one area
(upper left) on the north wall shows a young landslide about 100 km
wide. The volume of the landslide debris is more than 1000 times
greater than that from the May 18, 1980 debris avalanche from Mount
St. Helens. The longitudinal grooves seen in the foreground are
thought to be due to differential shear and lateral spreading at high
velocities. The landslide passes between mounds of interior layered
deposits on the floor of the chasma. _(Courtesy USGS)_
[71]Landslide in Valles Marineris _Landslide in Valles Marineris_
Although Valles Marineris originated as a tectonic structure, it has
been modified by other processes. This image shows a close-up view of
a landslide on the south wall of Valles Marineris. This landslide
partially removed the rim of the crater that is on the plateau
adjacent to Valles Marineris. Note the texture of the landslide
deposit where it flowed across the floor of Valles Marineris. Several
distinct layers can be seen in the walls of the trough. These layers
may be regions of distinct chemical composition or mechanical
properties in the Martian crust. _(Copyright Calvin J. Hamilton;
Caption: LPI)_
[72]Hubble Images of Mars _HST 3 Views of Mars at Opposition_
These Hubble Space Telescope views provide the most detailed complete
global coverage of the Red Planet ever seen from Earth. The pictures
were taken on February 25, 1995, when Mars was at a distance of 103
million kilometers (65 million miles). To the surprise of researchers,
Mars is cloudier than seen in previous years. This means the planet is
cooler and drier, because water vapor in the atmosphere freezes out to
form ice-crystal clouds. The three images show the Tharsis, Valles
Marineris and Syrtis Major regions. _(Credit: Philip James, University
of Toledo; Steven Lee, University of Colorado; and NASA)_
[73]Springtime on Mars _Springtime on Mars: Hubble's Best View of the
Red Planet_
This NASA Hubble Space Telescope view of Mars is the clearest picture
ever taken from Earth, surpassed only by close-up shots sent back by
visiting space probes. The picture was taken on February 25, 1995,
when Mars was at a distance of approximately 103 million kilometers
(65 million miles) from Earth.

Because it is spring in Mars' northern hemisphere, much of the carbon
dioxide frost around the permanent water-ice cap has sublimated, and
the cap has receded to its core of solid water-ice several hundred
miles across. The abundance of wispy white clouds indicates that the
atmosphere is cooler than seen by visiting space probes in the 1970s.
Morning clouds appear along the planet's western (left) limb. These
form overnight when Martian temperatures plunge and water in the
atmosphere freezes out to form ice-crystal clouds. Towering 25
kilometers (16 miles) above the surrounding plains, volcano Ascraeus
Mons pokes above the cloud deck near the western or limb. Valles
Marineris is in the lower left. _(Credit: Philip James, University of
Toledo; Steven Lee, University of Colorado; and NASA)_
[74]Channel Ravi Vallis _Outflow Source of Channel Ravi Vallis_
This image of the head of Ravi Vallis shows a 300-kilometer (186-mile)
long portion of a channel. Like many other channels that empty into
the northern plains of Mars, Ravi Vallis orginates in a region of
collapsed and disrupted ("chaotic") terrain within the planet's older,
cratered highlands. Structures in these channels indicate that they
were carved by liquid water moving at high flow rates. The abrupt
beginning of the channel, with no apparent tributaries, suggests that
the water was released under great pressure from beneath a confining
layer of frozen ground. As this water was released and flowed away,
the overlying surface collapsed, producing the disruption and
subsidence shown here. Three such regions of chaotic collapsed
material are seen in this image, connected by a channel whose floor
was scoured by the flowing water. The flow in this channel was from
west to east (left to right). This channel ultimately links up with a
system of channels that flowed northward into Chryse Basin.
_(Copyright Calvin J. Hamilton; Caption: LPI)_
[75]Streamlined Islands _Streamlined Islands_
The water that carved the channels to the north and east of the Valles
Marineris canyon system had tremendous erosive power. One consequence
of this erosion was the formation of streamlined islands where the
water encountered obstacles along its path. This image shows two
streamlined islands that formed as the water was diverted by two 8-10
kilometer (5-6 mile) diameter craters lying near the mouth of Ares
Vallis in Chryse Planitia. The water flowed from south to north
(bottom to top of the image). The height of the scarp surrounding the
upper island is about 400 meters (1,300 feet), while the scarp
surrounding the southern island is about 600 meters (2,000 feet) high.
_(Copyright Calvin J. Hamilton; Caption: LPI)_
[76]Mars: Valley Network _Valley Network_
Unlike the features shown in the above two images, many systems on
Mars do not show evidence of catastrophic flooding. Instead, they show
a resemblance to drainage systems on Earth, where water acts at slow
rates over long periods of time. As on Earth, the channels shown here
merge together to form larger channels.

