The document summarizes the main layers of Earth's atmosphere:
- The troposphere is the lowest layer where weather occurs.
- The stratosphere lies above, where temperature increases with altitude due to ozone absorption. It contains the ozone layer.
- The mesosphere is the coldest layer, where temperatures decrease with altitude.
- Above is the thermosphere, where temperatures continually rise with altitude. It contains the ionosphere, where solar radiation ionizes molecules.
- The outermost layers are the exosphere, where the atmosphere thins out, and the magnetosphere, which is influenced by the Earth's magnetic field.
its a small view of layers of atmosphere! maximum every person have to know this type of information etiher they're engineer, doctor or accountant! it's a basic for our lives!
its a small view of layers of atmosphere! maximum every person have to know this type of information etiher they're engineer, doctor or accountant! it's a basic for our lives!
this ppt is mainly for the students of grade 7 igcse
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Chapter 4THE ATMOSPHERE14.1 THE ATMOSPHERE4.1.1 .docxchristinemaritza
Chapter 4
THE ATMOSPHERE
1
4.1 THE ATMOSPHERE
4.1.1 INTRODUCTION
The atmosphere, the gaseous layer that surrounds the earth, formed over four billion years ago. During
the evolution of the solid earth, volcanic eruptions released gases into the developing atmosphere. Assuming
the outgasing was similar to that of modern volcanoes, the gases released included: water vapor (H2O),
carbon monoxide (CO), carbon dioxide (CO2), hydrochloric acid (HCl), methane (CH4), ammonia (NH3),
nitrogen (N2) and sulfur gases. The atmosphere was reducing because there was no free oxygen. Most of
the hydrogen and helium that outgassed would have eventually escaped into outer space due to the inability
of the earth's gravity to hold on to their small masses. There may have also been signi�cant contributions
of volatiles from the massive meteoritic bombardments known to have occurred early in the earth's history.
Water vapor in the atmosphere condensed and rained down, eventually forming lakes and oceans. The
oceans provided homes for the earliest organisms which were probably similar to cyanobacteria. Oxygen
was released into the atmosphere by these early organisms, and carbon became sequestered in sedimentary
rocks. This led to our current oxidizing atmosphere, which is mostly comprised of nitrogen (roughly 71
percent) and oxygen (roughly 28 percent). Water vapor, argon and carbon dioxide together comprise a
much smaller fraction (roughly 1 percent). The atmosphere also contains several gases in trace amounts,
such as helium, neon, methane and nitrous oxide. One very important trace gas is ozone, which absorbs
harmful UV radiation from the sun.
4.1.2 ATMOSPHERIC STRUCTURE
The earth's atmosphere extends outward to about 1,000 kilometers where it transitions to interplanetary
space. However, most of the mass of the atmosphere (greater than 99 percent) is located within the �rst
40 kilometers. The sun and the earth are the main sources of radiant energy in the atmosphere. The
sun's radiation spans the infrared, visible and ultraviolet light regions, while the earth's radiation is mostly
infrared.
The vertical temperature pro�le of the atmosphere is variable and depends upon the types of radiation
that a�ect each atmospheric layer. This, in turn, depends upon the chemical composition of that layer
(mostly involving trace gases). Based on these factors, the atmosphere can be divided into four distinct
layers: the troposphere, stratosphere, mesosphere, and thermosphere.
The troposphere is the atmospheric layer closest to the earth's surface. It extends about 8 - 16 kilometers
from the earth's surface. The thickness of the layer varies a few km according to latitude and the season of
the year. It is thicker near the equator and during the summer, and thinner near the poles and during the
1This content is available online at <http://cnx.org/content/m16687/1.2/>.
Available for free at Connexions <http://cnx.org/content/col10548/1.2>
15
16 CHAPTER 4. THE ATMOS ...
this ppt is mainly for the students of grade 7 igcse
go ahead,have a look!
follow for more ppts!
just comment whichever ppt you want next and it will be ready for u!
