📚 IB AQA Physics: High-Frequency Topics Summary | IB AQA 物理高频考点总结
Mastering IB Physics requires not only understanding concepts but also knowing which topics appear most frequently under the AQA-style assessment framework. This revision guide summarises high-yield areas across Mechanics, Thermal Physics, Waves, Electricity, Fields, Quantum and Nuclear Physics, and provides bilingual explanations to strengthen your exam readiness.
攻克 IB 物理不仅需要理解概念，还要熟悉在 AQA 风格的评估框架下哪些主题最常出现。这篇复习指南总结了力学、热学、波动、电学、场、量子与核物理等领域的高频考点，并提供中英双语解释，以强化你的备考能力。
1. Measurements and Uncertainties | 测量与不确定性
Every IB Physics paper demands precise handling of uncertainties. You must report measured values with absolute uncertainties (±) and combine them correctly in calculations.
每一张 IB 物理试卷都要求严谨处理不确定度。你需要以绝对不确定度（±）报告测量值，并在计算中正确合成它们。
For example, if a length is measured as (5.0 ± 0.1) cm and width as (3.0 ± 0.1) cm, the area’s fractional uncertainty adds: ΔA/A = Δl/l + Δw/w, giving an absolute uncertainty of about 0.65 cm².
例如，若长度测量值为 (5.0 ± 0.1) cm，宽度为 (3.0 ± 0.1) cm，面积的相对不确定度相加：ΔA/A = Δl/l + Δw/w，得出绝对不确定度约为 0.65 cm²。
Remember: for addition/subtraction, add absolute uncertainties; for multiplication/division, add relative (or percentage) uncertainties. Also express final answers to a sensible number of significant figures.
记住：加减运算时，绝对不确定度直接相加；乘除运算时，相对（或百分比）不确定度相加。最终答案应保留合理的有效数字位数。
2. Mechanics | 力学
Kinematics equations, Newton’s laws, momentum, energy conservation, and projectile motion appear repeatedly in IB exams. Core equations for uniform acceleration include:
运动学方程、牛顿定律、动量、能量守恒以及抛体运动在 IB 考试中反复出现。匀加速运动的核心公式有：
v = u + at
s = ut + ½ at²
v² = u² + 2as
Momentum is conserved in isolated systems. Impulse (FΔt) equals change in momentum (Δp). In collisions, distinguish between elastic (kinetic energy conserved) and inelastic cases.
动量在孤立系统中守恒。冲量 (FΔt) 等于动量变化量 (Δp)。在碰撞中，要区分弹性碰撞（动能守恒）和非弹性碰撞。
Energy conservation forms the backbone of problem-solving: initial total energy = final total energy, including kinetic, gravitational potential (mgh) and elastic potential (½ kx²).
能量守恒是解题的基础：初始总能量 = 末态总能量，包括动能、重力势能 (mgh) 和弹性势能 (½ kx²)。
3. Thermal Physics | 热学
Topics such as temperature, heat capacity, specific latent heat, and ideal gas behaviour are guaranteed marks if you recall the definitions precisely.
温度、热容、比潜热以及理想气体行为等主题，如果能精准记住定义，就等于拿到了必得分。
The specific heat capacity equation Q = mcΔθ and latent heat equation Q = mL are fundamental. Don’t confuse the mean kinetic energy of gas particles (proportional to absolute temperature) with internal energy, which also includes potential energy.
比热容方程 Q = mcΔθ 和潜热方程 Q = mL 是基础。不要混淆气体分子的平均动能（与绝对温度成正比）与内能，内能还包括分子势能。
Ideal gas law pV = nRT and the molecular form pV = NkBT link macroscopic variables. An adiabatic change (pVγ = constant) occurs without heat exchange; an isothermal change keeps temperature constant.
