Explain that, in a stable star (for example, our Sun), there is an equilibrium between radiation pressure and gravitational pressure.
E.2.7
Explain how atomic spectra may be used to deduce chemical and physical data for stars. Students must have a qualitatve apprecitaion of the Doppler effect as applied to light, including the terms red-shift and blue-shift.
F3
Stellar distances
5
E3
Stellar distances
5
E.3.7
Solve problems involving apparent magnitdue, absolute magnitude and distance.
F4
Cosmology
4
E4
Cosmology
4
E.4.10
Discuss how the density of the universe determines the development of the universe.
E.4.11
Discuss problems associated with determining the density of the universe. This statement is included to give the students a flavour for the ongoing and complex current nature of research. They should be able to discuss relevant observations and possible explanations. They should recognize that, in common with many other aspects of our universe, much about the phenomena is currently not well understood. Teachers should include dark matter, MACHOs and WIMPs.
E.4.12
State that current scientific evidence suggests that the universe is open.
E.4.13
Discuss an example of the international nature of recent astrophysics research. It is sufficient for students to outline any astrophysics project that is funded by more than one country.
E.4.14
Evaluate arguments related to investing significant resources into researching the nature of the universe. Students should be able to demonstrate their ability to understand the issues involved in deciding priorities for scientific research as well as being able to express their own opinions coherently.
Astrophysics for HL only
Astrophysics for HL only
F5
Stellar processes and stellar evolution
4
E5
Stellar processes and stellar evolution
4
E.5.2
State the effect of a star's mass on the end product of nuclear fusion.
E.5.4
Apply the mass-luminosity relation.
E.5.6
Compare the fate of a red giant and a red supergiant. Students should know that : a red giant forms a planetary nebula and then becomes a white dwarf, a white dwarf is stable due to electron degeneracy pressure, a red supergiant experiences a supernova and becomes a neutron star or collapsesto a black hole, a neutron star is stable due to neutron degeneracy pressure.
F6
Galaxies and the expanding universe
3
E6
Galaxies and the expanding universe
3
E.6.9
Explain how the expansion of the universe made possible the formation of light nuclei and atoms. Students should appreciate that, at the very high temperatures of the early universe, only elementary (fundamental) particles could exist and that expansion gave rise to cooling to temperatures at which light nuclei could be stable.
