The Good Shepherd School of Imelda, Inc.

RIVERSIDE, IMELDA, ZAMBOANGA SIBUGAYSEC. REG. #G19700393

GOVERNMENT PERMIT No. 37 S. 2015 (PRESCHOOL TO COMPLETE ELEMENTARY)
GOVERNMENT RECOGNITION (R-IX) NO. 002, S. 2008 (COMPLETE SECONDARY COURSE)

LESSON PLAN
Name of Teacher Christy P. Betita Subject SCIENCE
Grade Level 10 Time Allotment
Time Schedule 1:00pm-2:00pm TTH Time Frame
Quarter 3rd Evaluation Items

TOPIC
UNIT STANDARD CONTENT STANDARD
The learners demonstrate understanding the formation of the universe and the
solar system 2. the subsystems (geosphere, hydrosphere, atmosphere, and
biosphere) that make up the Earth 3. the Earth’s internal structure
PERFORMANCE STANDARD
The learners should be able to Conduct a survey to assess the possible geologic
hazards that your community may experience. (Note: Select this performance
standard if your school is in an area near faultlines, volcanoes, and steep slopes.)
2. Conduct a survey or design a study to assess the possible hydrometeorological
hazards that your community may experience. (Note: Select this performance
standard if your school is in an area that is frequently hit by tropical cyclones and
is usually flooded.)
PRIOR Directions:
KNOWLEDGE
A. Reviewing previous
lesson or presenting the
new lesson
ESSENTIAL
QUESTIONS
B. Establishing a purpose
of the lesson

ESSENTIAL
UNDERSTANDING

OBJECTIVES
VALUES
INTEGRATION
RESOURCES Government of the Philippines, Department of Education. 2015. Grade 10
Learner’s Material. Manila.

LESSON PROPER
STAGES ACTIVITIES
Exploration Time Allotment: Day: Tuesday
(EXPLORE) Directions: Look for the name of devices hidden in the puzzle below. The
C. Presenting
examples/instan
ces of the new
lesson

Explanation Time Allotment: 1 hour Day: Tuesday

(FIRM UP) 1. The Big Bang Theory
D. Discussing new  Overview: This is the most widely accepted theory, suggesting that the universe
concepts and began as a singularity approximately 13.8 billion years ago. It rapidly expanded and
practicing new continues to expand today.
skills  Evidence:
 o Cosmic Microwave Background Radiation: Discovered in 1965, this is the
afterglow of the initial explosion.
o Redshift of Galaxies: Observations by Edwin Hubble showed that galaxies
are moving away from each other, suggesting the universe is expanding.
o Abundance of Light Elements: The proportions of hydrogen, helium, and
lithium observed in the universe are consistent with predictions from the Big
Bang nucleosynthesis.
2. Steady State Theory
 Overview: Proposed in 1948 by Fred Hoyle, Thomas Gold, and Hermann Bondi, this
theory suggests that the universe has no beginning or end and maintains a constant
average density. New matter is continuously created to form new stars and galaxies at
the same rate as old ones become unobservable.
 Evidence: This theory has fallen out of favor because it does not explain the observed
cosmic microwave background radiation and the redshift of galaxies.
3. Oscillating Universe Theory
 Overview: This theory posits that the universe undergoes endless cycles of Big
Bangs and Big Crunches. After each Big Bang, the universe expands, eventually
slows down, and then contracts back into a singularity, only to expand again.
 Evidence: While intriguing, this theory lacks direct observational support and faces
challenges from the current understanding of cosmic expansion.
4. Inflationary Universe Theory
 Overview: A modification of the Big Bang Theory, proposed by Alan Guth in 1981,
which includes a brief period of rapid exponential expansion (inflation) in the first
fraction of a second after the Big Bang.
 Evidence:
o Flatness Problem: Inflation explains why the universe appears flat.
o Horizon Problem: Inflation accounts for the uniform temperature of the
cosmic microwave background radiation.
o Magnetic Monopole Problem: Inflation predicts the scarcity of magnetic
monopoles.
5. Multiverse Theory
 Overview: This theory suggests that our universe is one of many universes that exist.
These multiple universes together constitute the multiverse. Each universe may have
different physical laws and constants.
 Evidence: Largely theoretical and speculative, as direct evidence is challenging to
obtain. Some interpretations of quantum mechanics and string theory suggest the
possibility of a multiverse.
6. Ekpyrotic Theory
 Overview: Proposed as an alternative to inflation, this theory suggests that the
universe was created from the collision of two three-dimensional worlds (branes) in a
higher-dimensional space.
 Evidence: This theory is still under development and lacks the extensive
observational support that the Big Bang Theory has.
7. Plasma Cosmology
 Overview: This theory emphasizes the role of electromagnetic forces in shaping the
universe, suggesting that the dynamics of ionized gases (plasma) play a key role in
cosmic evolution.
 Evidence: Lacks support from the majority of the scientific community due to
insufficient explanatory power compared to the Big Bang Theory.

