Class 12 · Notes

Nuclei— Notes, Formulas & Revision

Complete revision notes and formulas for Nuclei (Class 12). Curated for JEE, NEET, AP Physics, SAT, and CUET. Tap any topic to open the live simulation and full PYQ set.

Radioactive Decay

Stochastic decay of atoms vs theoretical N(t) = N₀e^(−λt) with λ = ln2/T½.

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Radioactive decay: unstable nuclei spontaneously emit α, β, or γ radiation and transform into another nucleus.

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α-decay: emits ⁴₂He nucleus. (A, Z) → (A−4, Z−2) + α. Common in heavy nuclei (Z ≥ 83).

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β⁻-decay: a neutron converts to proton + electron + antineutrino. (A, Z) → (A, Z+1) + e⁻ + ν̄. Occurs in neutron-rich nuclei.

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β⁺-decay (positron emission): proton → neutron + e⁺ + ν. Occurs in proton-rich nuclei.

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γ-decay: nucleus de-excites by emitting a γ-ray photon (no change in A or Z) — analogous to atomic transitions.

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Decay is RANDOM: any single nucleus may decay at any time. Only the STATISTICAL behaviour is predictable.

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Decay law: dN/dt = −λN ⇒ N(t) = N₀ e^(−λt). λ = decay constant. τ = 1/λ = mean life.

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Half-life T_½ = (ln 2)/λ — time for half the nuclei to decay.

Decay law (exponential)

N₀ = initial number; λ = decay constant (s⁻¹).

Decay rate (activity)

Units: becquerel (Bq) = 1 disintegration/s. Curie (Ci) = 3.7 × 10¹⁰ Bq.

Half-life

Time for half the nuclei to decay.

Mean life

Average lifetime of a nucleus before decaying.

Radioactive decay is a NUCLEAR property — not affected by chemistry, temperature, or pressure.

α-particles are highly ionising but short range (~few cm in air; stopped by paper). β-particles penetrate further (~mm of aluminum). γ-rays are most penetrating.

Health hazard: α inside the body (inhaled/ingested) is dangerous; outside skin, paper stops it. γ from outside is the main external hazard.

Decay constants vary over many orders of magnitude: U-238 T₁/₂ ≈ 4.5 × 10⁹ years; carbon-14 ≈ 5730 years; iodine-131 ≈ 8 days.

Activity (Bq) does NOT equal mass — a tiny amount of short-lived isotope can have HUGE activity.

Common pitfall: confusing 'decay constant' (s⁻¹) with 'half-life' (s). They're related by ln 2.

Half-Life

Stacked halving boxes — 4 isotopes (C-14, I-131, U-238, P-32).

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Half-life T_½ is the time for half the nuclei in a sample to decay.

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After n half-lives, fraction surviving = (1/2)ⁿ ⇒ N/N₀ = 1/2ⁿ.

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T_½ is independent of starting amount or chemistry — depends ONLY on the isotope.

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Relation to decay constant: T_½ = (ln 2)/λ ≈ 0.693/λ.

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Examples: C-14 T_½ = 5730 yr; I-131 = 8.0 d; Po-214 = 164 μs; U-238 = 4.5 × 10⁹ yr; Tc-99m = 6 hours.

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Activity also halves every T_½: A(t) = A₀ × (1/2)^(t/T_½).

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Carbon-14 dating: dead organisms stop incorporating fresh C-14; the ratio C-14/C-12 decays exponentially.

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Tc-99m (T_½ = 6 hr, γ-emitter) is the most widely used medical imaging isotope — short enough for safety, long enough for procedures.

Half-life decay

After n half-lives, 2⁻ⁿ remain.

Half-life vs decay constant

Direct relation.

Mean lifetime

Average time before any single nucleus decays.

Carbon-14 dating

Determines age from current vs original ¹⁴C activity.

T_½ refers to STATISTICAL behaviour — a SINGLE nucleus has no 'half-life'. After T_½, each nucleus has 50% chance of having decayed.

Activity halves at the same rate as N — both follow the same exponential.

Memorise (1/2)^n: 1, ½, ¼, ⅛, 1/16, 1/32, … Useful for 'after 5 half-lives' questions.

