Survey
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
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 / 4d2 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 / 4d2 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 = 42r3/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 =3Ho2/8G. 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