Each of these theories offers a different perspective on the origin and evolution of the
universe, with the Big Bang Theory being the most widely supported due to its strong
alignment with observational data.

Describe the different hypotheses explaining the origin of the solar system.
There are several hypotheses that have been proposed to explain the origin of the solar
system. Here are the most prominent ones:
1. Nebular Hypothesis
 Overview: Proposed by Immanuel Kant in 1755 and later refined by Pierre-Simon
Laplace, this hypothesis suggests that the solar system formed from a large cloud of
gas and dust, called a nebula.
 Process:
 o The nebula began to collapse under its own gravity.
o As it collapsed, it spun faster and flattened into a disk.
o Most of the material was pulled toward the center, forming the Sun.
o The remaining material in the disk coalesced to form the planets, moons,
asteroids, and comets.
 Evidence:
o Observations of protoplanetary disks around other stars.
o The flattened, disk-like shape of the solar system.
o The chemical composition and distribution of planets and other solar system
bodies.
2. Planetesimal Hypothesis
 Overview: Proposed by Viktor Safronov and others in the 1940s and 1950s, this
hypothesis builds on the nebular hypothesis but provides more detail on the formation
of planets.
 Process:
o Within the protoplanetary disk, dust and gas began to coalesce into small
particles.
o These particles collided and stuck together, forming larger bodies called
planetesimals.
o Planetesimals continued to collide and merge, eventually forming
protoplanets.
o Protoplanets underwent further collisions and accretion to form the planets.
 Evidence:
o The presence of asteroids and comets, which are thought to be remnants of the
planetesimal stage.
o The cratering on planetary surfaces, indicative of past collisions.
3. Protoplanet Hypothesis
 Overview: This hypothesis is a modern refinement of the planetesimal hypothesis,
integrating ideas from both the nebular hypothesis and the concept of planetesimals.
 Process:
o The solar nebula collapses and forms a rotating disk.
o Within the disk, particles aggregate into planetesimals.
o Planetesimals merge into larger bodies called protoplanets.
o Protoplanets undergo differentiation and clearing of their orbits, forming the
planets.
 Evidence:
o Observations of young star systems with protoplanetary disks.
o Computer simulations of planetary formation that match the current solar
system structure.
4. Capture Theory
 Overview: Proposed by Michael Woolfson in the 1960s, this hypothesis suggests that
the Sun captured a passing cloud of gas and dust, leading to the formation of the solar
system.
 Process:
o The Sun passed through a dense interstellar cloud.
o The gravitational pull of the Sun caused the cloud to collapse and form a
protoplanetary disk.
o Planetesimals and protoplanets formed within this disk, leading to the creation
of the solar system.
 Evidence:
o This theory has less observational support compared to the nebular hypothesis.
o It struggles to explain the angular momentum distribution in the solar system.
5. Modern Laplacian Hypothesis
 Overview: A variation of the nebular hypothesis, this model incorporates modern
understanding of angular momentum and accretion processes.
 Process:
o Similar to the nebular hypothesis, but with a focus on the role of turbulence
and magnetic fields in the protoplanetary disk.
o Emphasizes the gradual buildup of material from small dust grains to
planetesimals to planets.
 Evidence:
 o Supported by observations of young stellar objects and protoplanetary disks.
o Consistent with computer models of disk evolution and planet formation.
6. Solar Fission Theory
 Overview: Proposed by George Darwin, this hypothesis suggests that the Sun ejected
material due to its rapid rotation, which eventually coalesced to form the planets.
 Process:
o The Sun was once a rapidly rotating body.
o Due to centrifugal forces, it ejected rings of material.
o These rings of material condensed to form the planets.
 Evidence:
o This theory has largely been discredited due to a lack of supporting evidence
and its inability to explain certain features of the solar system, such as the
distribution of angular momentum.
7. Accretion Theory
 Overview: This hypothesis combines elements of the nebular and planetesimal
hypotheses but places more emphasis on the role of accretion in the formation of the
planets.
 Process:
o A protoplanetary disk forms around the young Sun.
o Dust and gas in the disk gradually accumulate into larger bodies through
accretion.
o Planetesimals form and grow by colliding and sticking together, eventually
forming planets.
 Evidence:
o Supported by observations of disks around young stars.
o Consistent with the distribution of material in the solar system.

