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UNIT: 5 (PHYSICS FROM CREATION TO COLLAPSE)
SECTION TITLE: REACH FOR THE STARS
(5/STA)
Lesson
1
2
3+
Content
Learning Outcomes
Lesson Activities
Introduction
Overview of topic.
Appreciate the role and
importance of Cosmology in
ancient & modern societies.
General introduction to topic – ask
students what Cosmology is.
Show students concept map for the topic
& emphasise key areas of study.
Students make a glossary of key words.
DEMO: PowerPoint show on
Cosmology (see GHU).
Discuss nature of images.
Discuss the meaning of ‘FLUX’ & relate
to energy from the Sun.
Revise the meaning of the ‘inverse square
law’ (use examples on board). Read
p271-272.
Explain formula: F = L / 4d2
Discuss methods by which heat escapes
from the Sun (Convection, etc).
Questions
DEMO: Activity 2 Compare different
hot objects (Colour, Temperature &
Luminosity). Discuss results.
Explain Black-Body Spectrum &
radiation curves (see diagrams on p274).
Show the website on interactive BlackBody Spectrums (see list). Briefly discuss
formulae for Wein’s Law: maxT =
constant & Stefan’s La:w
F =  T4 .
Past paper questions.
Luminosity
Blackbodies &
Temperature
Recognise & Use the
connection between Flux
and Luminosity:
F = L / 4d2
Appreciate the idea of
Black-Body radiation and
the associated radiation
curves for different
temperatures.
Updated July 2006
Directed study &
references.
A2 book p 266-271
Risk ratings &
Resources needed
None
Laptop & projector
Activity 1:
Find out about the Sun +
Solar Physics (research).
A2 book p 270-273
Questions 1-3
None
You can show an ICT
animation of the inverse
square law (in the
shared area)
A2 book p 273-276
Questions 4-5
Additional sheet 1
Read p 277-278 and
answer Q6-8.
Read ahead: p279-280
(How old is the Solar
System?)
Risk rating C3
See notes for Activity
2. You could safely
heat an iron bar behind
a Bunsen screen. Care
will be needed.
Lesson
Content
Learning Outcomes
Lesson Activities
4+
Radiation
Appreciate the random &
spontaneous nature of
radioactive decay.
Know & Use the terms
nucleon (mass) number,
proton (atomic) number.
Ask groups of 2-3 students to draw a
quick mind-map to show what they
remember about radioactivity.
Revise random nature of radioactive
decay, background radiation, ,,
radiation & their properties.
DEMO: Activity 7 – Show properties
of ,, radiation. Alternatively, you
could do this as an ICT experiment using
the A2 Salters Virtual experiments.
Discuss changes in atomic structure that
result from the 3 main decay methods.
Questions.
Revise the idea of decay & half-life.
Define Decay Constant, , and Activity,
A and formula: A = dN/dt = -N.
Define Half life: t½ = ln2/.
Discuss radioactive decay and state the
Decay formula: N=Noe-t .
Sample questions. See examples on p289.
Past papers – June 2001 Q3, June 2000
Q4
Discuss nature of the Sun & how it
releases energy.
DEMO: Activity 11 (Projecting
Sunspots), if Sun is visible. Discuss
causes of sunspots.
DEMO: Activity 12 (Sun’s spectrum), if
Sun is visible. Discuss features &
Fraunhofer lines.
Revise causes of Emission & Absorption
spectra and their characteristic features.
VIDEO: Sun (Solar Physics) (20 mins)
5-6
7
Radioactive
Decay
Sunspots &
Spectra
Determine half-life
graphically.
Use equations for
radioactive decay.
Realise that the spectrum
from the Sun shows
characteristic Absorption
lines.
Directed study &
references.
A2 book p 280-286
Questions 9-12
Research activity:
Activity 9 - Find out how
Background count rate
varies across the planet
(use Internet to
investigate). Key skills
N2a, N3a, N3d, N4a/b.
A2 book p 286-292
Questions 13-17
Risk ratings &
Resources needed
Risk rating C3
Radioactive sources,
PANAX kit, GM tube
& ratemeter.
Make sure you sign
sources in/out & follow
standard rules for use of
radioactive sources.
None
Students can carry out
the A2 Salters Virtual
experiment – Half life of
Protactinium.
A2 book p 292-294
Questions 18
Research on Sunspots
(causes & patterns).
