OCR A level Physics: Chapter 20 Cosmology (Big Bang) is apart of the Module 5: Newtonian world and Astrophysics. All presentations come with worked examples, solutions and homeworks. 20.1 Astronomical Distances 20.2 The Doppler Effect 20.3 Hubble’s Law 20.4 The Big-bang Theory 20.5 Evolution of the Universe Astronomical distances: light-years, parsec, astronomical unit Astronomical angles - degree, arcminute, arcsecond Parallax Angle The definition of the Doppler effect Changes in pitch of sound waves due to relative motion Absorption spectra and electron energy levels Red-shift and blue-shift absorption spectra The Doppler equation The condition for velocity for the Doppler equation The Cosmological Principle Hubble’s Observations Hubble’s Law Hubble’s constant and the gradient of a graph Converting between km s-1 Mpc-1 into s-1 The expanding Universe model. Georges Lemaître’s Theory Evidence for the Big Bang Model Hubble’s Law (expanding Universe) Microwave Background Radiation Source of the Microwave Background Radiation Hubble’s constant and the age of the Universe The evolution of the Universe from the Big-bang to 13.7 billion years later The composition of the Universe Experimental evidence for dark matter Experimental evidence for dark energy

OCR A level Physics: Chapter 19 Stars is apart of the Module 5: Newtonian world and Astrophysics. All presentations come with worked examples, solutions and homeworks. 19.1 Objects in the Universe 19.2 Life Cycles of Stars 19.3 Hertzsprung-Russell Diagram 19.4 Energy Levels in Atoms 19.5 Spectra 19.6 Analysing Starlight 19.7 Stellar Luminosity The size of astronomical objects: Universe, Galaxies, Solar systems, Stars, Planets, Planetary satellites, Comets, Artificial planetary satellites Comparing planets and comets The birth of stars Stars in equilibrium during the main sequence Calculating mass in kg from solar mass Life cycle of stars with a mass between 0.5 and 10 solar masses Life cycle of stars with a mass above 10 solar masses Pauli exclusion principle and electron degeneracy pressure Red giants and white dwarfs The Chandrasekhar limit Red supergiants to black holes and neutron stars Stellar nucleosynthesis Definition of luminosity Usual axis choice of a HR diagram. Identifying the positions of the main sequence, white dwarfs, red giants, and red supergiants. Description of how stellar evolution is shown in a Hertzsprung-Russell diagram Atoms have different electron arrangements Ground state energy Bound electron states being negative Converting between joules and electronvolts Calculating the change of energy between energy states Calculating a photon’s frequency and wavelength The electromagnetic spectrum and wavelengths Definition of spectroscopy Electrons and energy levels Continuous spectra Emission spectra from gases Absorption spectra from gases Electromagnetic interference Double slit experiment Path and phase difference Diffraction grating The grating equation Lines per millimeter to grating spacing Maximum order, n Maximum number of maxima The electromagnetic spectrum, frequency/wavelength, and temperature Black body radiation Wein’s displacements law Stefan’s law (Stefan-Boltzmann law)

OCR A level Physics: Gravitational Fields is apart of the Module 5: Newtonian world and Astrophysics. All presentations come with worked examples, solutions and homeworks. 18.1 Gravitational Fields 18.2 Newton’s law of gravitation 18.3 Gravitational field strength for a point mass 18.4 Kepler’s laws 18.5 Satellites 18.6 Gravitational potential 18.7 Gravitational potential energy The terms: eccentricity, aphelion, perihelion, astronomical unit Kepler’s First Law Kepler’s Second Law Kepler’s Third Law Graphs of T^2 against r^3 to determine the gradient (constant of proportionality, k). Equating (4π)^2/𝐺𝑀 to the gradient (constant of proportionality, k) Key features of geostationary and low polar orbit satellites Conditions for stable orbits for satellites Applying Kepler’s laws to the orbits of satellites Radial and uniformed field Definition of gravitational potential energy Deriving escape velocity Force-Distance graphs for gravitational fields Center of mass and treating spherical objects as point masses Gravitational fields Definition of gravitational potential Applying the gravitational potential equation Graph of gravitational potential against distance (V against r) Combining gravitational potentials from more than one mass

All resources for P8 Global Challenges GCSE OCR Physics Gateway 9-1. Triple and combined (Higher and Foundation) is covered in this material. Average speeds of walking, running, cycling, cars, trains, wind, sound, and light. The speed equation The acceleration equation Explaining average speed camera Explaining instantaneous speed camera Estimating everyday accelerations Calculating speed from rotation speed and circumference of wheels Converting from miles per hour to meters per second Reaction time definition Factors that increase reaction time Simple reaction time experiment Thinking distance Rearranging equations Speed equation (Final velocity)2 – (Initial velocity)2 = 2 x Acceleration x Distance v2 – u2 = 2 a s Factors affecting braking distance Total stopping distances Calculating area of a velocity-time graph for displacement (distance traveled). Rearranging equations MOT testing Large accelerations produce large forces. Values of g that cause severe injury or death Road Safety Newton’s First Law and seat belts Crumple zones Force = Mass x Acceleration Acceleration = Change in velocity /Time taken Estimating speed, accelerations and forces involved in large accelerations for everyday road transport. Types of different energy sources Renewable and non-renewable definitions Different uses of energy sources - transport, heating, and generating electricity Advantages and disadvantages of different energy sources Fossil fuels – oil, coal, and natural gas. Nuclear fuel – Uranium Biofuels – wood, biodiesel, and biogas. The sun - solar (PV) panels and solar heating panels Tides Waves Hydroelectricity Wind Geothermal How use of energy resources have changed over time. (Biofuels, Fossil Fuels, Nuclear, Renewable). How energy use has increased (increase population and development of technology) Explain patterns and trends in the use of energy resources. Fossil fuels are finite and will run out at current consumption levels. Structure of the National Grid Step-up and Step-down transformers How transformers increase the efficiency of the National Grid Number of turns and potential difference Current and potential difference in primary and secondary coils Domestic Electrical Supply being 230 V, AC at 50 Hz. Direct potential difference and alternating potential difference. Reasons for insulation on wires. Potential Difference between different conductors. Function of the earth conductor. Double insulation and no earth wire. Reasons the live wire is dangerous. Reasons why live to earth is dangerous. Key facts about the Big-Bang model Cosmic Microwave Background (CMB, CMBR) Doppler Red shift of light from stars in galaxies Hubble’s evidence of absorption spectra being red shifted Structure of the solar system Nuclear Fusion Evolution of large stars Evolution of Sun like stars Gravitational force and force from nuclear fusion Natural Satellites Geostationary Satellites Low Polar Orbit Satellites Speed is constant and velocity is changing in stable orbits. Changing speed and radius Gravitational force, acceleration, and speed. Plotting data and describing relationships All objects emit electromagnetic radiation Describe how changing temperature changes frequency, wavelength, and intensity of the radiation produced. Explain why objects change temperature by absorbing and emitting radiation. Explain why the temperature of the Earth changes due to greenhouse gases in the atmosphere. S and P waves Structure of the Earth Reflection, absorption, and refraction of waves Sonar to map the ocean floor