Blue Brown Watercolour Style Water Cycle Presentation Title Slide: Title: "The Water Cycle: A Blue Brown Watercolour Journey" Subtitle: "Exploring the Earth's Natural Water Process" Background: Watercolor-style illustration blending blue and brown hues, depicting a stylized representation of the water cycle. Slide 1: Introduction Welcome message: "Welcome to our presentation on the water cycle!" Brief overview: "Today, we'll be diving into the fascinating world of the water cycle, exploring how water moves through the environment in a continuous process." Slide 2: What is the Water Cycle? Definition: "The water cycle, also known as the hydrological cycle, is the continuous movement of water on, above, and below the surface of the Earth." Visual: Diagram of the water cycle, with labels for evaporation, condensation, precipitation, and collection. Slide 3: Key Processes of the Water Cycle Evaporation: Explanation of how water evaporates from oceans, lakes, and rivers, driven by solar energy. Condensation: Description of how water vapor in the atmosphere cools and condenses into clouds. Precipitation: Explanation of how condensed water droplets fall to the Earth as rain, snow, sleet, or hail. Collection: Overview of how water collects in bodies of water, such as rivers, lakes, and oceans, before repeating the cycle. Slide 4: Importance of the Water Cycle Environmental balance: Discussion on how the water cycle maintains ecological balance by distributing water across different ecosystems. Human impact: Explanation of how human activities, such as deforestation and urbanization, can disrupt the water cycle and lead to water scarcity. Slide 5: Water Cycle in Action Real-world examples: Showcase of how the water cycle impacts different regions, such as arid deserts and tropical rainforests. Case study: Detailed analysis of a specific location or event where the water cycle plays a crucial role, such as a drought or flood. Slide 6: Conservation and Management Conservation practices: Overview of strategies for conserving water, such as rainwater harvesting and efficient irrigation techniques. Management approaches: Discussion on how governments and organizations can manage water resources sustainably to ensure long-term availability. Slide 7: Conclusion Recap: Summary of key points discussed in the presentation. Call to action: Encouragement for viewers to learn more about the water cycle and take steps to protect water resources. Slide 8: Additional Resources Links to further reading: References to books, articles, or websites for more information on the water cycle and water conservation. Slide 9: Thank You Thank you message: "Thank you for joining us on this journey through the water cycle!" Contact information: Optional contact details for the presenter or organization hosting the presentation. Slide 10: Questions and Answers Q&A session: Invite viewers to ask questions or share their thoughts on the presentation. Feel free to add more de

1. Star Life Cycle
T. RONNA JANE DC. MANUEL

2. Objectives:
Infers the characteristics of stars
based on the characteristics of
the sun

3. LET’S PICK-UP!
T. RONNA JANE DC. MANUEL

4. The Constellations
 Origins
 Star patterns named by
ancient peoples after
gods, goddesses,
animals, monsters, and
mythic heroes.
 The constellations used
by Western Culture
today originated in
Mesopotamia around
3,000 B.C.

5. The Constellations
 Only certain stars were part
of the pattern and belonged
to the constellation. Faint
stars were not part of any
constellations.
 Frequently constellations
were named for their
brightest star.
 Of the constellations
defined by the Babylonians,
Egyptians, and Greeks, 48
are still used today.

6. The Constellations
 The ancient civilizations
we got the 48 classical
constellations from
couldn’t see the entire
southern sky.
 During the Age of Sail,
European explorers
added 40 modern
constellations in the
“uncharted” areas of
the sky.

7. The Constellations
 The 48 classical and the 40 modern
constellations make up the 88 official
constellations used by astronomers today.
 The term constellation also now has a new
meaning:
 No longer refers to the pattern of stars itself.
 Now refers to a well defined region of the sky that
contains the traditional star pattern.
 Everything inside that region of the sky is now part
of the constellation, like a “celestial state”.

8. The Constellations

10. Stellar Evolution: Life of the Star
 The most massive stars
have the shortest lives.
Stars that are 25 to 50
times that of the sun live
for only a few million years.
Stars like our Sun live for
about 10 billion years. Stars
less massive than the Sun
have even longer life spans
 Stars are like humans they
are born, live and die

11. Stars are formed in
1. Nebulae, interstellar clouds
of dust and gas (mostly
hydrogen).
2. These stellar nurseries are
abundant in the arms of
spiral galaxies.
3. In these stellar nurseries,
dense parts of these clouds
undergo gravitational
collapse and compress to
form a rotating gas globule.
The Birth of Stars
It begins to spin as it shrinks