-proud dsrvian
Chapter 4THE ATMOSPHERE14.1 THE ATMOSPHERE4.1.1 .docxchristinemaritza
Chapter 4
THE ATMOSPHERE
1
4.1 THE ATMOSPHERE
4.1.1 INTRODUCTION
The atmosphere, the gaseous layer that surrounds the earth, formed over four billion years ago. During
the evolution of the solid earth, volcanic eruptions released gases into the developing atmosphere. Assuming
the outgasing was similar to that of modern volcanoes, the gases released included: water vapor (H2O),
carbon monoxide (CO), carbon dioxide (CO2), hydrochloric acid (HCl), methane (CH4), ammonia (NH3),
nitrogen (N2) and sulfur gases. The atmosphere was reducing because there was no free oxygen. Most of
the hydrogen and helium that outgassed would have eventually escaped into outer space due to the inability
of the earth's gravity to hold on to their small masses. There may have also been signi�cant contributions
of volatiles from the massive meteoritic bombardments known to have occurred early in the earth's history.
Water vapor in the atmosphere condensed and rained down, eventually forming lakes and oceans. The
oceans provided homes for the earliest organisms which were probably similar to cyanobacteria. Oxygen
was released into the atmosphere by these early organisms, and carbon became sequestered in sedimentary
rocks. This led to our current oxidizing atmosphere, which is mostly comprised of nitrogen (roughly 71
percent) and oxygen (roughly 28 percent). Water vapor, argon and carbon dioxide together comprise a
much smaller fraction (roughly 1 percent). The atmosphere also contains several gases in trace amounts,
such as helium, neon, methane and nitrous oxide. One very important trace gas is ozone, which absorbs
harmful UV radiation from the sun.
4.1.2 ATMOSPHERIC STRUCTURE
The earth's atmosphere extends outward to about 1,000 kilometers where it transitions to interplanetary
space. However, most of the mass of the atmosphere (greater than 99 percent) is located within the �rst
40 kilometers. The sun and the earth are the main sources of radiant energy in the atmosphere. The
sun's radiation spans the infrared, visible and ultraviolet light regions, while the earth's radiation is mostly
infrared.
The vertical temperature pro�le of the atmosphere is variable and depends upon the types of radiation
that a�ect each atmospheric layer. This, in turn, depends upon the chemical composition of that layer
(mostly involving trace gases). Based on these factors, the atmosphere can be divided into four distinct
layers: the troposphere, stratosphere, mesosphere, and thermosphere.
The troposphere is the atmospheric layer closest to the earth's surface. It extends about 8 - 16 kilometers
from the earth's surface. The thickness of the layer varies a few km according to latitude and the season of
the year. It is thicker near the equator and during the summer, and thinner near the poles and during the
1This content is available online at <http://cnx.org/content/m16687/1.2/>.
Available for free at Connexions <http://cnx.org/content/col10548/1.2>
15
16 CHAPTER 4. THE ATMOS ...
This presentation talks about our atmosphere, its composition, the layers of the atmosphere, effects of EM radiation, EM spectrum, Visible spectrum, factors affecting our atmosphere, terrestrial long wave flux and how earth's radiation release and income gets balanced in brief, the sources from which the information has been taken is mentioned in the end of the presentation.
What are the Layers and Structure of Atmosphere?Tutoroot
Explore Earth's atmospheric layers, from the troposphere to the exosphere. Learn about their unique compositions, temperatures, and roles in weather patterns and climate regulation. The atmosphere is a vital component of our planet, encompassing a complex arrangement of different layers. These layers of the atmosphere play a crucial role in the Earth’s climate, weather patterns, and the overall sustenance of life. Enroll now at Tutoroot.
Atmosphere is the blanket of air that surrounds the earth and the composition of the Atmosphere is 78% nitrogen, 21% oxygen 0.9% argon and 0.1% other gases. Earth has 6 layers of Atmosphere around it to protect us from harmful gases & maintain the suitable temperature for the life on the earth .The layers are Troposphere, Stratosphere, Mesosphere , Thermosphere , Exosphere and Ionosphere.
A brief information about the SCOP protein database used in bioinformatics.