However, these valley networks are less developed than typical
terrestrial drainage systems, with the Martian examples lacking
small-scale streams feeding into the larger valleys. Because of the
absence of small-scale streams in the Martian valley networks, it is
thought that the valleys were carved primarily by ground water flow
rather than by runoff of rain. Although liquid water is currently
unstable on the surface of Mars, theoretical studies indicate that
flowing groundwater might be able to form valley networks if the water
flowed beneath a protective cover of ice. Alternatively, because the
valley networks are confined to relatively old regions of Mars, their
presence may indicate that Mars once possessed a warmer and wetter
climate in its early history. _(Copyright Calvin J. Hamilton; Caption:
LPI)_
[77]Mars South Pole _South Polar Cap_
This image shows the south polar cap of Mars as it appears near its
minimum size of about 400 kilometers (249 miles). It consists mainly
of frozen carbon dioxide. This carbon dioxide cap never melts
completely. The ice appears reddish due to dust that has been
incorporated into the cap. _(Courtesy NASA)_
[78]Mars North Pole _North Polar Cap_
This image is an oblique view of the north polar cap of Mars. Unlike
the south polar cap, the north polar cap probably consists of
water-ice. _(Copyright Calvin J. Hamilton)_
[79]Mars Laminated Terrain _Polar Laminated Terrain_
One of the discoveries of the Mariner 9 spacecraft was that the south
polar cap of Mars was made of thin layers or laminations of ice and
sediment. Four years later, on October 10, 1976, the Viking 2
spacecraft took this picture of the Martian north polar cap. The
visible layering occurred as a result of wind born dust settling upon
the polar cap. As the caps experience climatic variations, they expand
and contract. The layers of dust sediment tend to grow thicker near
the poles where ice deposits remain for longer periods of time. The
thickness of the deposits indicates they were formed during cyclical
climatic variation rather than annual changes. As ice withdraws from a
region, wind exposes the layers sculpting valleys and scarps. The
formation of layered deposits is an active process today. _(Copyright
1998 by Calvin J. Hamilton)_
[80]Mars Dunefield _Dunefield_
This image shows several dune types which are found in the north
circumpolar dunefield. This thumnail image shows a section of
transverse dunes. The full image has a field of traverse dunes on the
left and barchan dunes on the right with a transition zone inbetween.
Transverse dunes are oriented perpendicular to the prevailing wind
direction. They are long and linear, and frequently join their
neighbor in a low-angle "Y" junction. Barchan dunes are
crescent-shaped mounds with downwind-pointing horns. These dunes are
comparable in size to the largest dunes found on the Earth.
_(Copyright Calvin J. Hamilton)_
[81]Mars Local Dust Storm _Local Dust Storm_
Local dust storms are relatively common on Mars. They tend to occur in
areas of high topographic and/or high thermal gradients (usually near
the polar caps), where surface winds would be strongest. This storm is
several hundreds of kilometers in extent and is located near the edge
of the south polar cap. Some local storms grow larger, others die out.
_(Copyright Calvin J. Hamilton; caption by LPI)_
[82]Mars: White Rock _White Rock_
This image shows a lesser known, but unusual feature on Mars. It is
commonly called _"White Rock"_. The white feature is eroded crater
fill, but exactly how it was formed has not been satisfactorily
explained. White Rock was not formed by polar processes because it
lies near to the equator at latitude -8 degrees and longitude 355
degrees. It has been modified through aeolian erosion showing
transverse and longitudinal erosional features. _(Copyright 1998 by
Calvin J. Hamilton)_
[83]Martian Atmosphere _Martian Atmosphere_
This oblique image taken by the Viking orbiter spacecraft shows a thin
band of the Martian atmosphere. This image looks northeast across the
Argyre basin. The Argyre basin is about 600 kilometers across with a
rugged rim of about 500 kilometers in width. _(Copyright 1997 by
Calvin J. Hamilton)_

