Detailed notes on The particulate nature of matter for IB DP Physics, covering key concepts, explanations, examples, and exam-focused revision points.
B.2 Greenhouse effect — IB Physics SL Study Notes (Theme B: The Particulate Nature of Matter)
How Earth stays warm: black-body radiation applied to the Sun and Earth, the solar constant, albedo and emissivity, balancing incoming absorbed sunlight against outgoing radiation to find Earth's equilibrium temperature, and the molecular mechanism by which greenhouse gases absorb and re-emit infrared radiation — including the enhanced greenhouse effect.
At a glance
The Sun and Earth both radiate like black bodies. The hot Sun (≈5800K) peaks in the visible; the cool Earth (≈255K) peaks in the infrared.
Solar constantS≈1361W m−2 — the mean intensity of sunlight arriving at the top of Earth's atmosphere at Earth's distance from the Sun.
Albedoα=power incidentpower reflected (no units, 0–1). Earth's average albedo ≈0.30, so about 30% is reflected and 70% absorbed.
Emissivityε=power radiated by a black body at the same temperaturepower radiated by a surface (0–1). A perfect black body has ε=1.
Energy balance: at equilibrium, absorbed solar power =S(1−α)πR2 equals radiated power =εσ4πR2T4. The disc absorbs (πR2) but the whole sphere emits (4πR2) — hence a factor of 4.
Equilibrium temperatureT=[4εσS(1−α)]1/4. For α=0.30 and ε=1 this gives T≈255K (−18∘C).
Greenhouse gases — carbon dioxide CO2, water vapour H2O, methane CH4, nitrous oxide N2O — absorb outgoing infrared at the natural (resonant) frequencies of their molecular bond vibrations and re-emit it in all directions, warming the surface.
Enhanced greenhouse effect: rising greenhouse-gas concentrations absorb more outgoing infrared, raising the surface temperature above its natural value (σ=5.67×10−8W m−2K−4).
What you’ll learn
Mapped to the 100452 subject guide (2025-onwards).
Apply the idea of black-body radiation to explain why the Sun emits mainly visible light while the Earth emits mainly infrared radiation.
Define and use the solar constant, albedo and emissivity, including the relationship albedo = total reflected power ÷ total incident power.
Set up the energy balance for a planet, treating the absorbing cross-section (πR²) and emitting surface (4πR²) correctly, and derive the equilibrium temperature.
Calculate a planet's equilibrium temperature from the solar constant, albedo and emissivity, and explain qualitatively how changes in albedo or emissivity change it.
Describe the molecular mechanism of the greenhouse effect and distinguish the natural greenhouse effect from the enhanced greenhouse effect.
Black-body radiation: the Sun and the Earth
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Everything radiates; hotter bodies radiate more and at shorter wavelengths — Sun in the visible, Earth in the infrared.
The greenhouse effect is really a story about black-body radiation (from B.1), so we begin there.
A black body is an idealised object that absorbs all the radiation falling on it and, at a given temperature, is the best possible emitter. Any warm object glows with a continuous spread of wavelengths — a black-body spectrum — and two rules govern that spectrum:
Hotter bodies radiate more power. The intensity (power per unit area) follows the Stefan–Boltzmann law, I=σT4, where σ=5.67×10−8W m−2K−4. Because of the fourth power, a small rise in temperature is a large rise in power.
Hotter bodies radiate at shorter wavelengths. The peak of the spectrum shifts to shorter wavelength as temperature rises (Wien's displacement law, B.1).
Now apply this to two very different objects:
Body
Surface temperature
Where its radiation peaks
So it emits mainly…
The Sun
≈5800K
≈500nm
visible light
The Earth
≈255K
≈10μm
infrared radiation
This single contrast is the key to the whole topic. Sunlight arrives as visible light, most of which passes straight through the atmosphere and warms the ground. The warm ground then radiates energy back as infrared. Greenhouse gases are almost transparent to incoming visible light but strongly absorb outgoing infrared — so the two motions of energy behave completely differently, and that asymmetry is what keeps the surface warm.
The hot Sun radiates mainly visible light; the cool Earth radiates mainly infrared. Greenhouse gases let the visible in but absorb the outgoing infrared — the origin of the greenhouse effect.
A black body absorbs all incident radiation and is the best emitter at its temperature.
Stefan–Boltzmann law: I = σT⁴, so power rises steeply with temperature.
Sun (≈5800 K) peaks in the visible; Earth (≈255 K) peaks in the infrared.
The solar constant and the geometry of intercepting sunlight
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S ≈ 1361 W m⁻² arrives on a disc of area πR², but the planet radiates from its whole surface 4πR².
The solar constantS is the mean intensity (power per unit area) of solar radiation arriving at the top of Earth's atmosphere, measured on a surface perpendicular to the Sun's rays at Earth's average distance:
S≈1361W m−2
How much power does the whole Earth intercept? Not the intensity times the surface area — the Sun's rays are (very nearly) parallel, so the Earth intercepts sunlight as though it were a flat disc facing the Sun. The area of that disc (the cross-section) is
Aintercept=πR2
where R is Earth's radius. So the total incoming solar power is
Pin=S×πR2.
How much power does the Earth radiate? The Earth radiates from its entire spherical surface (day and night, all directions), whose area is
Aemit=4πR2.