After 10 half-lives, only ~0.1% (1/1024) of the initial amount remains.

Carbon-14 dating works up to ~50,000 years (after that, activity is too low to measure reliably).

Half-life is NOT the same as mean lifetime — τ ≈ 1.44 T_½.

Decay Curve

Side-by-side linear N(t) + semilog lnN(t) — slope = −λ on the log plot.

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The decay curve N(t) = N₀ e^(−λt) is an exponential drop.

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It looks STRAIGHT on a semi-log plot (ln N vs t): slope = −λ, intercept = ln N₀.

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Half-lives evenly space along t-axis: at T_½, 2T_½, 3T_½, … the count halves each time.

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Tail of the curve never reaches zero (exponentials are asymptotic) — but after many T_½ the count is negligibly small.

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Daughter accumulation in a chain (Parent → Daughter): daughter builds up to a maximum, then decays if it too is unstable.

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Secular equilibrium: when parent is much longer-lived than daughter, daughter activity equals parent activity at equilibrium.

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Transient equilibrium: parent slightly longer than daughter; daughter exceeds parent for a while before equilibrium.

Exponential decay

Smooth curve; never reaches zero.

Logarithmic form (linearised)

Slope of ln N vs t = −λ.

After n half-lives

Useful discrete form.

Bateman (parent → daughter)

Daughter builds up then decays in a chain.

Plot N vs t: smooth exponential curve. Plot ln N vs t: straight line. Use semi-log to identify single exponentials.

Half-life can be read off the linear (semi-log) plot — successive halvings spaced by ΔT = T_½.

In sequential decays (A → B → C), the intermediate B builds up, peaks, then decays.

Activity curve has the SAME shape as N(t) — both decay exponentially with the same λ.

Tail: even after 10 T_½ (1/1024), activity remains — important for nuclear waste storage.

Real plots include statistical noise — short timescales need many counts to see the exponential cleanly.

Binding Energy per Nucleon

Weizsäcker semi-empirical mass formula — peak at ⁵⁶Fe, labeled key nuclei.

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Binding energy is the energy needed to disassemble a nucleus into its constituent protons and neutrons.

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Equivalently, it is the ENERGY RELEASED when free nucleons assemble into a nucleus (mass-energy equivalence).

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Mass defect: Δm = Zm_p + (A−Z)m_n − m_nucleus. The nucleus weighs LESS than its parts.

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Binding energy: B = Δm · c². Often quoted in MeV using 1 u = 931.5 MeV/c².

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Binding energy per nucleon B/A is the most useful quantity: nuclei with larger B/A are more stable.

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B/A peaks at A ≈ 56 (Fe-56, Ni-62) with ~8.8 MeV/nucleon. Falls off for heavier and lighter nuclei.

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Fission of heavy nuclei (A > 56) and fusion of light nuclei (A < 56) BOTH release energy because the products have higher B/A.

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Iron-56 is the most stable nucleus per nucleon — endpoint of stellar nucleosynthesis.

Mass defect

Always > 0 for bound nuclei.

Binding energy

Using 1 u = 931.5 MeV/c²: B [MeV] = Δm [u] × 931.5.

Binding energy per nucleon

Stability indicator; ~8.5 MeV for stable mid-mass nuclei.

Semi-empirical mass formula (Weizsäcker)

Volume, surface, Coulomb, asymmetry, pairing terms — fits B/A trend well.

B/A vs A curve: rises steeply for light nuclei, plateaus around 8-9 MeV for A = 50-150, slowly falls for heavy nuclei. Peak at Fe-56.

Light nuclei (H, He, Li) have low B/A ⇒ FUSION releases energy.

Heavy nuclei (U, Pu) have B/A ~ 7.6 ⇒ FISSION into mid-mass products (B/A ~ 8.5) releases ~200 MeV per fission.

Stellar nucleosynthesis produces elements up to iron via fusion — beyond iron, fusion is endothermic.

Heavier elements (gold, uranium) are made in SUPERNOVAE and neutron-star mergers via r-process.

Binding energy explains why mass is NOT conserved in nuclear reactions: energy released = mass defect × c².

