IB Physics HL E5 Fusion and Stars — Complete Cheatsheet
Every formula, definition and exam trap for IB Physics Topic E.5 — fusion reactions, Wien's Law, Stefan-Boltzmann, the HR diagram, stellar evolution, mass-luminosity, the Jeans criterion and standard candles. Hand-built by an IBO-experienced Singapore tutor.
Topic E.5 — Fusion and Stars — closes the IB Physics syllabus and is the topic that ties nuclear physics to astrophysics. SL students must handle fusion reactions, Wien's Law, the Stefan-Boltzmann law and the HR diagram; HL students extend this to the mass-luminosity relation, the Jeans criterion for star formation and Type Ia supernovae as standard candles. Examiners love mixing several formulae into a single Paper 2 question — a star's luminosity, then its radius from $L = 4\pi R^2 \sigma T^4$, then its distance from apparent brightness.
This cheatsheet condenses every formula, ratio trick and exam trap from Topic E.5 SL + HL onto one page. Scroll to the bottom for the printable PDF, the full notes pack and the gated tutorial library used by Photon Academy students in Singapore.
Deuterium–tritium fusion. Two light nuclei merge into helium-4 plus a neutron, releasing 17.6 MeV — the lost mass reappears as energy via $E=\Delta m c^2$.
From the Photon question bank
What examiners actually test on this concept:
4H → He (pp chain)D-T gives 17.6 MeVMass decreases, E = Δmc²High T + high density
Fusion combines light nuclei; mass DECREASES (BE per nucleon rises), releasing $E=\Delta m c^2$. D-T yields 17.6 MeV. frequent
Fusion needs BOTH high temperature (~$10^7$ K, to beat Coulomb repulsion) AND high density (collision rate) — state both.
The specific energy of fusion beats fission because hydrogen nuclei are so light.
§2 — Stellar Radiation Laws E.5 SL/HL
Wien's Law:$\lambda_{\max} T = 2.9 \times 10^{-3}$ m K
For ratios use $L_A/L_B=(R_A/R_B)^2(T_A/T_B)^4$ — $\sigma$ cancels.
§3 — Hertzsprung-Russell Diagram E.5 SL/HL
The Hertzsprung–Russell diagram. Luminosity rises upward, temperature increases to the left; the main sequence runs diagonally, with red giants upper-right, supergiants across the top, and white dwarfs lower-left.
The HR diagram plots luminosity (vertical, increasing upward, in $L_\odot$) against surface temperature (horizontal, increasing to the LEFT, in K).
Region
Location on HR
Notes
Main sequence
Diagonal band, upper-left to lower-right
~90% of stars; hydrogen fusion in core
Red giants
Upper right
Cool, large radius, evolved low/medium-mass stars
Supergiants
Top of diagram
Very luminous, very large; high-mass evolved stars
White dwarfs
Lower left
Hot but very small radius; remnants of low-mass stars
NoteLines of constant radius: $L \propto R^2 T^4$, so higher-$R$ lines run parallel to the main sequence, shifted upper-right. A star plotted to the upper-right of another at the same temperature must be larger.
From the Photon question bank
What examiners actually test on this concept:
L vs T (T reversed)Main sequenceRed giants / white dwarfsLines of constant R
HR plots luminosity (up) vs surface temperature increasing to the LEFT. The main sequence runs top-left (hot, bright) to bottom-right. very frequent
Red giants: upper-right (cool, huge); white dwarfs: lower-left (hot, tiny); the Sun sits mid-main-sequence.
Constant-radius lines follow $L\propto R^2T^4$ — a star to the upper-right of another at the same $T$ is larger.
§4 — Stellar Evolution E.5 SL/HL
Evolution pathways
Low / medium mass ($\lesssim 8\, M_\odot$, e.g. the Sun):
Main sequence $\rightarrow$ Red Giant $\rightarrow$ Planetary Nebula $\rightarrow$ White Dwarf.
High mass ($\gtrsim 8\, M_\odot$):
Main sequence $\rightarrow$ Red Supergiant $\rightarrow$ Supernova $\rightarrow$ Neutron Star or Black Hole.
Mass limits
Chandrasekhar limit $\approx 1.4\, M_\odot$: maximum mass of a white dwarf, set by electron degeneracy pressure.