Here is the crucial point that examiners test relentlessly: the planet absorbs over πR2 but emits over 4πR2. The ratio πR24πR2=4 is where the famous factor of 4 comes from. If you spread the intercepted sunlight over the whole surface, the average incoming intensity is only 4S≈340W m−2.
Sunlight is intercepted over the disc-shaped cross-section πR², but the planet radiates from its whole surface 4πR². The 4:1 ratio of these areas is the origin of the factor of 4 in the energy balance.
Solar constant S ≈ 1361 W m⁻² is the incoming intensity at Earth's distance.
Power intercepted = S × πR² (absorbs like a disc, cross-section πR²).
Power radiated is from the whole sphere 4πR² → the factor-of-4 difference.
Albedo and emissivity: how much is reflected, how well it emits
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Albedo is the fraction of sunlight reflected; emissivity compares a real emitter to a perfect black body.
Two dimensionless numbers (each between 0 and 1) turn the black-body idea into real planets.
Albedo α — the fraction of incident radiation a surface reflects:
α=total power incidenttotal power reflected.
It has no units because it is a ratio of powers. A perfect mirror has α=1; a perfect black body has α=0. Earth's average albedo is about 0.30, meaning roughly 30% of incoming sunlight is reflected (by clouds, ice, deserts and the atmosphere) and the remaining 70% is absorbed. That is why the absorbed power carries the factor (1−α):
Pabsorbed=S(1−α)πR2.
Bright surfaces raise the albedo: fresh snow reflects most of the light that hits it (α≈0.8–0.9), whereas the open ocean is dark (α≈0.06). This is why melting ice, by lowering the albedo, is a warming feedback.
Emissivity ε — how good a surface is at radiating, compared with a perfect black body at the same temperature:
ε=power radiated by a black body at the same temperaturepower radiated by the surface.
A perfect black body has ε=1; a shiny, poor emitter has a small ε. Emissivity multiplies the Stefan–Boltzmann law:
Pradiated=εσAT4.
For many planetary calculations the Earth is treated as a near-perfect emitter in the infrared, so ε≈1 unless a question tells you otherwise.
Keeping them straight: albedo is about incoming, reflected radiation; emissivity is about outgoing, radiated radiation. Both are just fractions — no units, never greater than 1.
Albedo α = reflected power ÷ incident power (0–1, no units); Earth ≈ 0.30.
Absorbed power carries the factor (1 − α); 30% reflected means 70% absorbed.
Emissivity ε = surface's radiated power ÷ black-body power at the same T (0–1).
Deriving Earth's equilibrium temperature (energy balance)
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Set absorbed solar power equal to radiated power and solve for T — the whole model in one line.
This is the central derivation of B.2, and it is built from first principles you already have. The idea is simple: if a planet's temperature is steady, the power it absorbs from the Sun must exactly equal the power it radiates back to space. This is the energy balance.
Step 1 — power absorbed. The planet intercepts sunlight over its disc πR2, but only the fraction (1−α) is absorbed:
Pin=S(1−α)πR2.
Step 2 — power radiated. The planet radiates as a (near) black body from its whole surface 4πR2, with emissivity ε and the Stefan–Boltzmann law:
Pout=εσ(4πR2)T4.
Step 3 — balance them. At the equilibrium temperature, Pin=Pout:
S(1−α)πR2=εσ4πR2T4.
Step 4 — the πR2 cancels (this is why the planet's actual size does not matter). Dividing both sides by πR2:
S(1−α)=4εσT4.
Step 5 — solve for T:T=[4εσS(1−α)]1/4
Put the numbers in (S=1361W m−2, α=0.30, ε=1, σ=5.67×10−8):
T=[4(1)(5.67×10−8)1361(1−0.30)]1/4=[2.268×10−7952.7]1/4=(4.20×109)1/4≈255K.
At a steady temperature the absorbed solar power equals the radiated power. Cancelling πR² and solving gives T = [S(1−α)/(4εσ)]^(1/4) ≈ 255 K for Earth.
What the answer tells you.255K=−18∘C — far below freezing. Yet Earth's true average surface temperature is about 288K (+15∘C). The 33∘C difference is exactly what the greenhouse effect provides: without it, the planet would be a frozen ball. The model also shows the levers clearly — a higher albedo lowers T (less energy absorbed), while a lower effective emissivity raises T (energy escapes to space less easily), which is precisely what adding greenhouse gases does.
Equilibrium: absorbed power S(1−α)πR² = radiated power εσ4πR²T⁴.
πR² cancels, leaving S(1−α) = 4εσT⁴, so T = [S(1−α)/(4εσ)]^(1/4).
For α = 0.30, ε = 1: T ≈ 255 K (−18 °C), well below Earth's real 288 K.
Greenhouse-gas molecules absorb outgoing infrared at their resonant vibration frequencies and re-emit it in all directions.
Now the physics that gives the topic its name. The main greenhouse gases in Earth's atmosphere are:
Water vapour (H2O) — the largest natural contributor,
Carbon dioxide (CO2),
Methane (CH4),
Nitrous oxide (N2O).
(Note that CO2 is not the only greenhouse gas — a very common misconception.)
Why these gases and not nitrogen or oxygen? A molecule can absorb infrared only if the vibration of its bonds changes its distribution of charge (its dipole). The simple diatomic molecules N2 and O2 — which make up 99% of the air — cannot do this, so they are transparent to infrared. Greenhouse-gas molecules have bonds that do interact with infrared.
The molecular mechanism, step by step:
Sunlight in. Incoming solar radiation is mostly visible; greenhouse gases barely absorb it, so it passes through the atmosphere and warms the surface.