理想气体状态方程 pV = nRT 及其分子形式 pV = NkBT 连接了宏观量。绝热变化 (pVγ = 常数) 没有热交换；等温变化则保持温度不变。
4. Wave Phenomena | 波动
You need a clear picture of transverse vs longitudinal waves, superposition, interference, diffraction, and standing waves. The wave equation v = f λ is essential.
你需要清晰理解横波与纵波、叠加、干涉、衍射以及驻波。波动方程 v = f λ 至关重要。
Young’s double-slit experiment confirms the wave nature of light: fringe spacing Δx = λD/d. Constructive interference occurs when path difference = nλ; destructive when path difference = (n+½)λ.
杨氏双缝实验证实了光的波动性：条纹间距 Δx = λD/d。当光程差等于 nλ 时发生相长干涉；等于 (n+½)λ 时发生相消干涉。
Be careful with single-slit diffraction: the first minimum occurs at a sin θ = λ. Also, standing waves in pipes and strings produce harmonic frequencies: fn = nv/(2L) for strings open/closed at both ends.
注意单缝衍射：第一级极小出现在 a sin θ = λ 处。此外，管中和弦上的驻波产生谐频：两端开放（或固定）的弦，频率 fn = nv/(2L)。
5. Electricity and Magnetism Fundamentals | 电与磁基础
Ohm’s law (V = IR), resistivity (R = ρL/A), power (P = IV = I²R = V²/R), and Kirchhoff’s laws form the circuit analysis toolkit. Always consider internal resistance r when drawing a cell: terminal p.d. = ε − Ir.
欧姆定律 (V = IR)、电阻率 (R = ρL/A)、功率 (P = IV = I²R = V²/R) 和基尔霍夫定律构成了电路分析的工具箱。处理电池时务必考虑内阻 r：端电压 = ε − Ir。
Magnetic fields exert force on moving charges: F = qvB sin θ (for a single charge) and F = BIL sin θ (for a current-carrying wire). Fleming’s left-hand rule helps determine motor effect direction.
磁场对运动电荷施加洛伦兹力：单个电荷 F = qvB sin θ，载流导线 F = BIL sin θ。左手定则用于判定电动机效应的方向。
Electromagnetic induction: Faraday’s law states that induced e.m.f. equals the rate of change of magnetic flux linkage (ε = −N ΔΦ/Δt). Lenz’s law gives the direction of induced current.
电磁感应：法拉第定律指出，感应电动势等于磁通链变化率的负值 (ε = −N ΔΦ/Δt)。楞次定律给出感应电流的方向。
6. Circular Motion and Gravitation | 圆周运动与引力
An object in uniform circular motion experiences a centripetal acceleration a = v²/r = ω²r. The centripetal force F = mv²/r = mω²r is always directed towards the centre.
做匀速圆周运动的物体有向心加速度 a = v²/r = ω²r。向心力 F = mv²/r = mω²r 始终指向圆心。
Newton’s law of gravitation: F = Gm₁m₂/r². Gravitational field strength g = F/m. At the surface of a planet, g = GM/r². Satellite motion links orbital speed and period: v = √(GM/r), T² ∝ r³ (Kepler’s third law).
牛顿万有引力定律：F = Gm₁m₂/r²。引力场强度 g = F/m。行星表面处 g = GM/r²。卫星运动将轨道速度和周期联系起来：v = √(GM/r)，T² ∝ r³（开普勒第三定律）。
7. Atomic, Nuclear and Particle Physics | 原子、核与粒子物理
You must be comfortable with atomic energy levels, photon emission/absorption (E = hf = hc/λ), and the photoelectric effect: hf = Φ + Ek max.
你须熟悉原子能级、光子的发射与吸收 (E = hf = hc/λ) 以及光电效应：hf = Φ + Ek max。
Nuclear decay: alpha (⁴₂He), beta-minus (electron, n → p + e⁻ + ν̄e), beta-plus (positron, p → n + e⁺ + νe), gamma. Decay equations must balance mass number A and atomic number Z.
