The structure and composition of the atmosphere
Table of Contents
The total mass of the atmosphere is approximately 5.3·1018
kg, against the 1.4·1021 kg mass of the
hydrosphere (oceans, sees, lakes, rivers, groundwater, snow and ice) and
5.98·1024 kg mass of the Earth. The upper border of the
atmosphere is not a well-defined altitude. The atmospheric material steadily decreases
with height, until it gradually reaches interplanetary space. The atmosphere is an
envelope of gases and particles surrounding the Earth. This amount of materials remains
around our planet during the rotation around its axis and orbit around the Sun. - 1.1. Formation of the Earth atmosphere
- 1.2. A short history of the atmospheric chemistry
- 1.3. Atmospheric composition
- 1.4. Vertical structure of the atmosphere
-
- 1.4.1. Vertical change of composition
- 1.4.2. Vertical temperature changes
- 1.5. The planetary boundary layer
The relatively dense area of the Earth's atmosphere is an extremely thin layer compared to the whole atmosphere. Half of the atmosphere’s mass can be found below 5.5 km and around 99% of the air is located in the lower 30 km’s layer. The whole atmosphere actually the same as the range of the magnetosphere (Figure 1.1), which is the result of the interaction between Earth’s natural magnetic field and solar wind[1].
The Earth formed about 4.5 billion years ago, as hot molten rock. It’s first
atmosphere probably contained hydrogen and helium and some simple compounds of
hydrogen, like ammonia (NH3) or methane
(CH4). This first atmosphere of the Earth could similar
to the atmosphere of Jupiter and Saturn today. Because our planet didn’t have a
magnetic field to protect it yet, the intense solar wind from the Sun blew this
early atmosphere away. In essence, the Earth was lost its early atmosphere.
Meanwhile, as the Earth cooled enough, a solid crust with several active volcanoes
was developed about 4.4 billion years ago. By the strong volcanic activity, gases
from the hot interior of our planet reached the surface. These gases – basically
water vapour, carbon dioxide and ammonia – created the secondary atmosphere of the
Earth. The atmospheres of Mars and Venus today – which contain mainly carbon-dioxide
– are similar to this early atmosphere of the Earth.
Over hundred millions of years the atmosphere cooled down gradually, therefore most of water vapour condensed and formed the clouds. Precipitation from these clouds created the oceans. Simultaneously, most of atmospheric carbon-dioxide was absorbed by the oceans. At the same time, light from the Sun broke down the ammonia molecules releasing the chemically inactive nitrogen into the atmosphere (Figure 1.2).
Based on some theory, the oxygen was first produced in the atmosphere by photochemical dissociation of water vapour by intense ultraviolet radiation:
However this amount was negligible and free oxygen was probably produced as a
by-product of photosynthesis[2] by tiny organisms known as cyanobacteria (or blue-green algae) from
around 2.500 millions years ago. Photosynthesis uses carbon dioxide, water, and
light energy releasing organic compounds (carbohydrates) and oxygen:
Initially, the small amount of atmospheric oxygen consumed for oxidation of rocks
at the surface (weathering process). Complete oxidation of the surface rocks, oxygen
levels in the atmosphere began to grow more intensively. As the atmospheric oxygen
reached 1–2% of present oxygen level, ozone (O3) could form
to shield Earth’s surface from intense ultraviolet radiation:
and
At this time, primitive plants formed which facilitated the photosynthesis
process. Land plants developed a few million (based on new studies around 700
million) years ago and would have removed carbon dioxide (from around 1–5% down to
0.04%) at the same time steadily increased the amount of oxygen in the atmosphere.
Oxygen levels fluctuated in the last few million years during various time periods
regulated by climate, volcanism and plate tectonics (Holland, 2006). Finally, the
atmospheric oxygen level stabilized at around 21% (Figure 1.3).
Over hundred millions of years the atmosphere cooled down gradually, therefore most of water vapour condensed and formed the clouds. Precipitation from these clouds created the oceans. Simultaneously, most of atmospheric carbon-dioxide was absorbed by the oceans. At the same time, light from the Sun broke down the ammonia molecules releasing the chemically inactive nitrogen into the atmosphere (Figure 1.2).
Based on some theory, the oxygen was first produced in the atmosphere by photochemical dissociation of water vapour by intense ultraviolet radiation:
2H2O + uv radiation →
2H2 + O2. |
(R1.1) |
CO2 + H2O + sunlight →
organic compounds + O2 |
(R1.2) |
2O2 + uv radiation → O3
+ O |
(R1.3) |
O + O2 = O3. |
(R1.4) |
[1] Solar wind: a stream of charged particles (electrons and protons) ejected
from the upper atmosphere of the Sun.
[2] Photosynthesis: during this process, plants and other organisms convert
light energy from the Sun to chemical energy. Photosynthesis requires
sunlight, carbon-dioxide and water. In plants, photosynthesis
occurs mainly within the leaves.
Table 1.1: Important discoveries of atmospheric elements
Table 1.2: Some important milestones of atmospheric chemistry in the
20th century
After the clarification of fundamental composition of the atmosphere till the late
19th century, the attention was focused on the
atmospheric trace gases with very small concentrations. In the
20th century new research directions were appeared,
namely the analysis of temporal variation of trace gas concentrations and
investigations of chemical reactions in the atmosphere (Table 1.2).
Today, major challenges of atmospheric chemistry are to describe the relationships and feedbacks between chemistry and climate, as well as the exchange processes between the surface and the atmosphere.
occurs mainly within the leaves.
1.2. A short history of the atmospheric chemistry
Greek philosopher, Anaximenes (585–528 BC) declared that air was the primary substance and the source of all other things. Later, Empedocles (ca. 490–430 BC) described the air as one of the four elements (see e.g. May, 2010). This conception was accepted until 18th century. At this time, a question was arisen: whether air is a compound, or a mixture of individual gases. First scientific studies about atmospheric composition were published in the 1700s. Chemical compounds in the atmosphere were discovered one after the other (Table 1.1) to confirm that air is a mixture of gases (see e.g. Anfossi and Sandroni, 1993).Table 1.1: Important discoveries of atmospheric elements
Date
|
Compound
|
Explorer(s)
|
1750s |
carbon dioxide |
Joseph Black |
1766 |
hydrogen |
Henry Cavendish |
1772 |
nitrogen |
Daniel Rutherford |
1774 1772 (published in 1777) |
oxygen |
Joseph Priestley and Carl Wilhelm Scheele |
1840 |
ozone |
Christian Friedrich Schönbein |
1894 |
argon |
Lord Rayleigh and William Ramsay |
Date
|
Explorer(s)
|
Discovery
|
1924 |
Gordon Dobson |
developed a spectrophotometer and started the regular measurements of
total-column ozone |
1930 |
Sydney Chapman |
described theory that explains existence of ozone „layer” |
1960 |
Arie Jan Haagen-Smit |
described the emergence of the photochemical smog |
1973 |
James Lovelock |
first detected CFC’s (Chlorofluorocarbons) in the atmosphere |
1995 |
Paul Crutzen, Mario Molina and Frank Sherwood Rowland |
the Nobel Prize in Chemistry was awarded jointly "for their
work in atmospheric chemistry, particularly concerning the formation
and decomposition of ozone". |
Today, major challenges of atmospheric chemistry are to describe the relationships and feedbacks between chemistry and climate, as well as the exchange processes between the surface and the atmosphere.
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