Nuclear Reactions (Q-value)

Q = Δm · c² — preset D-T, D-D, p-Li fusion and U-235 fission reactions.

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A nuclear reaction is when a projectile (n, α, γ, etc.) hits a target nucleus, producing a new nucleus + ejecta.

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Standard notation: target(projectile, ejected)product. Example: ¹⁴N(α, p)¹⁷O = α-particle + N-14 → O-17 + proton.

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Conservation laws: charge (Z), mass number (A), energy, momentum, and angular momentum are ALL conserved.

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Q-value: Q = (initial rest mass − final rest mass)·c² = total kinetic energy released.

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Endothermic (Q < 0): require minimum (threshold) KE of projectile. Exothermic (Q > 0): release energy.

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Reaction cross-section σ measures probability — typical units: barn = 10⁻²⁸ m². Depends strongly on energy.

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Compound nucleus model (Bohr): projectile is absorbed first, then a 'hot' compound nucleus decays.

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Direct reactions: fast, single-step (e.g., pickup or stripping). Compound-nucleus: slower, statistical.

Q-value of a reaction

Sum of rest masses; Q > 0 ⇒ exothermic.

Standard notation

Target X, projectile a, ejectile b, residue Y.

Threshold energy (endothermic)

Minimum lab KE of projectile to make Q < 0 reaction proceed.

Conservation of A and Z gives you DAUGHTER nucleus quickly: write A and Z on both sides and balance.

Q > 0 ⇒ reaction proceeds spontaneously (energy released). Q < 0 ⇒ need to inject energy.

Rutherford's 1919 experiment ¹⁴N(α,p)¹⁷O was the FIRST artificially-induced nuclear transmutation.

Cross-section σ is highly energy-dependent — sharp peaks (resonances) at compound-nucleus excitation energies.

Slow neutrons (thermal) have HUGE cross-sections for many nuclei because they spend more time inside.

Fission and fusion are special cases of nuclear reactions with very large |Q|.

Nuclear Fission

Animated chain reaction — tune k to toggle subcritical / critical / supercritical.

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Nuclear fission: heavy nucleus (e.g., U-235, Pu-239) splits into two smaller fragments, plus 2-3 free neutrons, plus energy.

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Discovered by Hahn and Strassmann (1938); explained by Meitner and Frisch using liquid-drop nuclear model.

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Typical fission of U-235: ²³⁵U + n → ¹⁴⁴Ba + ⁸⁹Kr + 3n + ~200 MeV.

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Energy comes from mass defect: products have higher B/A than parent.

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Released neutrons (~2.5 on average) can induce further fissions — basis of CHAIN REACTION.

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Critical mass: minimum amount of fissile material to sustain chain reaction (e.g., ~50 kg of U-235 bare-sphere, much less if reflected).

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Controlled chain reaction = NUCLEAR REACTOR. Uncontrolled = ATOMIC BOMB.

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Moderators (water, graphite, heavy water) slow neutrons to thermal speeds — thermal U-235 fission has much larger cross-section than fast.

Typical U-235 fission

Q ≈ 200 MeV — distributed among kinetic energy of fragments, neutrons, γ-rays, β-decays of fragments.

Energy per kg fissioned

~2.5 million times that of TNT (~4 × 10⁶ J/kg).

Chain-reaction criterion

k = 1 critical (steady), k > 1 supercritical (growing), k < 1 subcritical (dying).

Multiplication factor

Six-factor formula (four-factor for thermal): factors for neutron production, fast fission, resonance escape, thermal utilization, non-leakage probability.

One fission releases ~200 MeV — ~50 million times the energy from burning a single C atom.

U-235 (0.7% natural abundance) is fissile with thermal neutrons. U-238 (99.3%) is fertile (needs fast n).

Reactor moderators: light water (PWR/BWR), heavy water (CANDU), graphite (RBMK).

Control rods (cadmium, boron) absorb neutrons to control k_eff and stop runaway.

Fission products are intensely radioactive — main concern for waste storage and accidents.

Critical mass concept: enough material so that neutrons born inside have high probability of inducing further fissions before escaping.

Nuclear Fusion

D-T fusion overcoming Coulomb barrier — plasma T sets kinetic energy.

