Physics / advanced
Nuclei, forces, and collective structure
Connect nuclear binding and effective forces to shell structure, collective motion, decay selection rules, and evidence from nuclear observables.
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Module 01 advanced
Nuclei, forces, and collective structure
Connect nuclear binding and effective forces to shell structure, collective motion, decay selection rules, and evidence from nuclear observables.
- 01
Nuclear sizes and charge distributions
Infer a charge radius from a normalized form factor while separating sharp-sphere, charge, and matter radii.
30 min - 02
Binding energy and the semiempirical mass formula
Calculate binding and separation energies with consistent mass conventions, then interpret a fitted liquid-drop approximation.
30 min - 03
Nucleon–nucleon scattering and the deuteron
Connect low-energy phase shifts and shallow bound-state tails while retaining spin and tensor-channel distinctions.
30 min - 04
Isospin and charge symmetry
Organize proton-neutron states by approximate internal symmetry without identifying it with spatial spin or exact mass degeneracy.
30 min - 05
Nuclear shell model and magic numbers
Count fermionic orbital capacities and interpret shell closures without confusing a mean field with the full nuclear interaction.
30 min - 06
Spin-orbit force and shell ordering
Derive the sign, magnitude, and degeneracy balance of a nuclear spin-orbit doublet in a declared effective Hamiltonian.
30 min - 07
Collective nuclear rotations and vibrations
Distinguish rotational bands of a deformed nucleus from quantized small-amplitude shape vibrations using conditional spectral patterns.
30 min - 08
Nuclear pairing and odd-even masses
Use explicit mass-difference conventions to diagnose pairing while distinguishing empirical staggering from a model gap.
30 min - 09
Electromagnetic nuclear transition strengths
Separate reduced matrix elements, angular-momentum factors, and photon phase space when comparing nuclear transitions.
30 min - 10
Ab-initio nuclear methods and truncation errors
Connect a specified nuclear Hamiltonian to finite-space calculations, consistent operators, and a transparent uncertainty budget.
30 min