The Structural Classification of Proteins (SCOP) database is a comprehensive and authoritative resource for the structural and evolutionary relationships of proteins. It provides a detailed and curated classification of protein structures, grouping them into families, superfamilies, and folds based on their structural and sequence similarities.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...Ana Luísa Pinho
Functional Magnetic Resonance Imaging (fMRI) provides means to characterize brain activations in response to behavior. However, cognitive neuroscience has been limited to group-level effects referring to the performance of specific tasks. To obtain the functional profile of elementary cognitive mechanisms, the combination of brain responses to many tasks is required. Yet, to date, both structural atlases and parcellation-based activations do not fully account for cognitive function and still present several limitations. Further, they do not adapt overall to individual characteristics. In this talk, I will give an account of deep-behavioral phenotyping strategies, namely data-driven methods in large task-fMRI datasets, to optimize functional brain-data collection and improve inference of effects-of-interest related to mental processes. Key to this approach is the employment of fast multi-functional paradigms rich on features that can be well parametrized and, consequently, facilitate the creation of psycho-physiological constructs to be modelled with imaging data. Particular emphasis will be given to music stimuli when studying high-order cognitive mechanisms, due to their ecological nature and quality to enable complex behavior compounded by discrete entities. I will also discuss how deep-behavioral phenotyping and individualized models applied to neuroimaging data can better account for the subject-specific organization of domain-general cognitive systems in the human brain. Finally, the accumulation of functional brain signatures brings the possibility to clarify relationships among tasks and create a univocal link between brain systems and mental functions through: (1) the development of ontologies proposing an organization of cognitive processes; and (2) brain-network taxonomies describing functional specialization. To this end, tools to improve commensurability in cognitive science are necessary, such as public repositories, ontology-based platforms and automated meta-analysis tools. I will thus discuss some brain-atlasing resources currently under development, and their applicability in cognitive as well as clinical neuroscience.
(May 29th, 2024) Advancements in Intravital Microscopy- Insights for Preclini...Scintica Instrumentation
Intravital microscopy (IVM) is a powerful tool utilized to study cellular behavior over time and space in vivo. Much of our understanding of cell biology has been accomplished using various in vitro and ex vivo methods; however, these studies do not necessarily reflect the natural dynamics of biological processes. Unlike traditional cell culture or fixed tissue imaging, IVM allows for the ultra-fast high-resolution imaging of cellular processes over time and space and were studied in its natural environment. Real-time visualization of biological processes in the context of an intact organism helps maintain physiological relevance and provide insights into the progression of disease, response to treatments or developmental processes.
In this webinar we give an overview of advanced applications of the IVM system in preclinical research. IVIM technology is a provider of all-in-one intravital microscopy systems and solutions optimized for in vivo imaging of live animal models at sub-micron resolution. The system’s unique features and user-friendly software enables researchers to probe fast dynamic biological processes such as immune cell tracking, cell-cell interaction as well as vascularization and tumor metastasis with exceptional detail. This webinar will also give an overview of IVM being utilized in drug development, offering a view into the intricate interaction between drugs/nanoparticles and tissues in vivo and allows for the evaluation of therapeutic intervention in a variety of tissues and organs. This interdisciplinary collaboration continues to drive the advancements of novel therapeutic strategies.
Slide 1: Title Slide
Extrachromosomal Inheritance
Slide 2: Introduction to Extrachromosomal Inheritance
Definition: Extrachromosomal inheritance refers to the transmission of genetic material that is not found within the nucleus.
Key Components: Involves genes located in mitochondria, chloroplasts, and plasmids.
Slide 3: Mitochondrial Inheritance
Mitochondria: Organelles responsible for energy production.
Mitochondrial DNA (mtDNA): Circular DNA molecule found in mitochondria.
Inheritance Pattern: Maternally inherited, meaning it is passed from mothers to all their offspring.
Diseases: Examples include Leber’s hereditary optic neuropathy (LHON) and mitochondrial myopathy.
Slide 4: Chloroplast Inheritance
Chloroplasts: Organelles responsible for photosynthesis in plants.