Earth's unique combination of distance from the Sun, atmospheric composition, liquid water,
magnetic field, geological activity, stable climate, and diverse ecosystems make it the only
known planet in the solar system capable of supporting life. Understanding these properties
highlights the rarity and fragility of our planet, emphasizing the importance of preserving its
life-supporting conditions.

Earth is uniquely positioned in the solar system to support life. It has a combination of
properties that make it the only known planet where life as we know it can exist. These
properties include its distance from the Sun, its atmosphere, its water supply, its magnetic
field, and its geological activity.
Key Properties Supporting Life on Earth
1. Optimal Distance from the Sun (The Habitable Zone)
 Description: Earth orbits the Sun at an optimal distance, often referred to as the
"Goldilocks Zone" or habitable zone, where temperatures are just right for liquid
water to exist.
 Importance: Liquid water is essential for all known forms of life. If Earth were
closer to the Sun, it would be too hot, and if it were farther away, it would be too cold
for liquid water to persist.
2. Atmosphere
 Composition: Earth's atmosphere is composed of 78% nitrogen, 21% oxygen, and
trace amounts of other gases like carbon dioxide and water vapor.
 Functions:
o Oxygen Supply: Supports respiration for aerobic organisms.
o Ozone Layer: Protects living organisms from harmful ultraviolet (UV)
radiation from the Sun.
o Greenhouse Effect: Maintains a stable and warm climate by trapping heat.
3. Presence of Liquid Water
 Description: Earth has abundant liquid water on its surface, covering about 71% of
the planet.
 Importance: Water is a solvent for biochemical reactions, a medium for nutrient
transport, and essential for regulating temperature and climate.
4. Magnetic Field
  Generation: Earth's magnetic field is generated by the movement of molten iron in
its outer core.
 Protection: Shields the planet from harmful solar wind and cosmic radiation, which
could strip away the atmosphere and damage living organisms.
5. Geological Activity
 Plate Tectonics: Earth's surface is divided into tectonic plates that move and interact,
causing earthquakes, volcanic activity, and mountain building.
 Nutrient Recycling: Tectonic activity recycles nutrients through processes like
volcanic eruptions and seafloor spreading, supporting the biosphere.
6. Stable Climate and Seasons
 Axial Tilt: Earth's axial tilt of 23.5 degrees results in the seasonal variation of
climate, which helps create diverse habitats and promotes biodiversity.
 Climate Regulation: Earth's climate is regulated by various natural processes,
including the water cycle, carbon cycle, and ocean currents, providing a stable
environment for life.
7. Diverse Ecosystems
 Biodiversity: Earth supports a wide range of ecosystems, from tropical rainforests to
arctic tundras, each hosting diverse species adapted to their specific environments.
 Adaptation and Evolution: The diversity of environments and ecosystems has
driven the evolution of a vast array of life forms, each adapted to its niche.
Comparison with Other Planets
 Mars: Mars has evidence of past liquid water and a thin atmosphere, but it lacks a
magnetic field and has harsh surface conditions, making it inhospitable for current
life.
 Venus: Venus has a thick, toxic atmosphere primarily composed of carbon dioxide,
with surface temperatures hot enough to melt lead, preventing any form of known
life.
 Gas Giants (Jupiter, Saturn, Uranus, Neptune): These planets lack solid surfaces
and have extreme atmospheric conditions that are not conducive to life as we know it.
 Other Moons and Bodies: While moons like Europa and Enceladus have subsurface
oceans, they lack the combination of conditions necessary to support life on their
surfaces.
Earth is a complex, dynamic system made up of four interconnected subsystems: the