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Nuclear fusion: light nuclei combine to form heavier ones, releasing energy.

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Most famous: ²H + ³H → ⁴He + n + 17.6 MeV (D-T reaction, basis of H-bomb and tokamaks).

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Energy comes from mass defect: products are slightly lighter than reactants.

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Fusion requires extreme temperatures (~10⁸ K) to overcome electrostatic repulsion between positive nuclei (Coulomb barrier).

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In stars: gravity provides confinement; the Sun fuses H → He via proton-proton chain at ~15 million K.

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On Earth: magnetic confinement (tokamaks) or inertial confinement (laser implosion of fuel pellets).

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Fusion releases MORE energy PER NUCLEON than fission (~3.5 MeV/nucleon vs ~1 MeV/nucleon).

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Advantages over fission: abundant fuel (deuterium from seawater), no long-lived radioactive waste, no chain-reaction runaway risk.

Deuterium-Tritium fusion

Most-studied terrestrial fusion reaction.

Proton-proton chain (Sun)

Net stellar fusion: 4 protons → α + 2 positrons + 2 neutrinos + photons.

Coulomb barrier (D-T)

Quantum tunnelling allows fusion below this barrier at lower temperatures.

Lawson criterion (ignition)

Triple product of density, confinement time, and temperature required for net energy gain.

Fusion of light nuclei is what powers the Sun and all main-sequence stars.

Net energy gain on Earth requires extreme temperatures + sufficient confinement (Lawson criterion).

ITER (under construction in France) aims for Q = 10 (output / input energy). Expected first plasma ~2025.

Cold fusion (room-temperature fusion in metal lattices) is NOT established physics — claims have not been replicated.

Stellar nucleosynthesis builds elements up to iron via fusion; heavier elements form in supernovae.

Fusion bombs: trigger D-T fusion using a fission bomb to compress and heat the fuel — first tested 1952.

Mass–Energy Equivalence

E = mc² — mass in amu → J, MeV, kWh, megatons TNT. Presets for electron → ²³⁵U.

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Einstein's mass-energy equivalence (special relativity, 1905): E = mc².

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1 kg of mass corresponds to 9 × 10¹⁶ J of energy — vast, but only nuclear reactions release a measurable fraction.

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Atomic mass unit: 1 u = 1.66054 × 10⁻²⁷ kg. Energy equivalent: 1 u · c² = 931.494 MeV.

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Mass defect in any bound system = (sum of constituent masses) − (system mass). Always positive for bound states.

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Energy released = (mass defect) × c². For nuclear reactions, mass defect is detectable (~MeV scale).

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Chemical reactions also have mass defects — but ~10⁶× smaller (eV scale) ⇒ undetectable with chemical scales.

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Particle-antiparticle annihilation: m + m → 2γ. Each photon carries mc² of energy. Pair production: γ → e⁺ + e⁻ requires hf ≥ 2m_e·c² = 1.022 MeV.

Mass-energy equivalence

Rest energy of a particle of mass m.

Useful unit conversion

Converts mass defect in atomic units to energy in MeV.

Q-value of a reaction

Energy released if Q > 0 (exothermic), absorbed if Q < 0.

Pair production threshold

Minimum photon energy to produce an electron-positron pair.

Annihilation

Each photon's energy if particles were at rest.

Mass and energy are interconvertible — they are TWO ASPECTS of the same thing.

Even chemical reactions have mass defects, but they are too small to detect (Δm/m ~ 10⁻⁹).

Nuclear reactions have detectable mass defects (Δm/m ~ 10⁻³).

1 u corresponds to 931.5 MeV. Memorise this: it's the bridge between nuclear masses and energies.

E = mc² is the rest energy. Moving particles have additional kinetic energy ⇒ total E = mc²/√(1−v²/c²).

Mass-energy CONSERVATION (not separate mass conservation) holds in all physics.

Nuclei on sciphylab (also known as SciPhy, SciPhy Lab, SciPhy Labs). Free physics revision for Class 12, JEE Mains, JEE Advanced, NEET UG, AP Physics 1/2/C, SAT Subject Physics, and CUET-UG.