The early Earth had two primordial atmospheres composed of hydrogen and helium that escaped due to the planet's weak gravity, and a second composed of gases like water vapor, carbon dioxide, and nitrogen released by volcanoes. Around 2 billion years ago, the rise of oxygen-producing photosynthetic bacteria led to the establishment of a third atmosphere with near-modern levels of oxygen. Decreases in carbon dioxide due to photosynthesis and weathering eventually allowed glaciation until volcanic outgassing of carbon dioxide warmed the planet again.
En esta parte se desarrrolla que es una atmosfera y su estructura, la temperatura de un planeta,el efecto invernadero con respecto a la temperatura y cambio climatico global.
The universe began about 14.4 billion years ago.
The Big Bang Theory states that, in the beginning, the universe was all in one place.
To know more, see the presentation.
En esta parte se desarrrolla que es una atmosfera y su estructura, la temperatura de un planeta,el efecto invernadero con respecto a la temperatura y cambio climatico global.
The universe began about 14.4 billion years ago.
The Big Bang Theory states that, in the beginning, the universe was all in one place.
To know more, see the presentation.
Earth’s atmosphere is slightly warmer than what it should be due to direct solar heating because of a mild case of greenhouse effect…
The ground is heated by visible and (some) infrared light from the Sun.
The heated surface emits infrared light.
The majority of Earth’s atmosphere (N2 and O2) are not good greenhouse gas.
The small amount of greenhouse gases (H2O, CO2) traps (absorb and re-emit) the infrared radiation, increasing the temperature of the atmosphere…
In this presentation, I focused on the geomorphological aspect of earthquake which means tectonic plates. Additionally, we also included the origin of the Universe and tectonic plates. And also the Nepal and Taiwan earthquakes of 2015 was also described here in perspective with tectonic plates.
Earth’s atmosphere is slightly warmer than what it should be due to direct solar heating because of a mild case of greenhouse effect…
The ground is heated by visible and (some) infrared light from the Sun.
The heated surface emits infrared light.
The majority of Earth’s atmosphere (N2 and O2) are not good greenhouse gas.
The small amount of greenhouse gases (H2O, CO2) traps (absorb and re-emit) the infrared radiation, increasing the temperature of the atmosphere…
In this presentation, I focused on the geomorphological aspect of earthquake which means tectonic plates. Additionally, we also included the origin of the Universe and tectonic plates. And also the Nepal and Taiwan earthquakes of 2015 was also described here in perspective with tectonic plates.
What is greenhouse gasses and how many gasses are there to affect the Earth.moosaasad1975
What are greenhouse gasses how they affect the earth and its environment what is the future of the environment and earth how the weather and the climate effects.
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.
This pdf is about the Schizophrenia.
For more details visit on YouTube; @SELF-EXPLANATORY;
https://www.youtube.com/channel/UCAiarMZDNhe1A3Rnpr_WkzA/videos
Thanks...!
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
This presentation explores a brief idea about the structural and functional attributes of nucleotides, the structure and function of genetic materials along with the impact of UV rays and pH upon them.
Professional air quality monitoring systems provide immediate, on-site data for analysis, compliance, and decision-making.
Monitor common gases, weather parameters, particulates.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Comparing Evolved Extractive Text Summary Scores of Bidirectional Encoder Rep...University of Maribor
Slides from:
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Track: Artificial Intelligence
https://www.etran.rs/2024/en/home-english/
Comparative structure of adrenal gland in vertebrates
earth.ppt
1. The Origin of the Earth’s
Atmosphere
Still Many Uncertainties ….
2. About 4.5 billion
years ago, Earth
formed out of
nebula of gases and
dust that were to
become the solar
system
Small objects--called
planetoids-- accreted or
combined together to build
larger objects…such as planets
3. The First Atmosphere
• The early atmosphere would have been similar to
the Sun--mainly hydrogen and helium, but this
atmosphere was lost quickly for two reasons:
– (1) The gravity of the modest size earth was not strong
enough to prevent such light gases from escaping to
space. Particularly since the early earth was hot!
– (2) It appears that around 30 million years after the
earth’s formation, it was struck by a large object…the
size of Mars. The result: the origin of the moon and
loss of earth’s early H, He atmosphere.
6. Earth as Hell
• The surface of the earth during this period
was extremely hot with numerous volcanoes
• The earth was under near constant
bombardment by objects of varying sizes
• Slowly, the earth started to cool down and
the second atmosphere began to form.