Mars Moon Summary

The following table summarizes the radius, mass, distance from the
planet center, discoverer and the date of discovery of each of the
moons of Mars:

Moon   #  Radius(km)   Mass(kg)   Distance(km) Discoverer Date
Phobos I 13.5x10.8x9.4 1.08e+16    9,380         A. Hall 1877
Deimos II  7.5x6.1x5.5 1.80e+15   23,460         A. Hall 1877

References

Beatty, J. K. and A. Chaikin, eds. _The New Solar System_.
Massachusetts: Sky Publishing, 3rd Edition, 1990.

Carr M. H. _The Surface of Mars_. Yale University Press, New Haven,
1981.

Kiefer, Walter S., Allan H. Treiman, and Stephen M. Clifford. _The Red
Planet: A Survey of Mars - Slide Set._ Lunar and Planetary Institute.

Mutch T. A., Arvidson R. E., Head J. W. III, Jones K. L., and Saunders
R. S. _The Geology of Mars._ Princeton University Press, Princeton,
1976.

Williams, Steven H. _The Winds of Mars: Aeolian Activity and Landforms
- Slide Set._ Lunar and Planetary Institute.

[87]HOME [88]Return to Earth [89]Voyage to Jupiter

_Copyright © 1997-2001 by [90]Calvin J. Hamilton. All rights reserved._
[91]Privacy Statement.

[92][LINK] 