核衰变：α 衰变 (⁴₂He)、β⁻ 衰变 (电子，n → p + e⁻ + ν̄e)、β⁺ 衰变 (正电子，p → n + e⁺ + νe) 和 γ 衰变。衰变方程必须满足质量数 A 和原子序数 Z 守恒。
The half-life T½ = ln2/λ links decay constant λ and exponential decay N = N₀ e−λt. Binding energy per nucleon is a key graph, peaking around iron-56.
半衰期 T½ = ln2/λ 连接衰变常数 λ 与指数衰减律 N = N₀ e−λt。比结合能曲线至关重要，其峰值在铁-56 附近。
8. Energy Production | 能源生产
IB expects you to discuss energy sources, power generation efficiency, and environmental impact. Know the Sankey diagram for energy transfer and calculate efficiency: η = (useful output / total input) × 100%.
IB 要求你能讨论能源、发电效率及环境影响。要会看懂桑基能量流向图，并计算效率：η =（有用输出 / 总输入）× 100%。
Solar power (photovoltaic cells), wind turbines, hydroelectric, fossil fuels, nuclear fission, and nuclear fusion are all potential exam contexts. For fossil fuel, the energy density and specific energy are typical comparison values.
太阳能（光伏电池）、风力发电机、水力发电、化石燃料、核裂变和核聚变都可能成为考试情境。对于化石燃料，能量密度和比能量是常见的比较参数。
In nuclear fission, a neutron induces uranium-235 to split, releasing energy and more neutrons. A chain reaction requires a critical mass. Moderator (e.g., water) slows neutrons; control rods absorb them.
在核裂变中，中子引发铀-235 分裂，释放能量和更多中子。链式反应需要临界质量。慢化剂（如水）减慢中子速度，控制棒则吸收中子。
9. Quantum Physics and Nuclear Physics (HL) | 量子物理与核物理（HL 扩展）
Higher Level candidates must tackle the Bohr model, wave functions, Heisenberg uncertainty principle, and binding energy calculations in more depth. The De Broglie wavelength λ = h/p connects wave and particle behaviour.
高级水平考生需深入掌握玻尔模型、波函数、海森堡不确定性原理以及结合能的更深入计算。德布罗意波 λ = h/p 将波动性和粒子性联系起来。
The uncertainty principle: ΔxΔp ≥ h/(4π) or ΔEΔt ≥ h/(4π). You should explain the confinement of particles inside a nucleus or the width of spectral lines.
不确定性原理：ΔxΔp ≥ h/(4π) 或 ΔEΔt ≥ h/(4π)。你需要能解释原子核内粒子的束缚或光谱线的宽度。
Nuclear fusion in stars requires high temperature to overcome Coulomb repulsion. Binding energy per nucleon differences explain fusion up to iron and fission beyond it.
恒星中的核聚变需要高温来克服库仑斥力。比结合能随质量数的差异解释了在铁之前发生的聚变和铁之后的裂变。
10. Exam Strategy and Common Pitfalls | 考试策略与常见失分点
Always show your working clearly: state the principle (e.g., conservation of energy), substitute values with units, and present the final answer to the correct significant figures. Many marks are lost through omission of units.
务必清晰展示计算步骤：先写出原理（如能量守恒），代入带单位的数值，最后给出正确有效数字的答案。许多失分源于遗漏单位。
When defining terms, use precise wording. For instance, ‘electric field strength’ is force per unit positive charge, not just ‘force per charge’. ‘Half-life’ is the time for half the radioactive nuclei in a sample to decay.
定义术语时要用词精确。例如，“电场强度”是单位正电荷所受的力，而非简单的“力除以电荷”。“半衰期”是样本中一半放射性核衰变所需的时间。
For long-answer questions on energy production or particle physics, structure your response: state the science, apply to context, and if required, evaluate benefits and drawbacks. Use labelled diagrams where helpful.
对于能源生产或粒子物理的长答题，要梳理好结构：陈述科学原理、联系具体情境，若有必要，评价优点和缺点。合适时借助有标注的示意图。
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