LP

1. FIAT LUX ACADEME
CAVITE
SENIOR HIGH SCHOOL DEPARTMENT
Columnar Lesson Plan in Physical Science
Week 4 February 26-March 1, 2024
Subject Matter Objectives Activities Evaluation/Assessment Remarks
Topic:
Continuation of Formation
of Heavier Elements in the
Evolution of the Universe
Monday: Gr. 11 HUMSS Sartre (8:00 A.M. - 9:00 A.M.), Gr. 11 ABM Adams
(10:30 A.M. - 12:30 P.M), Gr. 12 TVL White (1:10 P.M - 3:10 P.M)
Tuesday and Thursday: Gr. 11 HUMSS Aristotle (8:00 A.M. - 10:00 A.M.), Gr.
11 ABM Bloomberg (3:10 P.M. - 4:10 P.M.)
Wednesday: Gr. 11 HUMSS Sartre (7:00 A.M. - 9:00 A.M.), Gr. 11 ABM Adams
(10:30 A.M. - 12:30 P.M), Gr. 12 TVL White (1:10 P.M - 3:10 P.M)
A. Preparation
A. Prayer
B. Greetings
C. Classroom Management
D. Checking of attendance
B. Motivation
Video Watch
The teacher will present a video clip for an initial knowledge on nucleosynthesis
and formation of heavier elements.
C. Lesson Proper/Discussion
Helium is made inside the star. The fusion of hydrogen nuclei to form helium
produces energy that powers the early stars and the present-day sun. The energy

2. References:
Caintic, H. (2020).
Physical Science for
Senior High School
Revised Edition. C &
E Publishing Inc.,
Quezon City.
Camacho, D., Palomar, B.
& Pantig, R. (2018).
Fundamentals of
Physical Science.
Abiva Publishing
House, Quezon City.
Ungson, O. (2016).
Physical Science
11/12. Trinitas
Publishing Inc.,
Quezon City.
Materials:
- PPT
- Laptop
- Book
- Periodic Table of
Elements
produced eventually causes the star to expand and cool down in its outer layer,
turning it into a red giant star.
As the stars evolved, the early universe existed with nothing but the first four
elements in the periodic table with hydrogen and helium dominating plus traces of
lithium and beryllium (and probably boron as well). These elements were first
formed because they have the simplest and lightest atomic nuclei.
A new element with six protons is produced and that is how the carbon (C) atom
is synthesized. Since the formation of the stable carbon-12 requires the collision
of three helium-4 nuclei, this nuclear process is called the triple alpha process. -
Sharing of Thoughts/Ideas

3. ● describe the
circumstances
that led to the
development
of the model
of atom
generates a relatively smaller energy compared to the proton-proton chain.
Thermonuclear is used to describe nuclear fusion involving high temperatures.
Major source of energy in stars enters into the second red giant phase. At this
phase, the heavier atoms–carbon, nitrogen, and oxygen–move to the core. Outside
this core is the layer where helium is being converted to carbon via the triple alpha
process. The next outer layer is a shell where helium is located at a temperature
low enough such that a thermonuclear reaction is not possible.
As a star matures, an important factor that plays a role in its growth is the loss of
mass. Solar mass is a unit based on the sun’s mass to indicate the mass of a star
Activity 3:
Balancing Nuclear Reactions
Predict the product or reactant
of the ff: nuclear reactions.

4. and other celestial bodies. Stellar winds are exceedingly hot gasses of ions that are
produced from the star’s surface. Additional mass loss at the surface of the star is
also due to helium burning or the consumption of helium. The mass of the
resultant star defines its properties because it indicates how much fuel is available,
that also affects the nuclear processes inside the star.
The rate at which the star uses its available fuel defines its brightness or
luminosity.
Lifetime = mass/luminosity x 10^10 years.
White dwarf - stage of the star that contains super-dense matter that is rich in
carbon and oxygen.
As helium fusion ends in a star, carbon begins to undergo further nuclear reactions
to create elements such as oxygen (O), neon (Ne), magnesium (Mg), silicon (Si)
until iron (Fe). At this stage, stars become red supergiant stars that are
characterized as very dense and massive.

5. Most nuclei heavier than 56Fe are due to neutron capture:
- s-process, in which neutron addition is slow compared to β-decay
- r-process, in which neutron addition is rapid compared to β-decay
Supernova - last stage of a star’s life cycle after a red supergiant star collapses and
shows an abrupt increase in its brightness where the population of neutrons is
large, allowing the neutron to occur in a fraction of a second.
The theory of nucleosynthesis and the formation of heavier elements were
proposed based not only on mathematics but also on observation in nature in
terms of the calculated and natural abundance of the chemical elements and their
isotopes on earth, in stars, and in interstellar space.
To summarize, after the expansion, the first light elements were created when the
star was born. The next elements up to magnesium were then produced in red
supergiant stars. Elements from iron to uranium were formed in supernovae.

6. These atoms then collided in space and chemical reactions occurred. These atoms
or molecules combined to form simple matter, which over time became more
complex and eventually led to the formation of today’s physical world.
Prepared by: Checked by:
Ms. Angeline O. Avendaño Rosahle S. Pagadora, MS
Faculty, SHS Principal