References

1. http://ad.doubleclick.net/jump/sonar.planetscapes/ros;sz=468x60;num=1234567
2. http://www.solarviews.com/eng/homepage.htm
3. http://www.solarviews.com/eng/toc.htm
4. http://www.solarviews.com/eng/new.htm
5. http://www.solarviews.com/cap/index/index.html
6. http://www.solarviews.com/eng/copyright.htm
7. http://crpuzzles.com/
8. http://www.solarviews.com/store/index.html
9. http://www.solarviews.com/eng/search.htm
10. http://www.solarviews.com/cap/mars/marssystem.htm
11. file://localhost/www/sat/files/comets/mars.htm#stats
12. file://localhost/www/sat/files/comets/mars.htm#movie
13. file://localhost/www/sat/files/comets/mars.htm#views
14. file://localhost/www/sat/files/comets/mars.htm#moons
15. http://www.solarviews.com/eng/deimos.htm
16. http://www.solarviews.com/eng/phobos.htm
17. http://www.solarviews.com/eng/marspr3.htm
18. http://www.solarviews.com/eng/marssurf.htm
19. http://www.solarviews.com/eng/pathfind.htm
20. http://www.solarviews.com/eng/pathpr1.htm
21. http://www.solarviews.com/eng/marslif1.htm
22. http://www.solarviews.com/eng/marsvolc.htm
23. http://www.solarviews.com/eng/marscld.htm
24. http://www.solarviews.com/eng/face.htm
25. http://www.solarviews.com/eng/marspr1.htm
26. http://www.solarviews.com/eng/marspr2.htm
27. http://www.solarviews.com/eng/mars3d.htm
28. http://www.solarviews.com/eng/marswhy.htm
29. http://www.solarviews.com/eng/craft2.htm#mars
30. http://www.solarviews.com/eng/vikingfs.htm
31. http://www.solarviews.com/eng/marsmag.htm
32. http://planetscapes.com/maps/ico.html
33. http://www.solarviews.com/cap/index/mars1.html
34. http://www.solarviews.com/history/SP-425/index.html
35. http://www.solarviews.com/history/SP-441/index.html
36. http://www.solarviews.com/history/SP-4212/index.html
37. http://mpfwww.jpl.nasa.gov/default.html
38. http://mpfwww.jpl.nasa.gov/mgs/index.html
39. http://mpfwww.jpl.nasa.gov/
40. http://cmex-www.arc.nasa.gov/MarsTools/Mars_Cat/Mars_Cat.html
41. http://nova.stanford.edu/projects/mgs/dmwr.html
42. http://barsoom.msss.com/http/vikingdb.html
43. http://cmex-www.arc.nasa.gov/
44. http://www.amazon.com/exec/obidos/ISBN=0792273737/viewsofthesolarsA/
45. http://www.amazon.com/exec/obidos/ISBN=0393052257/viewsofthesolarsA/
46. http://www.amazon.com/exec/obidos/ISBN=1883319587/viewsofthesolarsA/
47. http://www.amazon.com/exec/obidos/ISBN=9994032208/viewsofthesolarsA/
48. http://www.amazon.com/exec/obidos/ISBN=0525943366/viewsofthesolarsA/
49. http://www.amazon.com/exec/obidos/ISBN=0521561272/viewsofthesolarsA/
50. http://media.fastclick.net/w/click.here?sid=4218&m=3&c=1
51. http://www.solarviews.com/eng/marin4.htm
52. http://www.solarviews.com/eng/viking.htm
53. http://www.solarviews.com/eng/terms.htm#radiation
54. http://www.solarviews.com/cap/mars/vmars3.htm
55. http://www.solarviews.com/cap/mars/vmars4.htm
56. http://www.solarviews.com/cap/mars/vtharsis.htm
57. http://www.solarviews.com/cap/mars/voly1.htm
58. http://www.solarviews.com/cap/mars/vidmars5.htm
59. http://www.solarviews.com/cap/mars/vidmars1.htm
60. http://www.solarviews.com/cap/mars/vidmars2.htm
61. http://www.solarviews.com/cap/mars/vidmars3.htm
62. http://www.solarviews.com/cap/mars/vidmars4.htm
63. http://www.solarviews.com/cap/mars/vmars2.htm
64. http://www.solarviews.com/cap/mars/marsint.htm
65. http://www.solarviews.com/cap/mgs/mgstopo2.htm
66. http://www.solarviews.com/cap/mars/me04s341.htm
67. http://www.solarviews.com/cap/mars/me07s078.htm
68. http://www.solarviews.com/cap/mars/05s070.htm
69. http://www.solarviews.com/cap/mars/pia155.htm
70. http://www.solarviews.com/cap/mars/ophir.htm
71. http://www.solarviews.com/cap/mars/slump.htm
72. http://www.solarviews.com/cap/mars/mars3.htm
73. http://www.solarviews.com/cap/mars/mars060.htm
74. http://www.solarviews.com/cap/mars/outflow.htm
75. http://www.solarviews.com/cap/mars/islands.htm
76. http://www.solarviews.com/cap/mars/network.htm
77. http://www.solarviews.com/cap/mars/southpol.htm
78. http://www.solarviews.com/cap/mars/northpol.htm
79. http://www.solarviews.com/cap/mars/layers.htm
80. http://www.solarviews.com/cap/mars/dune1.htm
81. http://www.solarviews.com/cap/mars/lcldust.htm
82. http://www.solarviews.com/cap/mars/whiterk.htm
83. http://www.solarviews.com/cap/mars/marsatmo.htm
84. http://www.solarviews.com/eng/phobos.htm
85. http://www.solarviews.com/eng/people.htm#hall
86. http://www.solarviews.com/eng/deimos.htm
87. http://www.solarviews.com/eng/homepage.htm
88. http://www.solarviews.com/eng/earth.htm
89. http://www.solarviews.com/eng/jupiter.htm
90. http://www.solarviews.com/eng/author.htm
91. http://www.solarviews.com/eng/privacy.htm
92. http://ad.doubleclick.net/jump/sonar.planetscapes/ros;sz=468x60;num=1234567