Chloroplast DNA (cpDNA): Circular DNA molecule found in chloroplasts.
Inheritance Pattern: Often maternally inherited in most plants, but can vary in some species.
Examples: Variegation in plants, where leaf color patterns are determined by chloroplast DNA.
Slide 5: Plasmid Inheritance
Plasmids: Small, circular DNA molecules found in bacteria and some eukaryotes.
Features: Can carry antibiotic resistance genes and can be transferred between cells through processes like conjugation.
Significance: Important in biotechnology for gene cloning and genetic engineering.
Slide 6: Mechanisms of Extrachromosomal Inheritance
Non-Mendelian Patterns: Do not follow Mendel’s laws of inheritance.
Cytoplasmic Segregation: During cell division, organelles like mitochondria and chloroplasts are randomly distributed to daughter cells.
Heteroplasmy: Presence of more than one type of organellar genome within a cell, leading to variation in expression.
Slide 7: Examples of Extrachromosomal Inheritance
Four O’clock Plant (Mirabilis jalapa): Shows variegated leaves due to different cpDNA in leaf cells.
Petite Mutants in Yeast: Result from mutations in mitochondrial DNA affecting respiration.
Slide 8: Importance of Extrachromosomal Inheritance
Evolution: Provides insight into the evolution of eukaryotic cells.
Medicine: Understanding mitochondrial inheritance helps in diagnosing and treating mitochondrial diseases.
Agriculture: Chloroplast inheritance can be used in plant breeding and genetic modification.
Slide 9: Recent Research and Advances
Gene Editing: Techniques like CRISPR-Cas9 are being used to edit mitochondrial and chloroplast DNA.
Therapies: Development of mitochondrial replacement therapy (MRT) for preventing mitochondrial diseases.
Slide 10: Conclusion
Summary: Extrachromosomal inheritance involves the transmission of genetic material outside the nucleus and plays a crucial role in genetics, medicine, and biotechnology.
Future Directions: Continued research and technological advancements hold promise for new treatments and applications.
Slide 11: Questions and Discussion
Invite Audience: Open the floor for any questions or further discussion on the topic.
Professional air quality monitoring systems provide immediate, on-site data for analysis, compliance, and decision-making.
Monitor common gases, weather parameters, particulates.
Cancer cell metabolism: special Reference to Lactate PathwayAADYARAJPANDEY1
Normal Cell Metabolism:
Cellular respiration describes the series of steps that cells use to break down sugar and other chemicals to get the energy we need to function.
Energy is stored in the bonds of glucose and when glucose is broken down, much of that energy is released.
Cell utilize energy in the form of ATP.
The first step of respiration is called glycolysis. In a series of steps, glycolysis breaks glucose into two smaller molecules - a chemical called pyruvate. A small amount of ATP is formed during this process.
Most healthy cells continue the breakdown in a second process, called the Kreb's cycle. The Kreb's cycle allows cells to “burn” the pyruvates made in glycolysis to get more ATP.
The last step in the breakdown of glucose is called oxidative phosphorylation (Ox-Phos).
It takes place in specialized cell structures called mitochondria. This process produces a large amount of ATP. Importantly, cells need oxygen to complete oxidative phosphorylation.
If a cell completes only glycolysis, only 2 molecules of ATP are made per glucose. However, if the cell completes the entire respiration process (glycolysis - Kreb's - oxidative phosphorylation), about 36 molecules of ATP are created, giving it much more energy to use.
IN CANCER CELL:
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
introduction to WARBERG PHENOMENA:
WARBURG EFFECT Usually, cancer cells are highly glycolytic (glucose addiction) and take up more glucose than do normal cells from outside.
Otto Heinrich Warburg (; 8 October 1883 – 1 August 1970) In 1931 was awarded the Nobel Prize in Physiology for his "discovery of the nature and mode of action of the respiratory enzyme.
WARNBURG EFFECT : cancer cells under aerobic (well-oxygenated) conditions to metabolize glucose to lactate (aerobic glycolysis) is known as the Warburg effect. Warburg made the observation that tumor slices consume glucose and secrete lactate at a higher rate than normal tissues.
