The document summarizes the formation and evolution of the Earth. It describes how the Earth formed from a large gas cloud following the Big Bang around 14 billion years ago. As the cloud contracted under gravity, it began to rotate and the heavier elements condensed at the center to form the Sun, while the lighter elements formed the planets. The currently accepted theory is that the Solar System formed from a rotating disk of dust and gas leftover from the formation of the Sun. Over time, the planets accreted and the Earth developed differentiated layers, including a molten iron core. Bombardment from asteroids and comets continued for over 500 million years. The Moon formed from debris ejected during a giant impact with Earth around 4.5 billion
Origin of Earth, Big Bang theory, Nebular hypothesis, Internal heating of earth, formation of Earth's crust and inner structure, evolution of continents, oceans and atmosphere, continental drift theory, origin of life, Geological Time Scale.
Origin of Earth, Big Bang theory, Nebular hypothesis, Internal heating of earth, formation of Earth's crust and inner structure, evolution of continents, oceans and atmosphere, continental drift theory, origin of life, Geological Time Scale.
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.
The presentation aiding the lecture Structure of Earth and its Composition for the course CE 8392 Engineering Geology handled by Prof. Rathnavel Pon for Akshaya College of Engineering and Technology, Coimbatore
Origin and Abundance of elements in the Solar system and in the Earth and its...AkshayRaut51
Definition of Elements and atom
Origin of Universe
Theories of origin of Solar system and Earth
Chemical Composition of Planets
Chemical Composition of Earth
Chemical composition of Meteorites
Abundance of Elements
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.
The presentation aiding the lecture Structure of Earth and its Composition for the course CE 8392 Engineering Geology handled by Prof. Rathnavel Pon for Akshaya College of Engineering and Technology, Coimbatore
Origin and Abundance of elements in the Solar system and in the Earth and its...AkshayRaut51
Definition of Elements and atom
Origin of Universe
Theories of origin of Solar system and Earth
Chemical Composition of Planets
Chemical Composition of Earth
Chemical composition of Meteorites
Abundance of Elements
Earth, along with the other planets, is believed to have been born 4.5 billion years ago as a solidified cloud of dust and gases left over from the creation of the Sun.
A Strategic Approach: GenAI in EducationPeter Windle
Artificial Intelligence (AI) technologies such as Generative AI, Image Generators and Large Language Models have had a dramatic impact on teaching, learning and assessment over the past 18 months. The most immediate threat AI posed was to Academic Integrity with Higher Education Institutes (HEIs) focusing their efforts on combating the use of GenAI in assessment. Guidelines were developed for staff and students, policies put in place too. Innovative educators have forged paths in the use of Generative AI for teaching, learning and assessments leading to pockets of transformation springing up across HEIs, often with little or no top-down guidance, support or direction.
This Gasta posits a strategic approach to integrating AI into HEIs to prepare staff, students and the curriculum for an evolving world and workplace. We will highlight the advantages of working with these technologies beyond the realm of teaching, learning and assessment by considering prompt engineering skills, industry impact, curriculum changes, and the need for staff upskilling. In contrast, not engaging strategically with Generative AI poses risks, including falling behind peers, missed opportunities and failing to ensure our graduates remain employable. The rapid evolution of AI technologies necessitates a proactive and strategic approach if we are to remain relevant.
The French Revolution, which began in 1789, was a period of radical social and political upheaval in France. It marked the decline of absolute monarchies, the rise of secular and democratic republics, and the eventual rise of Napoleon Bonaparte. This revolutionary period is crucial in understanding the transition from feudalism to modernity in Europe.
For more information, visit-www.vavaclasses.com
Operation “Blue Star” is the only event in the history of Independent India where the state went into war with its own people. Even after about 40 years it is not clear if it was culmination of states anger over people of the region, a political game of power or start of dictatorial chapter in the democratic setup.
The people of Punjab felt alienated from main stream due to denial of their just demands during a long democratic struggle since independence. As it happen all over the word, it led to militant struggle with great loss of lives of military, police and civilian personnel. Killing of Indira Gandhi and massacre of innocent Sikhs in Delhi and other India cities was also associated with this movement.
2024.06.01 Introducing a competency framework for languag learning materials ...Sandy Millin
http://sandymillin.wordpress.com/iateflwebinar2024
Published classroom materials form the basis of syllabuses, drive teacher professional development, and have a potentially huge influence on learners, teachers and education systems. All teachers also create their own materials, whether a few sentences on a blackboard, a highly-structured fully-realised online course, or anything in between. Despite this, the knowledge and skills needed to create effective language learning materials are rarely part of teacher training, and are mostly learnt by trial and error.
Knowledge and skills frameworks, generally called competency frameworks, for ELT teachers, trainers and managers have existed for a few years now. However, until I created one for my MA dissertation, there wasn’t one drawing together what we need to know and do to be able to effectively produce language learning materials.
This webinar will introduce you to my framework, highlighting the key competencies I identified from my research. It will also show how anybody involved in language teaching (any language, not just English!), teacher training, managing schools or developing language learning materials can benefit from using the framework.