Write it up as a magazine
article. Key skills IT4d
Risk rating C3
ACTIVITY 11 Telescope or binoculars
& card with mount (see
GHU for either).
ACTIVITY 12 –
Student spectrometers.
VCR + TV.
NOTE: DO NOT
LOOK AT THE SUN!
Lesson
Content
Learning Outcomes
8
Nuclear Fusion
Explain the process of
Nuclear Fusion and
appreciate the need for high
Temperatures & Matter
Densities.
Understand the concept of
Nuclear Binding Energy.
9
Nuclear Fission
Describe the process of
Nuclear Fission and use the
formula: E=mc2
10*
Stellar Motion
& Distance
(* Optional –
leave out if short
of time)
Appreciate the apparent
motion of stars due to the
movement of the Earth and
be able to use the Parsec as
a unit of distance.
Lesson Activities
Directed study &
references.
A2 book p 294-296
Risk ratings &
Resources needed
Discuss how energy could be produced in
None.
Sun. Ask students their suggestions.
You will need to book
Discuss basic ideas of Nuclear Fusion & Extension/G+T:
computers with internet
Binding Energy. Emphasise the unstable
Possible Internet research access to do the
nature of many isotopes.
on Fusions & JET (Joint activity.
Show graph of binding energy per
European Torus).
nucleon against atomic no.
Students could look into There are some
the history of ‘cold
animations on Fission
DEMO – Show ICT animation &
fusion’.
& Fusion in the shared
PowerPoint of nuclear fusion.
area (students could
EXERC – Use computer & Internet to
look at virtual Tokamak/JET. Students Students can use laptops watch these to review
their understanding).
can also look at the MMSS pages revise to try activities from
MMSS 16-18 ICT
key ideas about nuclear stability &
binding energy (see references
software, Nuclear Atom,
opposite).
pages 14 – 25
Past papers – June 2000 Q5.
Review the basic idea of Nuclear Fission A2 book p 296-299
None.
& its uses in power stations & nuclear
Questions 19-21
weapons.
Worksheets
Optional video on
2
Summary:
Q22-24
Nuclear Power.
Discuss E=mc & Mass defect.
Past papers – June 2003
Show students how to work out basic
Q3, June 2002 Q5,
problems involving nuclear fission.
Specimen Q3
Past paper questions.
VIDEO: Nuclear Physics
Discuss key features of video.
Discuss motion of stars (show diagrams
A2 book p 301-303
None.
or photos to illustrate).
Questions 25-26
Discuss Parallax (demo with pencil) and
If there is time, discuss
how it is used to find distance using the
Night-time activity: Get
other possible ways to
students to look at
measure distances.
formula: d = r/. Define the Parsec.
constellations,
eg
Orion,
VIDEO: Starlight) (20 mins)
Try basic problems on working out stellar and try to determine
differences in colours of
distance using parallax (try Q25+26)
stars.
Lesson
11
Content
Learning Outcomes
Lesson Activities
Stellar
Luminosities
Recognise & use a simple
Hertzsprung-Russell
diagram to relate luminosity
& temperature for Main
sequence stars.
Read p304 and look at information on
stars in Orion.
Discuss main types of stars (OBAFGKM)
& features of each spectral type.
Emphasise the link between colour and
temperature of a star.
Look at the Hertzsprung-Russell (HR)
diagram and main groups (use OHP
sheets or PowerPoint show on Stars).
ACTIVITY 17 – Plot a log graph to
construct a HR diagram. Get students
to identify groups of stars on diagram
Questions.
Discuss Gravity and Forces in space. Ask
students to guess what factors affect the
force between 2 masses:
F = Gm1m2/r2
Sample problems & Past Paper Questions
Compare Electric & Gravitational fields.
Derive the expression: g = GM/r2
Use the OHP sheet to highlight
similarities & differences.
Activity 18 – Calculating F using a
spreadsheet (do with a calculator or
leave out if short of time).
Questions.
Discuss the role of gravity in orbits
(centripetal force). Derive equation:
M = v2r/G = 42r3/T2G.
Sample problems & Questions.
Discuss Binary Stars and use of Doppler
Shift to calculate v and M.
Past papers – June 2001 Q4.
Use log scales on graphs.
12+
13+
Gravitation
Orbits &
Satellites
Appreciate the factors
affecting the force between
2 masses and recall & use
the expression:
F = Gm1m2/r2
Derive & Use the
expression g = GM/r2 for
gravitational field strength.