geosphere, hydrosphere, atmosphere, and biosphere. These subsystems interact with each
other through the continuous exchange of matter and energy, creating the conditions
necessary for life and shaping the planet's environment.
1. Geosphere
 Description: The geosphere includes the solid parts of the Earth, such as rocks,
minerals, mountains, and the Earth's core, mantle, and crust.
 Components:
o Crust: The thin, outermost layer where we live.
o Mantle: A thick layer of hot, solid rock beneath the crust.
o Core: The innermost part, consisting of a solid inner core and a liquid outer
core.
 Functions:
o Provides nutrients and minerals essential for life.
o Drives plate tectonics, which influences the formation of landforms and the
distribution of continents.
2. Hydrosphere
 Description: The hydrosphere encompasses all the water on Earth, including oceans,
rivers, lakes, glaciers, groundwater, and water vapor.
 Components:
o Oceans: Cover about 71% of the Earth's surface and contain the majority of
Earth's water.
o Freshwater Bodies: Include rivers, lakes, and groundwater, which are crucial
for drinking water and agriculture.
o Ice: Glaciers and polar ice caps store freshwater and influence global climate
 patterns.
 Functions:
o Regulates temperature and climate through the distribution of heat.
o Provides habitat for aquatic life and is essential for all living organisms.
3. Atmosphere
 Description: The atmosphere is the layer of gases surrounding Earth, composed
mainly of nitrogen (78%) and oxygen (21%), with traces of other gases like carbon
dioxide and water vapor.
 Components:
o Troposphere: The lowest layer, where weather occurs.
o Stratosphere: Contains the ozone layer, which protects against harmful UV
radiation.
o Mesosphere, Thermosphere, and Exosphere: Higher layers with varying
functions, including protecting Earth from meteoroids and housing the
ionosphere.
 Functions:
o Protects life by blocking harmful solar radiation.
o Regulates temperature through the greenhouse effect.
o Facilitates the water cycle and weather patterns.
4. Biosphere
 Description: The biosphere includes all living organisms on Earth, from the deepest
ocean trenches to the highest mountains and into the atmosphere.
 Components:
o Flora: Plants that perform photosynthesis, producing oxygen and food.
o Fauna: Animals that depend on plants and other animals for food.
o Microorganisms: Bacteria, fungi, and other microscopic life forms that play
essential roles in nutrient cycling and decomposition.
 Functions:
o Supports and sustains life through food chains and ecosystems.
o Contributes to the carbon and nitrogen cycles, crucial for maintaining life-
supporting conditions.
Interactions and Flow of Matter and Energy
Matter and Energy Exchange
 Water Cycle: Water evaporates from the hydrosphere, condenses in the atmosphere,
and precipitates back to the geosphere and biosphere.
 Carbon Cycle: Carbon dioxide is absorbed by plants (biosphere) during
photosynthesis, released back into the atmosphere through respiration and
decomposition, and stored in the geosphere as fossil fuels.
 Nutrient Cycle: Nutrients like nitrogen and phosphorus move through the soil
(geosphere), water (hydrosphere), air (atmosphere), and living organisms (biosphere).
Energy Flow
 Solar Energy: The primary source of energy, driving weather patterns, ocean
currents, and photosynthesis.
 Geothermal Energy: Heat from the Earth's interior drives plate tectonics and
volcanic activity.
 Biological Energy: Energy flows through food chains from producers (plants) to
consumers (animals) and decomposers (microorganisms).
Examples of Interactions
 Volcanic Eruptions (Geosphere to Atmosphere): Release ash and gases into the
atmosphere, affecting climate and weather patterns.
 Photosynthesis (Atmosphere to Biosphere): Plants absorb carbon dioxide and
sunlight to produce oxygen and glucose, supporting life.
 Weathering and Erosion (Atmosphere and Hydrosphere to Geosphere): Wind
and water break down rocks, transporting sediments and reshaping landscapes.