How to Make a Field invisible in Odoo 17Celine George
It is possible to hide or invisible some fields in odoo. Commonly using “invisible” attribute in the field definition to invisible the fields. This slide will show how to make a field invisible in odoo 17.
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Francesca Gottschalk - How can education support child empowerment.pptxEduSkills OECD
Francesca Gottschalk from the OECD’s Centre for Educational Research and Innovation presents at the Ask an Expert Webinar: How can education support child empowerment?
The Roman Empire A Historical Colossus.pdfkaushalkr1407
The Roman Empire, a vast and enduring power, stands as one of history's most remarkable civilizations, leaving an indelible imprint on the world. It emerged from the Roman Republic, transitioning into an imperial powerhouse under the leadership of Augustus Caesar in 27 BCE. This transformation marked the beginning of an era defined by unprecedented territorial expansion, architectural marvels, and profound cultural influence.
The empire's roots lie in the city of Rome, founded, according to legend, by Romulus in 753 BCE. Over centuries, Rome evolved from a small settlement to a formidable republic, characterized by a complex political system with elected officials and checks on power. However, internal strife, class conflicts, and military ambitions paved the way for the end of the Republic. Julius Caesar’s dictatorship and subsequent assassination in 44 BCE created a power vacuum, leading to a civil war. Octavian, later Augustus, emerged victorious, heralding the Roman Empire’s birth.
Under Augustus, the empire experienced the Pax Romana, a 200-year period of relative peace and stability. Augustus reformed the military, established efficient administrative systems, and initiated grand construction projects. The empire's borders expanded, encompassing territories from Britain to Egypt and from Spain to the Euphrates. Roman legions, renowned for their discipline and engineering prowess, secured and maintained these vast territories, building roads, fortifications, and cities that facilitated control and integration.
The Roman Empire’s society was hierarchical, with a rigid class system. At the top were the patricians, wealthy elites who held significant political power. Below them were the plebeians, free citizens with limited political influence, and the vast numbers of slaves who formed the backbone of the economy. The family unit was central, governed by the paterfamilias, the male head who held absolute authority.
Culturally, the Romans were eclectic, absorbing and adapting elements from the civilizations they encountered, particularly the Greeks. Roman art, literature, and philosophy reflected this synthesis, creating a rich cultural tapestry. Latin, the Roman language, became the lingua franca of the Western world, influencing numerous modern languages.
Roman architecture and engineering achievements were monumental. They perfected the arch, vault, and dome, constructing enduring structures like the Colosseum, Pantheon, and aqueducts. These engineering marvels not only showcased Roman ingenuity but also served practical purposes, from public entertainment to water supply.
Introduction to AI for Nonprofits with Tapp NetworkTechSoup
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2. Origin of the Universe
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
All of its matter and
energy were squished
into an infinitely small
point, a singularity
Then it exploded
3. Origin of the Universe
The tremendous
amount of material
blown out by the
explosion eventually
formed the stars and
galaxies
After about 10 billion
years, our solar system
began to form
4. We know how the Earth and Solar System are today
and this allows us to work backwards and determine
how the Earth and Solar System were formed
Plus we can out into the universe for clues on how
stars and planets are currently being formed
Birth of the Solar System
5. In cosmogony, the Nebular Hypothesis is the
currently accepted argument about how a Solar
System can form
The Nebular Hypothesis
6. We have now discovered over two hundred planets
orbiting other stars
The processes that created our solar system have
also created an uncountable number of other solar
systems
Other Solar Systems
7. A large gas cloud (nebula) begins to condense
Most of the mass is in the center, there is
turbulence in the outer parts
The Nebular Hypothesis
8. The turbulent
eddies collect
matter measuring
meters across
Small chunks
grow and collide,
eventually
becoming large
aggregates of gas
and solid chunks
The Nebular Hypothesis
9. Pictures from the Hubble Space Telescope show
newborn stars emerging from dense, compact pockets
of interstellar gas called evaporating gaseous globules
The Nebular Hypothesis
10. Gravitational attraction causes the mass of gas
and dust to slowly contract and it begins to rotate
The dust and matter slowly falls towards the
center
The Nebular Hypothesis
12. The multi-colored area shows a dust disk
surrounding a newborn star
The red-orange area at the center represents the
brightest region, which contains the young star
It is surrounded by the cooler, dusty disk, which
appears as yellow, green and blue
The diameter of the disk is about 20 times larger
than our entire solar system
False Color Image of Protostar
13. After sufficient mass and density was achieved in
the Sun, the temperature rose to one million °C,
resulting in thermonuclear fusion.