Appreciate similarities
between electric and
gravitational fields.
Apply gravitation to orbits
of stars, planets & satellites.
Directed study &
references.
A2 book p 303-308
Questions 27-29
Worksheets
Risk ratings &
Resources needed
Graph paper only.
A2 book p 308-312
Questions 30-32
Worksheets
None.
You may want to book
laptops or computer
room for Activity 18.
Activity 18 could also be
done for homework. Key
skills IT4b
Past papers – June 2004
Q2, June 2003 Q2, June
2001 Q4
A2 book p 312-316
Questions 33-37
Worksheets
There are some ICT
simulations on Star
Life’ and the H-R
diagram to show, or get
students to watch.
If time, you could show
the video ‘The Big G’
about Gravitation.
None.
Students can try the
ICT animation ‘Gravity
Game’ (good fun!)
Lesson
Content
Learning Outcomes
Lesson Activities
14
Star Formation
& Gas Laws
Recall & use the expression
PV = nRT for an ideal gas.
Understand the concepts of
Absolute Zero & Internal
Energy, using the Kinetic
Theory.
15
Ideal Gases
Relate properties of a gas to
the motion of particles - not
necessary to know the
formula: PV=Nm<c2>/3
Recall assumptions of ideal
gases.
Briefly discuss how stars form from gas
clouds in the ISM (p317-318).
Review basic Gas Laws from Y10/11
Chemistry (Boyle’s Law, Charles’s Law,
Pressure Law). Combine them:
PV/T = constant = nR .
Define Mole, Avagadro number, Gas
Constant & Absolute Zero.
Sample questions.
Past papers – June 2002 Q4, June 2001
Q5
Ask students how they would model an
ideal gas (discussion).
State assumptions of Ideal Gases (list).
Derive formula: PV=Nm<c2>/3.
Sample problems & Questions.
DEMO: ICT simulation (JAVA) of
particles in a box.
Discuss links between pressure &
density. State formula: P=<c2>/3.
Discuss Kinetic Theory and how it
applies through Boltzman constant and
r.m.s. speed distribution. State formula:
Mean KE = 3kT/2 = 3RT/2NA .
Questions. & Past paper problems.
Read p328-329 (Making Stars)
Summary of Electric & Gravitational
field strength & potential (Add sheets 2).
Star Formation & Evolution (Add. sheet
3).
Read section in book and attempt
questions 46, 47, 48.
Review answers & Discuss ideas.
16
17
Pressure,
Particles &
Kinetic Theory
Gravitational
Potential &
Wells
Derive & Use other
formulae based on the
kinetic theory and the gas
laws.
Appreciate role of kinetic
theory & gravitation in star
formation.
Relate ideas about Electric
and Gravitational field
strength and potential to star
formation & nuclear fusion.
Directed study &
references.
A2 book p 317-321
Questions 38-39
Worksheets
Risk ratings &
Resources needed
None. Although you
could use the standard
apparatus to
demonstrate Boyle’s &
Charles’s Laws if
desired. You could also
demonstrate Boyle’s
Law with the ICT A2
Salters Physics virtual
experiment.
A2 book p 321-324
Laptop & Projector
Worksheets
Students could learn
derivation for a test!
A2 book p 324-327
Questions 40-45
None.
Worksheets
A2 book p 328-330
Questions 46-48
Finish questions from
Additional sheets 2+3.
Activity 23 (Star
Formation poster) could
be set as a homework.
None.
Lesson
18+
19+
20
Content
Learning Outcomes
Lesson Activities
Stellar
Evolution
Know about the evolution of
main sequence stars of
similar mass to the Sun &
much larger.
Estimate main sequence
lifetimes of stars.
Discuss how stars progress along the
Main Sequence on HR diagram (p331).
ACTIVITY 25 – End of the Sun.
Students complete table to show
evolution points & physical properties
of stars.
Discuss the main stages in stellar
evolution and the fate of massive stars
(supernovae & core contraction).
Questions 49-52
Ask students to contribute ideas about
what a ‘Black Hole’ is and how we know.
Discuss end states of massive stars –
Neutron Stars & Black Holes.
VIDEO: Black Holes (Equinox).
Read Additional Sheets 4+5. Discuss
how to use gravitation equations to work
out Schwartzschild radius for a 1 solar
mass black hole.
Questions.
Recap of the main ideas of Cosmology
and the work of Hubble & Einstein
(Some work covered in Y11). Possible
opportunity to address the ideas & beliefs
of other cultures/religions. Read p340341 in A2 textbook.