Current Advancements and Information on the Solar System
Recent years have seen significant advancements in our understanding of the solar system,
driven by new technologies, space missions, and scientific discoveries. Here are some of the
most notable recent advancements:
1. Mars Exploration
 Perseverance Rover: Launched by NASA in July 2020, Perseverance landed on
Mars in February 2021. Its mission is to search for signs of past microbial life, collect
rock and soil samples, and prepare for future human exploration. The rover has
already provided detailed images, conducted experiments, and identified promising
rock samples for future return missions.
 Ingenuity Helicopter: Accompanying Perseverance, Ingenuity is the first aircraft to
attempt controlled flight on another planet. It has successfully completed numerous
flights, demonstrating the potential for aerial exploration of Mars.
2. Moon Exploration
 Artemis Program: NASA's Artemis program aims to return humans to the Moon by
2024 and establish a sustainable presence by the end of the decade. This includes the
development of the Space Launch System (SLS) rocket and the Orion spacecraft, as
well as plans for the Lunar Gateway space station and lunar landers.
 China's Lunar Missions: China's Chang'e program has achieved several milestones,
including the Chang'e 4 mission, which successfully landed on the far side of the
Moon in 2019, and the Chang'e 5 mission, which returned lunar samples to Earth in
December 2020.
3. Outer Solar System Exploration
 Juno Mission: NASA's Juno spacecraft has been orbiting Jupiter since 2016,
providing detailed information about the planet's atmosphere, magnetic field, and
internal structure. It has captured stunning images of Jupiter's clouds and storms and
gathered data on its moons.
 Europa Clipper: Scheduled for launch in the mid-2020s, this NASA mission will
investigate Jupiter's moon Europa, which is believed to have a subsurface ocean. The
mission aims to assess Europa's habitability and search for signs of life.
4. Asteroid and Comet Exploration
 OSIRIS-REx: NASA's OSIRIS-REx mission successfully collected samples from the
asteroid Bennu in October 2020. The spacecraft is now on its way back to Earth, with
the samples expected to arrive in 2023. This mission will provide insights into the
early solar system and the building blocks of life.
 Hayabusa2: Japan's Hayabusa2 mission returned samples from the asteroid Ryugu to
Earth in December 2020. The mission has provided valuable data on the composition
of asteroids and the early solar system.
5. Exoplanet Research
 TESS Mission: NASA's Transiting Exoplanet Survey Satellite (TESS) has been
identifying exoplanets (planets outside our solar system) by monitoring the brightness
of nearby stars. Since its launch in 2018, TESS has discovered thousands of exoplanet
candidates, enhancing our understanding of planetary systems.
 James Webb Space Telescope (JWST): Scheduled for launch in December 2021,
JWST will be the most advanced space telescope ever built. It will study exoplanets,
star formation, and the early universe, providing unprecedented detail and expanding
our knowledge of distant solar systems.
6. Planetary Science
 Volcanism on Venus: Recent studies suggest that Venus may still be volcanically
active, with evidence of recent volcanic eruptions. This challenges the long-held view
of Venus as a geologically dead planet and has implications for understanding its
atmosphere and evolution.
 Pluto and Beyond: NASA's New Horizons mission, which provided the first close-
up images of Pluto in 2015, has continued to explore the Kuiper Belt. In 2019, it
conducted a flyby of the Kuiper Belt object Arrokoth, revealing insights into the early
solar system.
7. Solar Observations
 Parker Solar Probe: Launched in 2018, NASA's Parker Solar Probe is studying the
Sun's outer corona, solar winds, and magnetic fields by flying closer to the Sun than
