**1. Introduction**

Currently, it is believed that the gravitational accretion process, of material from the protoplanetary disk that orbited the Sun, was the reason by creating Mars about 4.6 billion years ago [1, 2]. At that time, the solar wind accumulated the elements with a lower boiling point on the outermost rocky planet, which explains why the red planet has a higher concentration of Cl, P and S than Earth [3]. Regarding its initial orbit, there are studies [4] that support the theory that its formation occurred in the asteroid belt, taking place around 120 million years later, a migration towards its current position. The presence of liquid water on the surface would gradually disappear as a result of the existence of a tenuous atmosphere and an intense solar wind [5].

In another vein, about 4 billion years ago, during the late heavy bombardment (LHB), most of the impact basins were created on planets'surface [6], which it given rise to the dichotomy between both Northern and Southern hemispheres of the red planet [7].

With regard to Martian geology, it is very important to bear in mind that the record of its evolution is preserved in the rocks and sediments existing on the surface of the red planet. In this sense, and according to [8], minerals can fingerprint many processes that build the Martian rock record. For this reason, and with the purpose of knowing the composition of this planet, infrared spectroscopy instruments have been used in order to make a series of mineralogical maps from orbiters or rovers currently existing on the surface.

As is well known, the surface of Mars is made up of ferric oxides and oxyhydroxides, giving its surface its characteristic red color. However, under the dust layer there is a basaltic crust, which bears some similarity to the terrestrial, more specifically to the oceanic. In relation to the above, it must be emphasized that the early Martian crust, formed during the first billion years, preserves a rich chemical record of multiple and diverse hydrated environments. Nevertheless, the more recent crust exhibits a less frequent and less intense interaction between itself and water [8]. This fact can reinforce the theory of the continuous drying of the planet and, therefore, the presence of high concentrations of salts on the surface.

Regarding its atmosphere, Mars is composed mainly of carbon dioxide (95.7% CO2, 2.1% Ar, 2% N2, traces of O2, CO, water and CH4 among other gases [9]). The mean atmospheric pressure on its surface is 6 mbar, about 0.6% of the mean sea level pressure on Earth. It ranges from a low of 0.30 mbar at the peak of Mount Olympus to more than 11.55 mbar in the depths in Hellas Planitia. Another interesting fact is that the mass of the Martian atmosphere (about 25 1015 kg) is about 200 times less than the Earth's (about 5148 1015 kg).

According to [10], Mars has important similarities to Earth, such as the presence of polar caps, the existence of seasonal changes, and the presence of observable weather patterns. While the climate of Mars has similarities to that of Earth, including periodic glaciations, there are also important differences, such as much lower thermal inertia. Although there has been a notable increase in sublimation in the polar regions, in recent decades there has been a decrease in global temperature, probably due to the same cyclical phenomenon that exists on Earth and, thanks to which, the climate change makes possible, every thousands of years, the appearance of a thermal variation with great repercussions on the entire planet. The fact of being further from the Sun than the Earth, as well as the existence of a tenuous atmosphere that retains little heat, causes the average surface temperature to be about 55°C, with superficial thermal variations from 27°C in summer, in the equator, down to 143°C in the polar caps [11]. It is convenient to emphasize dust storms (wind speed of around 200 km/h) caused by the difference in energy that the planet receives at aphelion and perihelion. Since they occur on a global scale, they cause a decrease in maximum temperatures (due to the decrease in energy from the Sun), and an increase in minimum temperatures.

In general, and with regard to the orography of the planet, [5] specifies that the existing channels, as well as the gullies and the runoff processes associated with them, suggest the presence of liquid water on the surface in the past. Furthermore, taking into account that the atmospheric pressure in the Martian past was ostensibly higher than the current one, and according to [12], raindrops with enough size could be formed to give rise to orographic incidents on the surface.

Regarding the erosion processes, reference [5] obtained a series of predictive algorithms of soil transported volume valid on Mars surface. Other studies [13] specifies that levitation forces enhance the downslope transport on Mars, even though there is evidence that in the past, in the period in which the atmospheric density was such that it allowed the existence of water in a liquid state on its surface, the loss of soil due to

*Prediction of the Transported Soil Volume by the Presence of Water in the Vicinity… DOI: http://dx.doi.org/10.5772/intechopen.102985*

sedimentary transport in watercourses was the force that it modeled the morphology of the Martian surface. In relation to the above, it is necessary to bear in mind the work of reference [14], since one way of being able to study the climatic conditions of Mars (when liquid water existed on the surface) is by observing the value of the angle formed by the valleys network ramifications on Mars. This consideration is due to the fact that, over the years, the angle that these ramifications have usually remains unchanged.

Although numerous studies have been carried out on Mars to date, none of them have obtained the transported soil volume using cross sections methodology. In the same way, no scientific work has inferred an algorithm capable of obtaining a novel model that can predict the rainfall concentration index (RCI) necessary to produce a certain water erosion on the Mars surface. For this reason, this work pretends to be a reference in future studies because this chapter's novel model may be applicable for rocky planets.