DEMO: Activity 30 - Big Bang
(simulations using expanding balloon,
elastic band, etc). Discuss main features.
VIDEO: Rubber Universe (GHU)
Make notes on the key ideas of the Big
Bang model of the universe.
Highlight uncertainties in the Hubble
constant.
Neutron Stars &
Black Holes
Cosmology &
Big Bang
Theory
Treat properties of neutron
stars & black holes
mathematically.
Appreciate that both can be
formed from the remains of
massive stars.
Be aware of the
contributions of Einstein &
Hubble to cosmology.
Know that recession of
distant galaxies implies
universal expansion.
Directed study &
references.
A2 book p 330-336
Questions 49-52
Risk ratings &
Resources needed
None.
Activity 26 (Fusion in
Stars) could also be set.
Worksheets
A2 book p 337-339
Questions 53-55
Research possible star
systems that may house
Black Holes.
Activity 28 (cartoon
sketches) could be set as
long-running homework.
Worksheets
A2 book p 340-342
Extension/G+T:
Research about Hubble
Constant (current
values?).
You could show some
ICT animations, such as
the ‘Tim & Moby’ clip.
VCR + TV
Elastic band, balloon,
etc.
VCR + TV (Selection
of other videos
available if desired).
Lesson
Content
Learning Outcomes
21
Hubble Constant Relate Redshift to the
distance of galaxies.
Recognise & use formula
z = / = f/f = v/c
z = Hod/c for a moving
source of EM waves at
cosmological distances.
22
Big Bang proof
&
Nucleosynthesis
23+
End of Universe
& Critical
Density
24*
Summary
(* Optional –
leave out of
short on time)
Lesson Activities
Recap Doppler effect and link nto
Redshift, z : z = / = f/f = v/c.
Discuss other uses of Doppler shift in
astrophysics (planetary rotation, etc).
ACTIVITY 29 – Redshift. Use the
CLEA Hubble software to carry out a
simulated sky survey.
Discuss Hubble’s Law: z = Hod/c.
Show how Ho is used to find the age of
the universe.
Past papers- June 2002 Q2, June 2003
Q4. June 2001 Q4
Be aware of observational
Discuss Steady State Theory and proof of
evidence that supports the
Big Bang (CMBR). Read p346 - 351.
Big Bang & Steady State
DEMO: Computer CD-ROM
theories.
animations of stages in the Big Bang.
Know that main stages in
Activity 32 - (Matter in the Universe).
the history of the universe,
Label diagrams. Discuss main stages of
beginning at the Big Bang.
the Big Bang & misconceptions.
Be aware of the controversy Ask students to recall the possible fates
over the age & fate of the
of the Universe & causes (graph).
universe, related to the
Discuss role of Critical Density (c) and
value of the Hubble
Dark Matter: c =3Ho2/8G.
Constant and the existence
Read Additional sheet 6. Questions.
of Dark Matter.
Summary of topic
Past paper – June 2001 Q6, June 2000
Q6
Summary of key ideas about Summary of main work covered in topic.
star formation & cosmology ACTIVITY 36 – Spot the Mistake.
covered in the topic.
Activity 38 – In the Beginning. This
poem can be used as a Literacy exercise
Revision questions (self-assess: at end
of book).
Discuss synoptic Cosmology questions.
Directed study &
references.
A2 book p 342-346
Questions 56-57
Risk ratings &
Resources needed
Use computers or
laptops that have the
CLEA software
Show the ICT animations installed. GHU has
‘Redshift & Doppler’
copies on disks if
(excellent summary of all required.
the key facts) &
‘Redshift’ (looks at
spectra and effects of
motion upon them).
A2 book p 347-354
Questions 58-67
Laptop + Projector.
CD-ROM’s on Space.
A2 book p 361-372
Questions 68-69
Activity 33 – Discussions
about consequences of
stronger gravity. Key
skills C5a.
None.
Students could use the
Internet to look at the
Java simulations on
dark matter loisted
under Activity 35.
A2 book p 370-376
Questions 70-78
Key skills C2b (activity
36)
Revise for test.
None.
Lesson
25
Content
Learning Outcomes
Lesson Activities
TEST
Assess students’
understanding of the work
covered in the topic.
TEST – REACH FOR THE STARS (55
minutes).
Directed study &
references.
None
Risk ratings &
Resources needed
None