Infrared out. The warm surface radiates energy back upward as infrared.
Resonant absorption. Each greenhouse-gas molecule has bonds that vibrate at particular natural (resonant) frequencies. When outgoing infrared radiation has a frequency matching one of these natural bond-vibration frequencies, the molecule absorbs that photon and vibrates more energetically — this is resonance.
Re-emission in all directions. The excited molecule quickly re-emits infrared radiation, but in all directions — including back down towards the surface.
Net warming. Because some of the outgoing infrared is returned to the surface instead of escaping to space, the surface receives extra energy and settles at a higher temperature than the bare energy balance predicts.
A greenhouse-gas molecule absorbs outgoing infrared when its frequency matches a natural bond-vibration (resonant) frequency, then re-emits it in all directions — returning some energy to the surface and warming it.
Say it precisely in the exam. Greenhouse gases do not simply "trap heat like a blanket". The correct physics is: they absorb infrared radiation at the natural (resonant) frequencies of their molecular bonds and re-emit it in all directions, so some returns to the surface. Naming that mechanism is what earns the marks.
Main greenhouse gases: H₂O, CO₂, CH₄, N₂O (CO₂ is not the only one).
They absorb outgoing infrared at the resonant frequencies of their bond vibrations.
They re-emit infrared in all directions; some returns to the surface, warming it.
The natural greenhouse effect keeps Earth habitable; the enhanced effect from extra greenhouse gases warms it further.
It is essential to keep two ideas apart.
The natural greenhouse effect is the warming that has always existed because Earth's atmosphere naturally contains water vapour, carbon dioxide and other greenhouse gases. It raises the surface from the bleak 255K predicted by the bare energy balance to a life-friendly ≈288K (+15∘C). Without it, Earth would be frozen and uninhabitable — so the natural greenhouse effect is a good and necessary thing.
The enhanced greenhouse effect is the extra warming caused by rising concentrations of greenhouse gases, largely from human activity — burning fossil fuels (CO2), agriculture and livestock (CH4, N2O) and deforestation. More greenhouse-gas molecules absorb a greater fraction of the outgoing infrared and return more of it to the surface, so:
more greenhouse gas⇒more outgoing infrared absorbed⇒lower effective emissivity to space⇒higher surface temperature.
This shifts the energy balance: to radiate the same total power out to space at a higher opacity, the surface must sit at a higher temperature. The result is global warming and climate change.
Feedbacks amplify it. A warmer surface melts ice, lowering the albedo (dark water absorbs more than bright ice), which warms things further. Warming also increases evaporation, adding more water vapour — itself a greenhouse gas. These positive feedbacks are why a modest forcing can produce a larger response.
International-mindedness. Because the atmosphere is shared, greenhouse-gas emissions in one country affect the whole planet, which is why the physics feeds directly into global agreements on emissions. Understanding the underlying energy balance is what lets scientists quantify how much warming a given rise in CO2 will cause.
Natural greenhouse effect: always present, raises Earth from ~255 K to ~288 K — essential for life.
Enhanced greenhouse effect: extra warming from rising greenhouse-gas concentrations (mostly human).
Positive feedbacks (ice-albedo, extra water vapour) amplify the initial warming.
The Sun (≈5800 K) radiates mainly visible light; the Earth (≈255 K) radiates mainly infrared — greenhouse gases absorb the outgoing infrared.
Solar constant S ≈ 1361 W m⁻²; the planet intercepts power over πR² but radiates over 4πR², giving the factor of 4.
Albedo α = reflected ÷ incident (Earth ≈ 0.30, so 70% absorbed); emissivity ε = radiated power ÷ black-body power at the same temperature.
Energy balance S(1−α)πR² = εσ4πR²T⁴ gives T = [S(1−α)/(4εσ)]^(1/4) ≈ 255 K for Earth.
Greenhouse gases (H₂O, CO₂, CH₄, N₂O) absorb infrared at the resonant frequencies of their bond vibrations and re-emit it in all directions.
The natural greenhouse effect (≈33 °C of warming) is essential for life; the enhanced greenhouse effect from rising gas concentrations causes global warming.
Memorise this
Verbatim phrases, formulae and definitions IB DP mark schemes credit (key for AO1 knowledge marks on Paper 1).
Solar constant S ≈ 1361 W m⁻²; σ = 5.67 × 10⁻⁸ W m⁻² K⁻⁴.
Albedo α = total power reflected ÷ total power incident (no units, 0–1); Earth ≈ 0.30.
Emissivity ε = power radiated by surface ÷ power radiated by a black body at the same T (0–1).
Power absorbed = S(1−α)πR²; power radiated = εσ4πR²T⁴ (disc absorbs, sphere emits → factor of 4).
Equilibrium temperature T = [S(1−α)/(4εσ)]^(1/4); Earth ≈ 255 K (−18 °C).
Greenhouse gases: H₂O, CO₂, CH₄, N₂O — absorb infrared at resonant molecular-vibration frequencies and re-emit in all directions.
Natural greenhouse effect ≈ +33 °C (essential); enhanced greenhouse effect = extra warming from rising greenhouse-gas levels.
Always convert temperatures to KELVIN before using σT⁴.
