Topography of Mars

Running from the eastern flanks of the rise, roughly along the equator, is Valles Marineris, a split in the martian crust 4000 km long (about a fifth of the martian circumference), up to 600 km wide and 7 km deep. The Grand Canyon is a mere 450 km long, up to 29 km wide and 1.6 km deep.

Then there is the Hellas Basin in the southern hemisphere, which is an enormous impact crater 2300 km in diameter and more than 9 km deep. But perhaps most striking of all is the general difference in height and surface roughness between the northern and southern hemispheres. The northern hemisphere is smooth and flat and on average 6 km lower than the rugged highlands of the south.  
 

	Olympus Mons, 25 kilometres high, is the highest volcano in the Solar System

Water and life
 
Three decades of space exploration have also revealed that Mars is a cold, dry place with a thin atmosphere, consisting mainly of carbon dioxide. There is evidence, though, that conditions were very different early in the planet's history (3.8 billion years ago). Mars may once have been warm and wet.

If liquid water did flow on early Mars, could life have evolved there? The more we know about life on Earth, the more likely it seems that life could exist elsewhere. Over recent years, micro-organisms have turned up in the most inhospitable niches on Earth, where nobody previously thought anything could survive.
 
 
An energy source and water seem to be the only two essential prerequisites for life common to these niches. Water may once have flowed freely on Mars and, like the Earth, the planet receives sunlight and has its own internal energy source. So the odds on primitive life thriving for at least some time during the planet’s history are reasonably good.