The ASGCT Annual Meeting was packed with exciting progress in the field advan...
Atmospheric layers of earth
1. Atmospheric Layers Of Earth
Presented By
Mandar Mahindrakar
Department Of Geology
Govt.Institute Of Science
Aurangabad
2. Introduction
The atmosphere is a mixture of different gases, particles and aerosols
collectively known as air which envelops the Earth.
The atmosphere protects us by filtering out deadly cosmic rays,
powerful ultraviolet (UV) radiation from the Sun, and even meteors on
collision course with Earth.
99% of the mass of the atmosphere lies below about 25 to 30km
altitude, whilst 50% is concentrated in the lowest 5km (less than the
height of Mount Everest).
The two most abundant gases are nitrogen (78% by volume) and
oxygen (21% by volume), and together they make up over 99% of the
lower atmosphere.
In addition to nitrogen and oxygen, air contains a number of trace gases,
including the noble gases, greenhouse gases and ozone.
significant variations in temperature and pressure with altitude, which
define a number of atmospheric layers, including the troposphere,
stratosphere, and mesosphere. Beyond about 50 miles (80 kilometers)
altitude, the air is very very thin indeed
Layers used to describe the outer reaches of the atmosphere include
the thermosphere, the ionosphere, the exosphere and the
magnetosphere. Another well-known layer is the ozone layer, residing in
the stratosphere and protecting life below from the harmful effects of
5. Troposphere
The lowest layer of the
atmosphere is called the
troposphere. It ranges in
thickness from 8km at the poles
to 16km over the equator
The troposphere is denser
than the layers of the
atmosphere above it (because
of the weight compressing it),
and it contains up to 75% of the
mass of the atmosphere.
The troposphere is the layer
where most of the world's
weather takes place. Since
temperature decreases with
altitude in the troposphere
Nearly all atmospheric water
vapor or moisture ,clouds is
found in the troposphere.
6. Stratosphere
The stratosphere is the second
major layer of the atmosphere. It
lies above the troposphere and is
separated from it by the
tropopause
It occupies the region of
atmosphere from about 12 to 50
km
The stratosphere defines a layer
in which temperatures rises with
increasing altitude
This rise in temperature is
caused by the absorption of
ultraviolet (UV) radiation from the
Sun by the ozone layer
Consequently the stratosphere is
almost completely free of clouds or
other forms of weather,provides
some advantages for long-distant
flight because it is above stormy
weather and has strong, steady,
horizontal winds.
7. Mesosphere
The mesosphere (literally
middle sphere) is the third
highest layer in our atmosphere
Occupying the region 50 km to
80 km above the surface of the
Earth
Temperatures in the
mesosphere drop with
increasing altitude to about -
100°C. The mesosphere is the
coldest of the atmospheric
layers.
In fact it is colder then
Antarctica's lowest recorded
temperature. It is cold enough to
freeze water vapor into ice
clouds
The mesosphere is also the
layer in which a lot of meteors
burn up while entering the
Earth's atmosphere. From the
8. Thermosphere
The thermosphere
(literally "heat sphere") is
the outer layer of the
atmosphere
the thermosphere, from
80 to 550 km above the
Earth's surface
Within the thermosphere
temperatures rise
continually to well beyond
1000°C.
The few molecules that
are present in the
thermosphere receive
extraordinary amounts of
energy from the Sun,
causing the layer to warm
to such high temperatures
9. Ionosphere
The ionosphere is a layer of ionized air in the atmosphere extending
from almost 80 km above the Earth's surface altitudes of 600 km and
more
Technically, the ionosphere is not another atmospheric layer. It
occupies the same region of the upper atmosphere as the
thermosphere.
In this region of the atmosphere the Sun's energy is so strong that it
breaks apart molecules and atoms of air, leaving ions (atoms with
missing electrons) and free-floating electrons.
The ionosphere is the region of the atmosphere where the auroras
occur.