How it’s examined
B.2 appears across all three papers and links black-body radiation (B.1) to real climate physics. Paper 1A (MCQ): definitions of albedo and emissivity, identifying greenhouse gases, recognising the factor of 4 (average intensity S/4), and reasoning about how a change in albedo or emissivity changes the equilibrium temperature — no calculator, so numbers are chosen to be clean. Paper 1B (data-based): using given values of S, α and ε to estimate an equilibrium temperature, or comparing incoming and outgoing power on an energy-balance diagram. Paper 2: structured questions (3–8 marks) that ask you to show that the equilibrium temperature is a certain value from the energy balance, calculate T for a planet, or describe/explain the molecular mechanism of the greenhouse effect and distinguish the natural from the enhanced effect. Command terms: state, define, calculate, determine, show that, describe, explain, outline. Examiner reports repeatedly flag: forgetting the (1−α) absorbed fraction, using 4πR² for the absorbing area (the factor-of-4 slip), leaving temperatures in °C instead of kelvin, describing greenhouse gases as 'trapping' heat rather than absorbing and re-emitting infrared at resonant frequencies, and confusing the natural with the enhanced greenhouse effect. Always show the energy balance explicitly and quote answers in kelvin with sensible significant figures.
Sources: IB Diploma Programme Physics Guide (first assessment 2025) — Theme B: The particulate nature of matter (B.2 Greenhouse effect); IB Physics Data Booklet (2025) — solar constant, Stefan–Boltzmann constant; IB Physics subject reports and specimen papers (2023–2025). Last reviewed 2026-07-21.
Take this whole topic with you
Step-by-step worked examples — Greenhouse effect
Step-by-step solutions to past-paper-style questions on greenhouse effect, written exactly the way a tutor would explain them at the board.
Question type:
1Calculating a planet's albedo
Getting startedDirect calculation• albedo, AO2
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Question
The total solar power incident on the Earth is about 1.74×1017W, of which about 5.2×1016W is reflected back into space. Calculate the Earth's average albedo. (2 marks)
Step-by-step solution
Step 1
Albedo is the ratio of the total power reflected to the total power incident — a pure number with no units.
α=PincidentPreflected=1.74×10175.2×1016
Step 2
Evaluate the ratio.
α=0.30
Answer
α ≈ 0.30 (about 30% of the incident sunlight is reflected).
Examiner tip
Mark scheme: (1) correct ratio reflected/incident; (2) α ≈ 0.30 with no units. Note that an albedo of 0.30 means 70% is absorbed — that (1−α) fraction is what drives the energy balance.
A patch of ground at 288 K radiates 350 W m⁻². A perfect black body at the same temperature would radiate 390 W m⁻². Calculate the emissivity of the ground. (2 marks)
Step-by-step solution
Step 1
Emissivity is the ratio of the power radiated by the surface to the power radiated by a black body at the same temperature.
ε=Pblack bodyPsurface=390350
Step 2
Evaluate the ratio (no units).
ε=0.90
Answer
ε ≈ 0.90.
Examiner tip
Mark scheme: (1) ratio of surface power to black-body power at the SAME temperature; (2) ε ≈ 0.90, no units. Emissivity is always ≤ 1; a value greater than 1 signals a slip.
3Power the Earth intercepts from the Sun
Getting startedDirect calculation• solar constant, geometry, AO2
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Question
The solar constant is S=1361W m−2 and the Earth's radius is R=6.37×106m. Calculate the total solar power intercepted by the Earth. (3 marks)
Step-by-step solution
Step 1
The Earth intercepts sunlight over its cross-sectional disc, not its whole surface. The area of that disc is πR2.
A=πR2=π(6.37×106)2=1.27×1014m2
Step 2
Multiply the intercepting area by the solar constant (the incoming intensity).
P=S×πR2=1361×1.27×1014
Step 3
Evaluate.
P=1.74×1017W
Answer
P ≈ 1.7 × 10¹⁷ W.
Examiner tip
Mark scheme: (1) use πR² (cross-section, not 4πR²); (2) multiply by S; (3) P ≈ 1.74 × 10¹⁷ W. The single most common error is using the full surface area 4πR² for the intercepted power — sunlight only lands on the disc facing the Sun.
4Earth's equilibrium temperature
Building confidenceMulti-step problem• energy balance, equilibrium temperature, AO2
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Question
Treating the Earth as a black body (ε=1) with albedo α=0.30, and using S=1361W m−2 and σ=5.67×10−8W m−2K−4, calculate the Earth's equilibrium temperature. (4 marks)
Step-by-step solution
Step 1
At equilibrium the absorbed solar power equals the radiated power. The disc absorbs and the sphere emits:
Mark scheme: (1) correct energy balance with (1−α) and the factor of 4; (2) rearrange for T; (3) correct substitution; (4) T ≈ 255 K. This is well below Earth's real 288 K — the 33 °C gap is the natural greenhouse effect.
5Matching infrared frequency to a molecular vibration
Building confidenceWord problem• greenhouse mechanism, resonance, AO2
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Question
Carbon dioxide absorbs infrared radiation strongly at a wavelength of about 15 µm. (a) Calculate the frequency of this radiation (c=3.00×108m s−1). (b) State why CO₂ absorbs radiation at this particular frequency. (3 marks)
Step-by-step solution
Step 1
Use c=fλ to find the frequency, with λ=15μm=15×10−6m.
f=λc=15×10−63.00×108=2.0×1013Hz
Step 2
This infrared frequency matches a natural (resonant) frequency of vibration of the CO₂ molecule's bonds, so the molecule absorbs the radiation and vibrates more energetically (resonance).
