3.1.2 Limitation of physical measurements
- Random and systematic errors.
- Precision, repeatability, reproducibility, resolution and accuracy.
- Uncertainty.
- Students should understand the link between the number of significant figures in the value of a quantity and its associated uncertainty.
3.2.1.1 Constituents of the atom
- Simple model of the atom, including the proton, neutron and electron. Charge and mass of the proton, neutron and electron in SI units and relative units.
3.2.2.3 Energy levels and photon emission
- Line spectra (eg of atomic hydrogen) as evidence for transitions between discrete energy levels in atoms.
hf = E1 − E2
3.2.2.4 Wave-particle duality
- Appreciation of how knowledge and understanding of the nature of matter changes over time.
- Appreciation that such changes need to be evaluated through peer review and validated by the scientific community.
3.6.1.3 Single harmonic systems (A-level only)
- Study of mass-spring system: T = 2*Pi sqrt(m/k)
3.9.1.3 Single dish radio telescopes, I-R, U-V and X-ray telescopes (A-level only)
- Similarities and differences of radio telescopes compared to optical telescopes. Discussion should include structure, positioning and use, together with comparisons of resolving and collecting powers.
3.9.2 Classification of stars (A-level only)
- General shape of black-body curves, use of Wien’s displacement law to estimate black-body temperature of sources.
- Assumption that a star is a black body.
3.9.2.4 Principles of the use of stellar spectral classes (A-level only)
Description of the main classes
3.9.2.5 The Hertzsprung-Russell (HR) diagram (A-level only)
- General shape: main sequence, dwarfs and giants.
- Axis scales range from –10 to +15 (absolute magnitude) and 50 000 K to 2 500 K (temperature) or OBAFGKM (spectral class).
- Students should be familiar with the position of the Sun on the HR diagram.
- Stellar evolution: path of a star similar to our Sun on the HR diagram from formation to white dwarf.
3.9.3.4 Detection of exoplanets (A-level only)
- Difficulties in the direct detection of exoplanets.
- Detection techniques will be limited to variation in Doppler shift (radial velocity method) and the transit method.
- Typical light curve.