any previous spacecraft. The mission aims to improve our understanding of solar
 processes and their impact on space weather.
 Solar Orbiter: A collaboration between ESA and NASA, the Solar Orbiter mission,
launched in 2020, is studying the Sun's poles and solar wind. The spacecraft is
providing high-resolution images and data to understand the Sun's behavior and its
effects on the solar system.
8. Planetary Defense
 DART Mission: NASA's Double Asteroid Redirection Test (DART) mission,
launched in November 2021, aims to test our ability to change the trajectory of an
asteroid. DART will collide with the moonlet of the asteroid Didymos to assess the
feasibility of asteroid deflection as a planetary defense strategy
Many individuals have made significant contributions to our understanding of Earth's
systems. Their work spans various fields, including geology, meteorology, oceanography,
and environmental science. Here’s a look at some key personalities and their contributions:
1. James Hutton (1726–1797)
 Contribution: Often regarded as the "Father of Modern Geology."
 Key Work: Developed the theory of uniformitarianism, which posits that the Earth's
processes observed in the present have worked in the same way throughout geological
time. His work laid the foundation for modern geology and understanding of Earth's
history.
2. Charles Lyell (1797–1875)
 Contribution: Promoted and expanded on Hutton’s ideas.
 Key Work: His book Principles of Geology (1830–1833) provided a comprehensive
exposition of uniformitarianism and greatly influenced the scientific community,
including Charles Darwin.
3. Alfred Wegener (1880–1930)
 Contribution: Proposed the theory of continental drift.
 Key Work: His theory, published in The Origin of Continents and Oceans (1915),
suggested that continents were once connected in a supercontinent called Pangaea and
have since drifted apart. This theory laid the groundwork for the development of plate
tectonics.
4. Marie Tharp (1920–2006)
 Contribution: Mapped the ocean floor and supported the theory of plate tectonics.
 Key Work: Created the first detailed map of the Atlantic Ocean floor, revealing the
Mid-Atlantic Ridge and supporting the theory of seafloor spreading, which provided
crucial evidence for plate tectonics.
5. Harry Hess (1906–1969)
 Contribution: Developed the theory of seafloor spreading.
 Key Work: His work during World War II on submarine warfare led to the discovery
of mid-ocean ridges and the idea that new oceanic crust is formed at these ridges and
spread outward. His theory was fundamental in developing the plate tectonics theory.
6. Vladimir Vernadsky (1863–1945)
 Contribution: Pioneered the concept of the biosphere.
 Key Work: His work The Biosphere (1926) introduced the idea that the biosphere is
a global ecological system integrating all living beings and their relationships with the
atmosphere, hydrosphere, and geosphere.
7. Rachel Carson (1907–1964)
 Contribution: Raised awareness about environmental issues and the impact of
pesticides.
 Key Work: Her book Silent Spring (1962) documented the adverse effects of
pesticides on the environment and is credited with advancing the environmental
movement and leading to changes in environmental policy.
8. John Tyndall (1820–1893)
 Contribution: Investigated the greenhouse effect.
 Key Work: Tyndall’s experiments demonstrated that certain gases (e.g., carbon
dioxide) trap heat in the atmosphere, contributing to our understanding of the
greenhouse effect and climate change.
9. Louis Agassiz (1807–1873)
  Contribution: Studied glaciation and the impact of ice ages.
 Key Work: His research on glaciers and ice ages provided early evidence for the
existence of past ice ages, leading to a better understanding of Earth's climatic
history.
10. James Lovelock (1919–2018)
 Contribution: Developed the Gaia theory.
 Key Work: The Gaia theory proposes that the Earth functions as a self-regulating
system with living and non-living components interacting to maintain conditions