Answer
(a) f = 2.0 × 10¹³ Hz; (b) it equals a natural (resonant) frequency of the CO₂ bond vibrations, so the molecule absorbs the infrared.
Examiner tip
Mark scheme: (1) correct use of c = fλ with the wavelength in metres; (2) f ≈ 2.0 × 10¹³ Hz; (3) absorption occurs because the frequency matches a resonant molecular-vibration frequency. Saying the gas 'traps' the radiation earns nothing — name the resonant absorption.
6Infrared radiated by the Earth's surface
Building confidenceDirect calculation• Stefan-Boltzmann, AO2
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Question
The Earth's average surface temperature is 288 K. Treating the surface as a black body (ε=1), calculate the power radiated per square metre. (σ=5.67×10−8W m−2K−4) (3 marks)
Step-by-step solution
Step 1
The power radiated per unit area (intensity) of a black body is given by the Stefan–Boltzmann law I=σT4. Make sure the temperature is in kelvin.
I=σT4=(5.67×10−8)(288)4
Step 2
Evaluate 2884.
2884=6.88×109K4
Step 3
Multiply through.
I=(5.67×10−8)(6.88×109)=390W m−2
Answer
I ≈ 390 W m⁻².
Examiner tip
Mark scheme: (1) use I = σT⁴ with T in kelvin; (2) 288⁴ ≈ 6.88 × 10⁹; (3) I ≈ 390 W m⁻². Forgetting to keep the temperature in kelvin (or trying to raise °C to the fourth power) is the classic slip here.
7Equilibrium temperature with emissivity less than 1
StretchShow that / prove• energy balance, emissivity, AO2, AO3
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Question
A planet has albedo α=0.30 and receives the same solar constant as Earth (S=1361W m−2), but its atmosphere gives it an effective emissivity of only ε=0.90. Show that its equilibrium temperature is about 261 K, and comment on how this compares with the black-body case of 255 K. (4 marks)
Step-by-step solution
Step 1
Start from the rearranged energy balance, now keeping the emissivity in the denominator.
A lower emissivity gives a HIGHER equilibrium temperature (261 K > 255 K), because the surface radiates less efficiently to space and so must be warmer to shed the same power. This is exactly how greenhouse gases warm a planet.
Answer
T ≈ 261 K; lower emissivity → higher temperature than the black-body value of 255 K.
Examiner tip
Mark scheme: (1) ε correctly placed in the denominator; (2) correct substitution; (3) T ≈ 261 K; (4) comment that reducing emissivity raises the temperature. The physical insight — that reduced emissivity to space warms the surface — is the model for the greenhouse effect itself.
If the Earth's albedo rose from 0.30 to 0.40 (with ε=1, S=1361W m−2), calculate the new equilibrium temperature and state, with reasoning, the direction of the change. Explain why the real ice–albedo feedback works in the opposite direction. (5 marks)
Step-by-step solution
Step 1
Use the equilibrium-temperature expression with the new albedo.
A higher albedo means less sunlight absorbed ((1−α) is smaller), so the equilibrium temperature falls from 255 K to about 245 K.
Step 5
The real ice–albedo feedback runs the other way: warming melts bright ice, exposing dark ocean or land which has a lower albedo, so more sunlight is absorbed and the planet warms further — a positive (amplifying) feedback.
Answer
T ≈ 245 K — a higher albedo cools the planet; the ice–albedo feedback instead lowers albedo (melting ice) and amplifies warming.
Examiner tip
Mark scheme: (1) correct expression; (2) substitute α = 0.40; (3) T ≈ 245 K; (4) higher albedo → less absorbed → cooler; (5) ice–albedo feedback lowers albedo and amplifies warming. Linking the calculation to the direction of the feedback is the AO3 discriminator.
Model Answers — Greenhouse effect
High-scoring sample answers for greenhouse effect on the Cambridge IGCSE paper, with examiner-style notes mapping each response to the mark scheme and assessment objectives.
Question 1
2 marks
Q (2 marks). Define albedo and state a typical value for the Earth's average albedo.
Model answer
Albedo is the ratio of the total power (of radiation) reflected by a surface to the total power incident on it:
α=total power incidenttotal power reflected
It is a dimensionless number between 0 and 1. The Earth's average albedo is about 0.30 (roughly 30% of incoming sunlight is reflected).
Why this scores
Why this scores 2/2. (1) albedo = reflected power ÷ incident power (as a ratio); (2) Earth ≈ 0.30. Stating it as a fraction of power (not just 'light bounced off') is what earns the definition mark.
Question 2
2 marks
Q (2 marks). Define emissivity and state its value for a perfect black body.
Model answer
Emissivity is the ratio of the power radiated per unit area by a surface to the power radiated per unit area by a black body at the same temperature:
ε=power radiated by a black body at the same temperaturepower radiated by the surface
It is dimensionless and lies between 0 and 1. A perfect black body has an emissivity of 1.
Why this scores
Why this scores 2/2. (1) emissivity = surface power ÷ black-body power at the same temperature; (2) black body ε = 1. The phrase 'at the same temperature' is essential — omitting it loses the definition mark.
Question 3
3 marks
Q (3 marks). The solar constant is 1361 W m⁻². (a) Explain why the average solar intensity over the Earth's whole surface is one quarter of the solar constant. (b) State this average value.