Oppenheimer-Volkoff limit $\approx 3\, M_\odot$: maximum mass of a neutron star, set by neutron degeneracy pressure.
Above the OV limit $\Rightarrow$ collapse to a black hole.
TrickA 2-solar-mass star $\rightarrow$ red giant $\rightarrow$ planetary nebula $\rightarrow$ white dwarf. NOT a supernova — it is below the $\sim 8 M_\odot$ threshold.
Trap"Red giant" vs "red supergiant": giants come from low-mass stars; supergiants come from high-mass stars. They have different endpoints — white dwarf vs supernova / neutron star / black hole.
Stellar evolution. Low/medium-mass stars end as white dwarfs (via a planetary nebula); high-mass stars go supernova and leave a neutron star or black hole.
From the Photon question bank
What examiners actually test on this concept:
Low mass → white dwarfHigh mass → SN → NS/BHChandrasekhar 1.4 M☉OV limit ~3 M☉
Low/medium mass (≲8 M☉): MS → red giant → planetary nebula → white dwarf. High mass (≳8): MS → red supergiant → supernova → neutron star or black hole.frequent
Chandrasekhar limit ~1.4 M☉ (max white dwarf, electron degeneracy); Oppenheimer–Volkoff ~3 M☉ (max neutron star) — above it, a black hole.
Don't confuse red giant (low mass) with red supergiant (high mass) — different endpoints.
TrickTo find mass from luminosity: $M/M_\odot = (L/L_\odot)^{1/3.5} = (L/L_\odot)^{0.286}$. High-mass stars are massively more luminous AND massively shorter-lived.
Jeans criterion
A gas cloud collapses under gravity when $|E_{\text{grav}}| > E_{\text{thermal}}$.
Jeans mass: $M_J \propto T^{3/2}\, \rho^{-1/2}$.
Lower temperature OR higher density $\Rightarrow$ smaller $M_J$ $\Rightarrow$ easier to collapse $\Rightarrow$ star formation.
NoteSupernovae can trigger nearby cloud collapse by compressing the cloud — increasing $\rho$ and pushing it past the Jeans threshold.
From the Photon question bank
What examiners actually test on this concept:
L ∝ M^3.5MS lifetime ∝ M^−2.5Jeans massCloud collapse
Main-sequence $L\propto M^{3.5}$, so lifetime $\propto M/L\propto M^{-2.5}$ — massive stars are far brighter AND far shorter-lived. frequent (HL)
A cloud collapses when $|E_{\text{grav}}|>E_{\text{thermal}}$; Jeans mass $M_J\propto T^{3/2}\rho^{-1/2}$ — cooler/denser clouds collapse more easily.
A supernova can compress a nearby cloud past its Jeans threshold, triggering star formation.
1 parsec:$3.09 \times 10^{16}$ m $\approx 3.26$ ly
TrapParallax only works out to about 1000 pc. Beyond this, the parallax angle $p$ is too small to measure — you need a different distance method (e.g. standard candles).
Type Ia supernovae as standard candles
A white dwarf accretes mass from a binary companion until it exceeds the Chandrasekhar limit, then undergoes runaway thermonuclear ignition.
Always at $\approx 1.4\, M_\odot$ $\Rightarrow$ same peak luminosity every time.
Used to measure distances to remote galaxies — the foundation of the discovery of the accelerating expansion of the universe.
TrickDistance from apparent brightness: $d = \sqrt{L/(4\pi b)}$. Know this formula and use it in both directions — given $L$ and $b$, find $d$; or given $d$ and $b$, find $L$.
TrapType Ia (white dwarf accretion) is a standard candle. Type II (core collapse of a high-mass star) is NOT a standard candle — its peak luminosity varies with progenitor mass.
Stellar parallax. As Earth orbits, a nearby star shifts against the distant background; the parallax angle $p$ gives $d(\text{pc})=1/p(\text{arcsec})$.
From the Photon question bank
What examiners actually test on this concept:
d(pc) = 1/p(arcsec)Parallax limit ~1000 pcType Ia standard candled = √(L/4πb)
Distance $d(\text{pc})=1/p(\text{arcsec})$; 1 pc = 3.26 ly. Parallax works only out to ~1000 pc. frequent (HL)
Type Ia supernovae have the SAME peak luminosity → standard candles; Type II is NOT (its peak varies with progenitor mass).
