Team:Brown-Stanford/PowerCell/Background

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Planetary scientists have systematically recorded the density of atmospheric H2O column for the entire surface of Mars, compiling a global map of water vapor.
Planetary scientists have systematically recorded the density of atmospheric H2O column for the entire surface of Mars, compiling a global map of water vapor.
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FIGURE Smith 2001: over entire surface, seasonally averaged water vapor column abundance (in um precipitation)
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FIGURE Smith 2001: over entire surface, seasonally averaged water vapor column abundance (in um precipitation)
From this map it becomes clear that, as on Earth, there are variations in the distribution of atmospheric water vapor based on longitude and latitude. In particular, the Northern hemisphere contains significantly more atmospheric H2O than the South. The figures represent a seasonal average because there are also fluctuations in water vapor content corresponding to the phases of the Martian solar cycle.
From this map it becomes clear that, as on Earth, there are variations in the distribution of atmospheric water vapor based on longitude and latitude. In particular, the Northern hemisphere contains significantly more atmospheric H2O than the South. The figures represent a seasonal average because there are also fluctuations in water vapor content corresponding to the phases of the Martian solar cycle.

Revision as of 18:21, 24 September 2011

Brown-Stanford
iGEM

Photosynthesis on Mars

Photosynthesis on Earth represents an efficient way of converting solar to chemical energy on a large scale. However, photosynthetic output depends on variables such as atmospheric composition and amount of accessible sunlight. In this section we offer an estimate of the usefulness of photosynthesis on Mars by evaluating several environmental conditions.

Atmosphere

H2O Content

Water vapor content on Mars is measured from orbiting satellites (Smith 2001, Melchiorri 2006, Fouchet 2007). Cameras circling Mars can determine the presence of water by using spectrometers to image the planet and noting the intensity of peaks at certain wavelengths. From this information, they can quantify the amount of water vapor existing in a hypothetical column of atmosphere (this is measured in pr-µm, or micrometers of precipitable H2O)


FIGURE Melchiorri 2006: H2O column density at High Northern latitudes (think the “Arctic circle”) for Ls = 101-105


Planetary scientists have systematically recorded the density of atmospheric H2O column for the entire surface of Mars, compiling a global map of water vapor.

FIGURE Smith 2001: over entire surface, seasonally averaged water vapor column abundance (in um precipitation)

From this map it becomes clear that, as on Earth, there are variations in the distribution of atmospheric water vapor based on longitude and latitude. In particular, the Northern hemisphere contains significantly more atmospheric H2O than the South. The figures represent a seasonal average because there are also fluctuations in water vapor content corresponding to the phases of the Martian solar cycle.


FIGURE Smith 2001: Fluctuation of total atmospheric water vapor levels over time, northern and southern hemispheres

Dust particulate in the Martian Atmosphere

Solar irradiance

Estimating the extent of energy conversion

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