Model answer
(a) Sunlight is intercepted only over the Earth's cross-sectional disc, of area πR2. However, the Earth radiates from its whole spherical surface, of area 4πR2. Spreading the intercepted power over the full surface therefore divides the intensity by
πR24πR2=4.
(b) Average intensity =4S=41361≈340W m−2.
Why this scores
Why this scores 3/3. (1) intercepting area is the disc πR²; (2) surface area is 4πR², ratio 4; (3) S/4 ≈ 340 W m⁻². The factor of 4 is the ratio of emitting area to absorbing area — a favourite Paper 1 idea.
Question 4
4 marks
Q (4 marks). Name two greenhouse gases and describe how greenhouse gases in the atmosphere warm the Earth's surface.
Model answer
Two greenhouse gases (any of): carbon dioxide (CO₂), water vapour (H₂O), methane (CH₄) or nitrous oxide (N₂O).
Mechanism:
The warm Earth surface radiates energy back into the atmosphere as infrared radiation.
Greenhouse-gas molecules absorb this infrared radiation when its frequency matches the natural (resonant) frequencies of vibration of their molecular bonds.
The molecules then re-emit the infrared radiation in all directions, so some of it is returned downward to the surface.
This extra returning energy raises the surface temperature above the value it would have with no atmosphere.
Why this scores
Why this scores 4/4. (1) two named greenhouse gases; (2) surface emits infrared; (3) greenhouse gases absorb IR at resonant molecular-vibration frequencies; (4) re-emit in all directions, returning some to the surface. Answers that say the gas 'traps' or 'reflects' heat do not earn the mechanism marks.
Question 5
5 marks
Q (5 marks). A planet has an albedo of 0.25 and behaves as a black body (ε=1). The solar intensity at its distance from its star is 1000 W m⁻². Taking σ=5.67×10−8W m−2K−4, calculate its equilibrium temperature.
Model answer
At equilibrium, the absorbed solar power equals the radiated power. The planet absorbs over its cross-section πR2 and emits from its whole surface 4πR2:
Why this scores 5/5. (1) energy balance stated; (2) (1−α) factor and the factor of 4 both present; (3) rearranged correctly for T; (4) correct substitution; (5) T ≈ 240 K. Dropping the (1−α) term or using 4πR² for the absorbing area are the two errors examiners see most.
Question 6
4 marks
Q (4 marks). Distinguish between the natural greenhouse effect and the enhanced greenhouse effect, and state why the natural greenhouse effect is important for life on Earth.
Model answer
The natural greenhouse effect is the warming caused by the greenhouse gases that have always been present in the atmosphere (mainly water vapour and carbon dioxide). It raises the average surface temperature from about 255 K (the value from the bare energy balance) to about 288 K.
This natural warming of roughly 33 °C is essential: without it the Earth's surface would be well below freezing and could not support liquid water or life as we know it.
The enhanced greenhouse effect is the additional warming caused by rising concentrations of greenhouse gases (mostly from human activities such as burning fossil fuels). More greenhouse gas absorbs a greater fraction of the outgoing infrared, raising the surface temperature further and causing global warming.
Why this scores
Why this scores 4/4. (1) natural effect = warming from naturally present greenhouse gases; (2) it raises T from ~255 K to ~288 K and is essential for life; (3) enhanced effect = extra warming from increased concentrations; (4) linked to human activity/global warming. The key distinction is 'always present and beneficial' versus 'extra and harmful'.
Question 7
6 marks
Q (6 marks). By considering the power a planet absorbs from its star and the power it radiates, show that its equilibrium temperature is given by T=[4εσS(1−α)]1/4, defining each symbol.
Model answer
Power absorbed. The planet intercepts starlight over its circular cross-section of area πR2, where R is the planet's radius and S is the solar intensity (solar constant) at its distance. Only the fraction (1−α) is absorbed, where α is the albedo (fraction reflected):
Pin=S(1−α)πR2
Power radiated. The planet radiates from its whole spherical surface of area 4πR2 as a body of emissivityε (0–1) at temperature T, following the Stefan–Boltzmann law (σ=5.67×10−8W m−2K−4):
Pout=εσ(4πR2)T4
Equilibrium. At a steady temperature the absorbed and radiated powers are equal:
S(1−α)πR2=εσ4πR2T4
The factor πR2cancels (so the size of the planet does not matter), leaving:
S(1−α)=4εσT4⇒T=[4εσS(1−α)]1/4(as required).
Why this scores
Why this scores 6/6. (1) absorbing area πR²; (2) (1−α) absorbed fraction; (3) emitting area 4πR²; (4) Stefan–Boltzmann with ε; (5) set P_in = P_out; (6) cancel πR² and rearrange, with symbols defined. The factor of 4 arising from 4πR² ÷ πR² is the crux of the 'show that'.
Question 8
6 marks
Q (6 marks). A planet has albedo 0.30, receives solar intensity S=1361W m−2, and has an effective emissivity of 0.80 because of its atmosphere. (a) Calculate its equilibrium temperature. (b) The black-body value (ε=1) is 255 K — explain why a lower emissivity gives a higher temperature.
(b) A surface with a lower emissivity radiates less efficiently to space. To get rid of the same absorbed power (fixed by S and α), it must reach a higher temperature, because the radiated power depends on εσT4 — reducing ε must be compensated by increasing T4. This is exactly how greenhouse gases warm a planet: by reducing the effective emissivity of the atmosphere to outgoing infrared.