Ionization of air molecules in the ionosphere is produced by
ultraviolet radiation from the Sun, and to a lesser extent by high-energy
particles from the Sun and from cosmic rays.
The large number of free electrons in the ionosphere allows the
propagation of electromagnetic waves.
Radio signals - a form of electromagnetic radiation - can be
"bounced" off the ionosphere allowing radio communication over long
distances.
10.
11. Exosphere
The exosphere is the
highest layer of the
atmosphere.
Together with the
ionosphere, it makes up the
thermosphere.
The exosphere extends to
10,000 km above the
Earth's surface. This is the
upper limit of our
atmosphere
In this region of the
atmosphere, hydrogen and
helium are the prime
components and are only
present at extremely low
densities.
This is the area where
many satellites orbit the
Earth.
12. Magnetosphere
The magnetosphere extends into the vacuum of space from approximately
80 to 60,000 kilometers on the side toward the Sun, and trails out more than
300,000 kilometers away from the Sun.
Earth's magnetic field protects us from the harmful effects of the solar wind.
The Earth is like a huge magnet, and its magnetic influence extends far into
space.
It is made up of positively charged protons and negatively charged electrons.
The solar wind would singe our atmosphere if not for the Earth's magnetic
field.
Many of the remaining particles that are given off by the Sun are
concentrated into belts or layers called the Van Allen radiation belts.
13. Coriolis Force
The Coriolis force is a force which acts upon any moving body in an
independently rotating system.
The most well known application of the Coriolis force is for the
movement or flow of air across the Earth.
The effect is named after the French physicist Gaspard de Coriolis
(1792-1843), who first analyzed the phenomenon mathematically
Moving air undergoes an apparent deflection from its path, as seen
by an observer on the Earth. This apparent deflection is the result of
the Coriolis force
Therefore, slowly blowing winds will be deflected only a small
amount, while stronger winds will be deflected more.
Likewise, winds blowing closer to the poles will be deflected more
than winds at the same speed closer to the equator.
The Coriolis force only acts on large objects like air masses moving
considerable distances of Small objects,
for example ships at sea, are too small to experience significant
deflections in direction due to the Coriolis Force.
14.
15. Ozone Layer
The ozone layer is a layer of ozone particles scattered between 19 and 30
kilometers (12 to 30 miles) up in the Earth's atmosphere, in a region called the
stratosphere.
The concentration of ozone in the ozone layer is usually under 10 parts
ozone per million. Without the ozone layer, ultraviolet (UV) radiation from the
Sun would not be stopped from entering the Earth's atmosphere and arriving
at the surface, causing damage to most living species.
Ozone is created in the stratosphere when highly energetic solar radiation
strikes molecules of oxygen (O2) and causes the two oxygen atoms to split
apart.
If a freed atom bumps into another O2, it joins up, forming ozone (O3). This
process known as photolysis
In an unpolluted atmosphere there is a balance between the amount of
ozone being produced and the amount of ozone being destroyed. As a result,
the total amount of ozone in the stratosphere remains relatively constant
Ozone's unique physical properties allow the ozone layer to act as our
planet's sunscreen, providing an invisible filter to help protect all life forms from
the Sun's damaging ultraviolet (UV) rays.
Most incoming UV radiation is absorbed by ozone and prevented from
reaching the Earth's surface. Without the protective effect of ozone, life on
Earth would not have evolved in the way it has.
16.
17. Jet Streams
The jet stream is a current of fast moving
air found in the upper levels of the
troposphere which blow from west to east
due to the Earth's rotation.
This rapid current is typically thousands of
kilometers long, a few hundred kilometers
wide, and only a few kilometers thick.
Jet streams are usually found somewhere
between 10-15 km (6-9 miles) above the
Earth's surface.
Wind speed within jet streams can range
from between 50 -and 300 miles per hour.
The position of the jet stream denotes the
location of the strongest temperature
contrasts between different latitudes on the
Earth surface. Consequently, the strongest
jet streams usually occur during the winter
months,
when large temperature differences exist
between low and high latitudes. There are
two main jet streams - the subtropical jet
stream at about 30 degrees latitude and the