7.
8.
9. Earth’s Second Atmosphere
• A new atmosphere was established by the
outgasing of volcanoes…the mixture of gases was
probably similar to those of today’s volcanoes:
• H20 vapor (roughly 80%)
• CO2 (roughly 10%)
• N2 (few percent)
• Small amounts of CO, HCL, HS (Hydrogen
Sulfide), SO2, CH4 (Methane), Ammonia (NH3),
and other trace gases.
10.
11. Earth’s Second Atmosphere
• Virtually no oxygen in that second atmosphere.
• Thus, no ozone layer, so ultraviolet radiation
flooded the earth’s surface.
• With a huge influx of water vapor and the cooling
of the planet, clouds and earth’s oceans formed.
• At that time the sun was about 30% weaker than
today…why didn’t the earth freeze over?
• The apparent reason: so much CO2 so there was a
very strong greenhouse effect.
12. The Rise of Oxygen and the Third
Atmosphere
• In the first two billion years of the planet’s evolution,
the atmosphere acquired a small amount of oxygen,
probably by the splitting of water (H20) molecules by
solar radiation.
• The evidence of this oxygen is suggested by minor
rust in some early rocks.
• The oxygen also led to the establishment of an ozone
layer that reduced UV radiation at the surface.
• With the rise of photosynthetic bacteria
(cyanobacteria) and early plants, oxygen levels began
to rise rapidly as did indications of rust in rocks
• Between 2.5 billion years ago to about 500 bya, 02
rose to near current levels.
13.
14.
15. The Third Atmosphere
• While O2 was increasing, CO2 decreased
due to several reasons:
• (1) In photosynthesis CO2 is used to
produce organic matter, some of which is
lost to the system (e.g., drops to the bottom
of the ocean or is buried)
• (2) chemical weathering, which removes
CO2
16. Chemical Weathering
• H20 + CO2 --> H2CO3 carbonic acid
• CaSiO3 + H2CO3 --> CaCO3 + SiO2 + H20
Silicate Rock Carbonate
• At first this happened without life, but the process was
sped up tremendously by living organisms
• Marine organisms would incorporate carbonate into their
shells, which would fall to the ocean bottom when they
died---thus, removing them from the system for a long
time.
• The bottom line…CO2 was being removed from the
system.
17. More Changes
• Sulfur compounds were taken out of the
atmosphere as acid rain and were deposited
on the ground as sulfates.
• N2 gas increased slowly but progressively
since it was relatively inert.
• Current composition of the atmosphere was
established approximately a billion years
ago.
18. A Problem
• With lower CO2 levels the earth became more
susceptable to ice ages when solar radiation
decreases due to orbital variations,
• It appears that around 750-550 million years ago
the earth cooled down and became nearly entirely
glaciated.
• Note: one can get into a feedback with snow
reflecting solar radiation, producing cooler
temperatures and more snow, leading to less
radiation, etc.
19.
20. How Did We Get UnFrozen?
• Volcanoes were still putting CO2 into the
atmosphere
• Weathering was greatly reduced…since
little liquid water.
• So CO2 increased until the greenhouse
effect was so large the earth warmed up.
• Once warming started it would have
happened very rapidly.
21. The Last 500 million Years
• The climate has not been constant, with
warm periods interrupted by ice ages.
• Much of the variability forced by changing
solar radiation due to periodic changes in
the earth’s orbital characteristics and tilt
(Milankovitch cycles) and major volcanic
eruptions (putting out massive CO2 that
caused warming.
22. More Snowball Earths?
• Less chance now
• Sun is getting progressively stronger
• Human’s can now stop it (increasing
greenhouse gases)
33. Mars
Surface Pressure: ~6 hPa
Mostly (96%)CO2, small
amounts of
H20 vapor
CO2 and H20 polar ice
Lots of dust
Average T: -80F but warmer
near equator in summer
(70F)
43. Earth’s Atmosphere Is a Thin Veneer
Earth’s radius is about 6400 km
(3840 miles)
Nearly all of the atmosphere is
contained in the layer from the
surface to 100 km. Habitable
atmosphere only the first 5 km.
So the habitable atmosphere is
only 5/6400 km….00078 ….or
1/1280th of the distance to the
earth’s center. Much thinner than
the peel on an orange.