#5.5.2a
energy levels of electrons in isolated gas atoms
#5.5.2b
the idea that energy levels have negative values
#5.5.2c
emission spectral lines from hot gases in terms of emission of photons and transition of electrons between discrete energy levels
#5.5.2d
the equations \(hf = ΔE \) and \(\dfrac{hc}{λ} = ΔE \)
Learners will also require knowledge of section 4.5
#5.5.2e
different atoms have different spectral lines which can be used to identify elements within stars
#5.5.2f
continuous spectrum, emission line spectrum and absorption line spectrum
#5.5.2g
transmission diffraction grating used to determine the wavelength of light
The structure and use of an optical spectrometer are not required;
PAG 5
#5.5.2h
the condition for maxima \(d\sin{θ} = nλ\), where d is the grating spacing
Proof of this equation is not required.
#5.5.2i
use of Wien’s displacement law \(λ_{max} ∝ \dfrac{1}{T} \) to estimate the peak surface temperature (of a star)
#5.5.2j
luminosity L of a star;
Stefan’s law \(L = 4πr^2σT^4 \) where σ is the Stefan constant
Learners will also require knowledge of 4.4.1
#5.5.2k
use of Wien’s displacement law and Stefan’s law to estimate the radius of a star.