$d=\sqrt{L/4\pi b}$ links luminosity, brightness and distance — use it both ways.
Worked Example — HR Diagram & Distance
Question (HL Paper 2 style — 7 marks)
Star Sirius A has a peak emission wavelength $\lambda_{\max} = 290$ nm and an apparent brightness $b = 1.2 \times 10^{-7}$ W m${}^{-2}$ as measured from Earth. Its luminosity is $L = 25\, L_\odot$ where $L_\odot = 3.83 \times 10^{26}$ W.
(a) Estimate the surface temperature of Sirius A using Wien's Law. [2]
(b) Calculate the distance to Sirius A in metres. [3]
(c) State whether Sirius A lies on the main sequence and justify briefly. [2]
$d \approx 8.0 \times 10^{16}$ m (about 2.6 pc, in good agreement with the measured 2.64 pc to Sirius). (A1)
At $T \approx 10000$ K and $L \approx 25\, L_\odot$, Sirius A plots in the upper-left region of the main sequence — luminous and hot. (R1)
It IS on the main sequence (it is a hydrogen-fusing A-type star, not a giant or white dwarf — its measured radius is consistent with $L = 4\pi R^2 \sigma T^4$ for a main-sequence value). (A1)
Examiner's note: Two common errors. (i) Forgetting to convert $L$ from solar units to watts before using the brightness equation — keep all SI units throughout. (ii) Mixing up the temperature axis direction on the HR diagram (hot is on the LEFT) when justifying part (c). Always sketch the HR diagram in rough first to anchor your reasoning.
Common Student Questions
Why does a star need both high temperature AND high density to fuse?
High temperature gives the protons enough kinetic energy to overcome the Coulomb barrier (electrostatic repulsion) when they collide. High density gives a high collision frequency, so enough fusion events happen per second to keep the star shining. Either alone is not enough — the Sun's core sits at $\sim 1.5 \times 10^7$ K AND $\sim 1.6 \times 10^5$ kg m${}^{-3}$.
Which way does temperature go on the Hertzsprung-Russell diagram?
Temperature increases to the LEFT — hot blue stars on the left, cool red stars on the right. Luminosity increases upward. The main sequence runs diagonally from upper-left (hot, luminous) to lower-right (cool, faint). Confusing the temperature axis direction is a frequent IB mark loss.
Does every star end its life as a supernova?
No. Only high-mass stars ($\gtrsim 8\, M_\odot$) end as core-collapse supernovae and leave behind a neutron star or black hole. Low / medium-mass stars like the Sun ($\lesssim 8\, M_\odot$) become red giants, shed a planetary nebula and end as white dwarfs — no supernova. A 2-solar-mass star will NOT supernova.
Why are Type Ia supernovae used as standard candles, but not Type II?
Type Ia supernovae form from a white dwarf accreting mass until it exceeds the Chandrasekhar limit ($\sim 1.4\, M_\odot$) and undergoes runaway thermonuclear ignition. Because the trigger mass is always the same, the peak luminosity is always the same ($\sim 5 \times 10^9\, L_\odot$). Type II supernovae are core-collapse events from variable-mass progenitors, so their peak luminosities vary widely — they cannot be used as standard candles.
What are the units of Wien's displacement law constant?
The Wien constant is $2.9 \times 10^{-3}$ m·K (metre-kelvin), NOT m/K. The law is $\lambda_{\max} \cdot T = 2.9 \times 10^{-3}$ m·K, so to find peak wavelength you divide: $\lambda_{\max} = 2.9 \times 10^{-3}/T$ (in metres). To convert to nanometres, divide the metre value by $10^{-9}$. Mixing up the units is the most common Wien-law mark loss.
What's NOT in this cheatsheet
This page gives you the formulas and the traps. The full Photon Academy E.5 Fusion & Stars library (only available to enrolled students or via the resource library subscription) adds:
40-page Notes PDF — every concept worked through in full, including a labelled HR diagram and stellar-evolution flow charts.
Tutorial booklet — 30+ IB-style questions sequenced from foundation to AHL difficulty.
Tutorial Solutions — full mark-scheme-style worked solutions with M1/A1/R1 annotations.
Practice Solutions — extra past-paper-style problems with detailed walk-throughs.
Cheatsheet PDF — print-ready, brand-formatted, the same one our students take into mock exams.