Why this scores
Why this scores 6/6. (a) correct placement of ε in the denominator (2), correct substitution (1), T ≈ 269 K (1); (b) lower ε means less efficient radiator (1), so higher T needed to shed the same power (1). The physics link — reduced emissivity → higher surface temperature → the greenhouse mechanism — is what raises this above a plug-in.
Question 9
10 marks
Q (10 marks — extended response). (a) The solar constant is S=1361W m−2, the Earth's albedo is 0.30 and σ=5.67×10−8W m−2K−4. Treating the Earth as a black body (ε=1), calculate its equilibrium temperature. (b) The Earth's true average surface temperature is about 288 K. Account for the difference, describing the molecular mechanism responsible. (c) Explain how the enhanced greenhouse effect arises and describe one positive feedback that amplifies it.
Model answer
(a) Equilibrium temperature. At equilibrium, absorbed power = radiated power:
(b) The 33 K difference — the natural greenhouse effect. The calculated 255 K assumes all the outgoing infrared escapes freely to space. In reality the atmosphere contains greenhouse gases (water vapour, carbon dioxide, methane, nitrous oxide). The warm surface radiates infrared; these molecules absorb infrared radiation whose frequency matches the natural (resonant) frequencies of their bond vibrations, and then re-emit it in all directions, returning some to the surface. This extra downward energy warms the surface from 255 K to about 288 K — a warming of roughly 33 °C that is essential for life.
(c) The enhanced greenhouse effect and a feedback. Human activities (burning fossil fuels, agriculture, deforestation) increase the concentration of greenhouse gases. More molecules absorb a greater fraction of the outgoing infrared and return more of it to the surface, so the surface temperature rises above its natural value — the enhanced greenhouse effect, i.e. global warming.
A positive (amplifying) feedback is the ice–albedo feedback: warming melts bright, reflective ice, exposing darker ocean and land with a lower albedo. Less sunlight is reflected and more is absorbed, so the planet warms further, which melts still more ice. (An alternative valid feedback: warming increases evaporation, adding more water vapour — itself a greenhouse gas — which causes further warming.)
Why this scores
Why this scores 10/10. (a) energy balance and rearrangement (1), correct substitution (1), T ≈ 255 K (1); (b) states the 255 K assumes free escape of IR (1), greenhouse gases absorb IR at resonant frequencies (1), re-emit in all directions returning energy to surface (1), gives ~288 K / 33 °C natural warming (1); (c) enhanced effect = extra warming from rising concentrations linked to human activity (1), identifies a positive feedback (1) and explains its amplifying mechanism (1). A model Paper 2 extended response: it combines a clean calculation with the precise molecular mechanism and a correctly reasoned feedback.
Key Formulae — Greenhouse effect
The formulae you need to memorise for greenhouse effect on the Cambridge IGCSE paper, with every variable defined in plain English and a note on when to use it.
Intensity (inverse-square law)
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I=4πd2L
I
intensity / power per unit area (W m⁻²)
L
luminosity — total power output of the star (W)
d
distance from the star (m)
When to use
To find the solar intensity (e.g. the solar constant) at a planet's distance from its star; intensity falls off as 1/d².
Example
At Earth's distance the Sun's radiation gives the solar constant S ≈ 1361 W m⁻².
Albedo
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α=PincidentPreflected
α
albedo (dimensionless, 0–1)
Preflected
total power reflected (W)
Pincident
total power incident (W)
When to use
To find the fraction of incoming radiation reflected; the fraction absorbed is then (1 − α). Earth's average albedo ≈ 0.30.
Example
Reflects 5.2×10¹⁶ W of an incident 1.74×10¹⁷ W: α = 0.30.
Emissivity
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ε=power radiated by black body at same Tpower radiated by surface
ε
emissivity (dimensionless, 0–1)
When to use
To compare a real surface's radiated power with a perfect black body at the same temperature; ε = 1 for a black body.
Example
Radiates 350 W m⁻² where a black body would radiate 390 W m⁻²: ε ≈ 0.90.
Stefan–Boltzmann law (with emissivity)
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P=εσAT4
P
power radiated (W)
ε
emissivity (0–1)
σ
Stefan–Boltzmann constant = 5.67×10⁻⁸ W m⁻² K⁻⁴
A
surface area radiating (m²)
T
absolute temperature (K)
When to use
To find the power radiated by a surface; temperature MUST be in kelvin. Per unit area, I = εσT⁴.
Example
Black body at 288 K: I = σT⁴ = 5.67×10⁻⁸ × 288⁴ ≈ 390 W m⁻².
Solar power absorbed by a planet
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Pabsorbed=S(1−α)πR2
S
solar intensity at the planet (W m⁻²)
α
albedo (0–1)
R
planet's radius (m)
When to use
For the incoming side of the energy balance. The planet intercepts over the disc πR² and absorbs only the fraction (1 − α).
The result of setting absorbed power = radiated power and cancelling πR². The factor 4 comes from 4πR² ÷ πR².
Example
Earth (α = 0.30, ε = 1): T ≈ 255 K (−18 °C).
Key Definitions and Keywords — Greenhouse effect
Definitions to memorise and the exact keywords mark schemes credit for greenhouse effect answers — sharpened from recent examiner reports for the 2026 Cambridge IGCSE sitting.
Black body
Examiner keyword▼
An idealised object that absorbs all radiation incident on it and, at a given temperature, is the best possible emitter of radiation. Its emissivity is 1.