conducive to life. His work has influenced environmental science and the study of
Earth's systems.
11. Eugene Shoemaker (1928–1997)
 Contribution: Contributed to the understanding of impact craters.
 Key Work: Shoemaker’s research on impact craters, including the discovery of the
Shoemaker-Levy 9 comet's impact with Jupiter, advanced our understanding of the
role of extraterrestrial impacts in shaping Earth’s geology.
12. Klaus Hasselmann (1931–2023)
 Contribution: Developed climate models linking human activities to climate change.
 Key Work: Hasselmann’s work on climate models and the detection of
anthropogenic climate change has been fundamental in understanding and predicting
climate change effects.
The Earth is composed of several distinct layers, each with unique properties and
characteristics. These layers can be broadly categorized into three main divisions: the crust,
the mantle, and the core. Here's a detailed look at each layer:
1. Crust
 Description: The outermost layer of the Earth, consisting of solid rock.
 Types:
o Continental Crust: Forms the continents and is primarily composed of
granitic rocks. It is thicker (averaging about 35 km to 40 km) and less dense
compared to oceanic crust.
o Oceanic Crust: Underlies the oceans and is primarily composed of basaltic
rocks. It is thinner (averaging about 7 km to 10 km) and denser compared to
continental crust.
 Characteristics:
o The crust is divided into tectonic plates that float on the semi-fluid mantle
beneath them.
o It is where we find all surface features such as mountains, valleys, and plains.
2. Mantle
 Description: The layer beneath the crust, extending to a depth of about 2,900 km. It
is composed of silicate minerals rich in iron and magnesium.
 Structure:
o Upper Mantle: Extends from the base of the crust down to about 410 km. It
includes the lithosphere (the rigid outer part of the Earth) and the
asthenosphere (a more ductile, semi-fluid region that allows for tectonic plate
movement).
o Transition Zone: From about 410 km to 660 km deep. This region
experiences changes in mineral composition and density due to increasing
pressure.
o Lower Mantle: Extends from about 660 km to 2,900 km. It is more rigid
compared to the upper mantle, though still capable of slow, convective flow.
 Characteristics:
o The mantle's convective currents drive the movement of tectonic plates and
influence volcanic activity.
o It contains the majority of Earth's mass and volume.
3. Core
 Description: The innermost layer of the Earth, composed mostly of iron and nickel.
 Structure:
o Outer Core: Extends from about 2,900 km to 5,150 km deep. It is in a liquid
 state and is responsible for generating Earth's magnetic field through its
convective motions.
o Inner Core: Extends from about 5,150 km to the center of the Earth at about
6,371 km. It is solid and extremely hot, with temperatures reaching up to
5,700°C. The inner core is solid due to the immense pressure despite the high
temperatures.
 Characteristics:
o The core plays a crucial role in generating Earth's magnetic field and
influencing seismic activity.
Summary
 Crust: The outer layer, including continental and oceanic crust, with a solid structure.
 Mantle: Located beneath the crust, divided into the upper mantle (including the
lithosphere and asthenosphere), transition zone, and lower mantle, characterized by
convective flow.
 Core: The innermost layer, consisting of a liquid outer core and a solid inner core,
responsible for Earth's magnetic field.
These layers interact dynamically, influencing geological processes such as plate tectonics,
volcanism, and seismic activity.

Exposition Time Allotment: Day: Thursday

(DEEPEN)
E. Making
generalizations
and abstractions
about the lesson

Integration Time Allotment:

(TRANSFER)
F. Creating a
Realistic
Performance
Output

Evaluation Time Allotment: 1 hour Day: Tuesday

(TRANSFER)

Criteria for
Evaluation

Performance Time Allotment: Day: Monday

Output
(TRANSFER)
Advance Study