12. NEBULA PICTURES

13. Protostar stage: The nebula flattens
and the center condenses:
• Temps start to increase due to
friction (more collision of
molecules).
• When temps reach 10 million K,
NUCLEAR FUSION begins
• Nuclear Fusion generates the
energy for a star.
• When fusion begins, it is officially
considered a STAR. (yeah!)
• Fusion – combining a lightweight
nuclei into a heavier nuclei

14. Protostar
Pictures

16. Stars live out the majority of
their lives in a phase termed
as the Main Sequence.
Longest stage of a star
The protostar is now a stable
main sequence star which will
remain in this state for about 10
billion years. After that, the
hydrogen fuel is depleted and
the star begins to die.
Main-Sequence Stage

17. Main Sequence Star

18. When a star has burned between 10% and 20% of its
hydrogen, its core will to run out of fuel.
At this stage, the star is entering the end of its life.
The diameter of the star can increase by a factor of 200,
while its cooling is translated into a reddening of its
radiation : the star is becoming what is called a red giant.
RED GIANT STAGE

19.  Star has run out of
Hydrogen atoms in the
core to undergo fusion.
 Our sun has used only
about 5% of its Hydrogen
 Star expands about 10x
bigger and cools.
 Its luminosity increases,
temp decreases.
 Helium fuses to form
Carbon, and the core
shrinks.
 It begins losing outer
layers

20. BETELGEUSE –RED GIANT
 Only a few million years old,
Betelgeuse is already dying.
Astronomers predict that it's
doomed to explode as a
soon, within 1,000 years or
so, an event that will be
spectacular for Earth's
future inhabitants.
(Conceivably, it's already
happened as Betelgeuse is
640 light-years away!)

21. •Star size comparison

22. Burnout and Death
 Fate of a Star depends
on its mass
 All stars, regardless of
size, run out of fuel
and collapse due to
gravity
 A star will become
either a black
dwarf, neutron
star, or black hole,
depending on
how massive it
was. .

23. Death of low-mass stars
 Never evolve into red giants
 Remain stable main-sequence
stars until hydrogen is gone
 Collapse into white dwarfs

24. Death of medium-mass stars
 Sun-like Stars
(Mass under 1.5 times the mass of the Sun)
Red Giant --> Planetary Nebula -->White Dwarf
--> Black Dwarf

25. Death of massive stars
 Huge Stars
(Mass between 1.5 to 3 times
the mass of the Sun)
Red SuperGiant -->
Supernova --> Neutron
Star
 Giant Stars
(Mass over 3 times the mass
of the Sun)
Red SuperGiant -->
Supernova --> Black Hole

28. PLANETARY NEBULA
 This is left when a giant loses its
outer layers of gas.
 Leaves only the core.
 The core will become a white
dwarf

29. Planetary nebula
pictures

30. WHITE DWARF
Only hot, dense core is left of this star.
 It will shine for billions of years before cooling.
 Stable star with no nuclear fuel,radiates left over fuel for billions
of years
 Could become a black dwarf, but the universe is not old
enough to form these

31. White Dwarf Pictures

33. SUPER NOVA
 Super Giant eventually
loses its outer layers in an
explosion leaving only
the core – this is the super
nova.

34. Eventually this core collapses (in an instant). As
the iron atoms are crushed together in this
gravitational collapse, the core temperature rises
to about 100 billion degrees.
The repulsive electrical forces
between the atoms' nuclei overcomes
the gravitational forces, causing a
massive, bright, short-lived explosion
called a supernova. During the
explosion, shock waves, blow away the
star's outer layers.

35. NEUTRON STAR
 After a Super Nova explosion, the core may
condense into a small core of neutrons.
 It is so dense – 1 spoonful of Earth would weigh
100 million tons.
 Rotates very rapidly.
If the star's remaining mass is between 1 1/2 to 3
times the mass of the Sun, it will collapse into a
small, dense neutron star (about ten miles in
diameter, about 1.4 times the mass of the Sun,
with an extraordinarily strong magnetic field, and
rapid spin).

36. Neutron Star Pictures

38. BLACK HOLE
 This is the 3rd predicted result to a star.
 This is the most dense core of a star that
can be left.
 Gravity is so strong, light cannot escape.
 Makes it look like a dark hole in space.
If the star's remaining mass is greater than
three times the mass of the Sun, the star
contracts tremendously and becomes a
black hole

39. Black Hole Pictures
Anatomy of a black hole

40.  The density of a star is pre-determined based on its weight (the
amount of dust and gas) it begins with.
 Smaller stars become white dwarfs.
 Very large stars become neutron stars or black holes.
•Life Cycle of a Star Video

41. LET’S CREATE!
Open your book on page 201
and answer Activity Zone