Black-body radiation
Examiner keyword▼
The continuous spectrum of electromagnetic radiation emitted by a black body; its total intensity (σT⁴) and peak wavelength depend only on the temperature.
Solar constant
Examiner keyword▼
The mean intensity of solar radiation arriving at the top of Earth's atmosphere on a surface perpendicular to the Sun's rays, at Earth's average distance from the Sun; S ≈ 1361 W m⁻².
Albedo (α)
Examiner keyword▼
The ratio of the total power reflected by a surface to the total power incident on it. Dimensionless (0–1); Earth's average albedo ≈ 0.30.
Emissivity (ε)
Examiner keyword▼
The ratio of the power radiated by a surface to the power radiated by a black body at the same temperature. Dimensionless (0–1); a black body has ε = 1.
Stefan–Boltzmann law
Examiner keyword▼
The power radiated by a body is P = εσAT⁴, where σ = 5.67×10⁻⁸ W m⁻² K⁻⁴. The intensity (power per unit area) of a black body is I = σT⁴.
Intensity
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The radiant power passing through unit area perpendicular to the radiation, measured in W m⁻². Falls off with distance as 1/d² (inverse-square law).
Equilibrium temperature
Examiner keyword▼
The steady temperature at which a planet's absorbed solar power equals the power it radiates; T = [S(1−α)/(4εσ)]^(1/4). For Earth (black body) ≈ 255 K.
Energy balance
Examiner keyword▼
The condition, at a steady temperature, that the power a planet absorbs from its star equals the power it radiates back to space: S(1−α)πR² = εσ4πR²T⁴.
Greenhouse gas
Examiner keyword▼
An atmospheric gas that absorbs and re-emits infrared radiation, e.g. water vapour (H₂O), carbon dioxide (CO₂), methane (CH₄) and nitrous oxide (N₂O).
Greenhouse effect (natural)
Examiner keyword▼
The warming of a planet's surface caused by naturally present greenhouse gases absorbing outgoing infrared radiation and re-emitting some of it back to the surface; raises Earth from ~255 K to ~288 K.
Enhanced greenhouse effect
Examiner keyword▼
The additional warming caused by rising concentrations of greenhouse gases (largely from human activity), which absorb a greater fraction of outgoing infrared and raise the surface temperature further.
Infrared radiation
▼
Electromagnetic radiation with wavelengths longer than visible light (roughly 700 nm to 1 mm). The Earth's surface radiates mainly in the infrared, which greenhouse gases absorb.
Natural (resonant) frequency
Examiner keyword▼
A frequency at which a molecule's bonds naturally vibrate. When infrared radiation has a matching frequency, the molecule absorbs it strongly (resonance) and vibrates more energetically.
Positive feedback (climate)
▼
A process that amplifies an initial change, e.g. the ice–albedo feedback: warming melts ice, lowering the albedo, so more sunlight is absorbed and the warming increases further.
Common Mistakes and Misconceptions — Greenhouse effect
The traps other students keep falling into on greenhouse effect questions — taken from recent Cambridge IGCSE examiner reports and mark schemes — and how to avoid them.
✕Forgetting the (1 − α) factor for the absorbed solar power
IB Physics Theme B subject reports
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Why it happens
Students multiply the solar constant straight into the energy balance without subtracting the reflected fraction.
How to avoid it
Only the fraction (1 − α) of incident sunlight is absorbed; the rest is reflected. Always write the absorbed power as S(1 − α)πR², not SπR².
✕Confusing the absorbing cross-section (πR²) with the emitting surface (4πR²)
IB Physics Theme B subject reports
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Why it happens
Both areas involve R, so students use the same area for absorption and emission and lose the factor of 4.
How to avoid it
The planet absorbs over the disc πR² (sunlight is parallel) but radiates over the whole sphere 4πR². Their ratio gives the factor of 4 that appears in T = [S(1−α)/(4εσ)]^(1/4).
✕Leaving the temperature in degrees Celsius when using σT⁴
IB Physics Theme B subject reports
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Why it happens
Students read a temperature such as 15 °C and substitute it directly into the Stefan–Boltzmann law.
How to avoid it
Always convert to KELVIN before raising to the fourth power (add 273). Using °C makes the radiated power wildly wrong because of the fourth-power dependence.
✕Saying greenhouse gases 'trap' or 'reflect' heat like a blanket
IB Physics Theme B subject reports
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Why it happens
The blanket analogy is common in everyday language, so students repeat it instead of the physics.
How to avoid it
State the mechanism precisely: greenhouse-gas molecules ABSORB infrared radiation at the natural (resonant) frequencies of their bond vibrations and RE-EMIT it in all directions, returning some to the surface.
✕Confusing the natural greenhouse effect with the enhanced greenhouse effect
IB Physics Theme B subject reports
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Why it happens
Both involve greenhouse gases, so students describe the natural effect as if it were the cause of climate change.
How to avoid it
The NATURAL greenhouse effect is always present and keeps Earth habitable (~+33 °C). The ENHANCED greenhouse effect is the EXTRA warming from rising gas concentrations — that is what causes global warming.
✕Thinking carbon dioxide is the only greenhouse gas
IB Physics Theme B subject reports
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Why it happens
CO₂ dominates public discussion of climate change, so students name it alone.
How to avoid it
Remember the main greenhouse gases: water vapour (the largest natural contributor), carbon dioxide, methane and nitrous oxide. Water vapour and methane are especially important.