H atom + H atom = He atom + energy
The Sun
15. Gravitational forces allow the inner planets to
accrue and compact solid matter (including light
and heavy atoms)
Solar radiation blew gases (primarily hydrogen,
helium) away from inner planets
These gases were collected and condensed into the
gas giants (Jupiter, Saturn, Uranus, Neptune)
Beyond Neptune, ice and frozen gases form Pluto,
Sedna and the Kuiper Belt Objects
Left-over debris form comets and asteroids
Protoplanets
18. Fig. 1.9
Venus, Earth and Mars
These maps are color coded to display different
elevations on the surface of each planet
19. Earth is ~ 4,570,000,000 years old
The Age of the Earth
Meteorites give us access to debris left over
from the formation of the solar system
We can date meteorites using radioactive
isotopes and their decay products
21. Bombardment From Space
For the first half billion years of its existence, the
surface of the Earth was repeatedly pulverized by
asteroids and comets of all sizes
One of these collisions formed the Moon
22. Formation of the Moon
The Giant Impact
Hypothesis predicts
that around 50 million
years after the initial
creation of Earth, a
planet about the size of
Mars collided with Earth
This idea was first
proposed about 30
years ago, but it took
calculations by modern
high-speed computers
to prove the feasibility
23. Formation of the Moon
This collision had to be very spectacular!
A considerable amount of material was blown off
into space, but most fell back onto the Earth
24. Formation of the Moon
Part of the material from the collision remained
in orbit around the Earth
By the process collision and accretion, this
orbiting material coalesced into the Moon
The early Moon orbited very close to the Earth
25. The Early Earth Heats Up
1. Collisions (Transfer of
kinetic energy into
heat)
2. Compression
3. Radioactivity of
elements (e.g. uranium,
potassium, or thorium)
Three major factors that caused heating and melting
in the early Earth’s interior:
26. The Core
About 100 million years after initial accretion,
temperatures at depths of 400 to 800 km below the
Earth’s surface reach the melting point of iron
In a process called global
chemical differential, the
heavier elements, including
the melted iron, began to
sink down into the core of
the Earth, while the lighter
elements such as oxygen
and silica floated up towards
the surface
27. Global Chemical Differentiation
This global chemical differential was completed by
about 4.3 billion years ago, and the Earth had
developed a inner and outer core, a mantle and crust
28. Chemical Composition of Earth
Whole Earth:
Fe+O+Si+Mg = 93%
Crust:
Si+O+Al = 82%
Each of the major layers has a distinctive
chemical composition, with the crust being
quite different from the Earth as a whole
29. Lithosphere: strong, rocky outer shell of the solid
Earth including all the crust and the upper part of
the mantle to a depth of ~100 km (forms the
plates)
Asthenosphere: weak,ductile layer of the mantle
beneath the lithosphere; deforms to
accommodate the motions of the overlying plates
Deep Mantle: mantle beneath the asthenosphere
(~400 to 2900 km in depth)
Outer core: liquid shell composed of mostly iron
Inner core: innermost sphere composed primarily
of solid iron
Chemical Composition of Earth
30. Continents: Formed from solidified magma that
floated up from the Mantle
Chemical Composition of Earth
Oceans and Atmosphere:
Fluid and gaseous outer
layers believed to have
been created by out-
gassing of gases and
fluids from volcanic
eruptions (in a process
called volatile transfer)
31. The Evolving Atmosphere
Right after its creation, the Earth is thought to have
had a thin atmosphere composed primarily of
helium (He) and hydrogen (H) gases
The Earths gravity
could not hold these
light gases and they
easily escaped into
outer space
Today, H and He are
very rare in our
atmosphere
32. The Evolving Atmosphere
For the next several hundred million years,
volcanic out-gassing began to create a thicker
atmosphere composed of a wide variety of gases
The gases that were released were probably similar
to those created by modern volcanic eruptions
33. These would include:
Water vapor (H2O)
Sulfur dioxide (SO2)
Hydrogen sulfide (H2S)
Carbon dioxide (CO2)
Carbon Monoxide (CO)
Ammonia (NH3)
Methane (CH4)
The Evolving Atmosphere
Note that oxygen (O2) gas is not created by
volcanic eruptions
34. It is hypothesized that water vapor escaping from
the interior of the Earth via countless volcanic
eruptions created the oceans (this took hundreds
of millions of years)
Creating the Oceans
35. Astronomers also
hypothesize that
comets impacting the
Earth were a major
source of water that
contributed to creation
of the oceans
Remember, that
comets are best
described as “dirty ice
balls”
Creating the Oceans
36. Creating the Oceans
The earliest evidence of surface water on
Earth dates back about 3.8 billion years
37. A billion Year Old Earth
By 3.5 billion years ago, when the Earth was a
billion years old, it had a thick atmosphere
composed of CO2, methane, water vapor and
other volcanic gases
By human standards
this early atmosphere
was very poisonous
It contained almost no
oxygen
Remember, today our
atmosphere is 21%
oxygen
38. A billion Year Old Earth
By 3.5 billion years ago, the Earth also had
extensive oceans and seas of salt water, which
contained many dissolved elements, such as
iron
39. A billion Year Old Earth
But most important, by 3.5 billion years
ago, there was life on Earth
40. The Continents
By 2.5 billion years ago, the
continents had been formed
The density of the continental
crust (2.8 gr/cm3) is lighter
that the crust found on ocean
bottoms (3.2 gr/cm3), so the
continents rise above the
ocean floor
A question that remains
unanswered is, when did
plate tectonics start?