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Learn how stellar parallax uses Earth's orbit and apparent angular shift to calculate a star's distance in parsecs for IB Physics SL and HL exams accurately.
Read the answerCompare nuclear fusion and fission in IB Physics through binding energy, mass defect, reaction conditions, chain reactions, products, waste, and stars.
Learn how astronomical units, light-years, and parsecs differ, how to convert between them, and how stellar parallax is tested in IB Physics E.5 exams.
Learn how to use the Stefan-Boltzmann law to calculate a star's radius from luminosity and absolute surface temperature in IB Physics exam questions.
Learn Newton's three laws of motion for IB Physics, including inertia, resultant force, momentum, action-reaction pairs, and exam applications.
Learn why impulse equals change in momentum, calculate it from force-time data, and avoid common errors in IB Physics A.2 questions at SL and HL.
Learn how stellar mass controls core temperature, fusion rate, lifetime, and whether a star becomes a white dwarf, neutron star, or black hole in IB Physics.
Learn how to read an HR diagram's axes, locate main-sequence stars, giants and white dwarfs, and infer temperature, luminosity and radius in IB Physics.
Learn how elastic and inelastic collisions differ through momentum, kinetic energy, equations, worked examples, and IB Physics exam technique for A.2.
Learn where the main sequence, red giants, supergiants, and white dwarfs appear on an HR diagram and what their positions reveal for IB Physics exams.
Learn how mass differs from weight in IB Physics, including units, scalar and vector properties, gravitational field strength, and exam calculations clearly.
Learn how gravity, thermal pressure, radiation pressure, and nuclear fusion maintain hydrostatic equilibrium and keep a main-sequence star stable.
Learn the IB Physics method for explosions: define the system, choose signs, conserve vector momentum, calculate velocity, and check energy correctly.
Learn why nuclear fusion powers stars, how mass defect releases energy, and how gravity, temperature and density sustain stellar equilibrium.
Learn why fusion needs extremely high temperature and density, how stellar gravity confines plasma, and what IB Physics exam answers should include clearly.
Learn how Sankey diagrams represent energy transfers, efficiency and dissipated energy in IB Physics A.3, with a worked example for exam questions.
Understand why nuclear waste is difficult to manage, including radiation, long half-lives, heat, transport, storage, cost, and disposal in IB Physics.
Learn what moment of inertia means, how mass distribution and the rotation axis affect it, and how to calculate it for IB Physics HL exams.
Learn to calculate fission energy from mass defect using mass and energy equivalence, atomic masses, MeV conversion, and a uranium-235 example.
Learn what angular momentum means, why zero resultant external torque conserves it, and how to apply the principle in IB Physics HL exam questions.
Learn what angular impulse means in IB Physics HL, how torque changes angular momentum, and how to calculate it from torque versus time graph data.
Learn the roles of control rods, moderators, heat exchangers and shielding in an IB Physics nuclear power plant, with key exam errors corrected.
Learn how nuclear fission splits heavy nuclei, releases energy and neutrons, sustains chain reactions, and is safely controlled in IB Physics reactors.
Learn how neutron-induced fission sustains a controlled chain reaction in a reactor, and how moderators and control rods regulate reactor power safely.
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