AST study plan

Derive and interpret the Hubble-Lemaître law and compute distances, redshifts, and recession velocities for a set of given numerical cases.

Distinguish among the Friedmann models (open, flat, closed) and calculate the critical density and density parameter from supplied values of H0.

Explain the observational evidence for dark energy, dark matter, and the CMB blackbody spectrum, writing short causal arguments for each.

Build a one-page formula sheet covering cosmological redshift, luminosity distance, angular diameter distance, and the distance modulus.

Compare the cosmological distance ladder rungs (parallax, standard candles, standard rulers) and state the calibration assumptions of each.

Derive the main-sequence mass-luminosity relation scaling from homology arguments and apply it to estimate lifetimes.

Explain the physics of the Hertzsprung-Russell diagram and classify stars by spectral type and luminosity class.

Calculate stellar masses, radii, and effective temperatures from supplied luminosity, temperature, and binary-orbit data.

Trace the evolutionary path of low-, intermediate-, and high-mass stars and identify the nuclear burning stages at each phase.

Explain the physics of degeneracy pressure and apply the Chandrasekhar limit to white dwarf and supernova scenarios.

Describe the structure and energetics of core-collapse supernovae and the formation of neutron stars and black holes.

Compute binding energies and mass deficits for given nuclear reactions and remnant masses.

Classify galaxies by Hubble type and explain how morphology correlates with gas content, star formation, and environment.

Compare the rotation-curve evidence for dark matter halos with the observed scaling relations (Tully-Fisher, Fundamental Plane).

Describe the structure of the Milky Way (disk, bulge, halo, spiral arms) and the evidence for its central supermassive black hole.

Explain galaxy clustering, the Local Group, and the role of mergers in galaxy evolution.

Compare the formation and internal structure of terrestrial and giant planets, including the role of the frost line.

Explain Keplerian orbital parameters and apply them to compute planetary masses, densities, and orbital periods.

Describe the physics of atmospheres, greenhouse effects, and the conditions for habitability.

Summarize the properties of small bodies (asteroids, comets, Kuiper belt) and impact processes.

Explain the operating principles of optical telescopes, detectors, and the sources of noise and limiting magnitude.

Compute angular resolution, plate scale, exposure times, and signal-to-noise ratios from supplied instrument parameters.

Apply Kepler's laws and the vis-viva equation to solve two-body orbital problems, including escape and transfer orbits.

Describe tidal forces, Roche limits, resonances, and the three-body problem qualitatively with worked examples.

Describe the phases of the interstellar medium and the observational signatures of molecular clouds and dust.

Explain the Jeans criterion and the stages of star formation from cloud collapse to protostellar disk and outflow.

Apply fundamental physics (blackbody radiation, Doppler effect, atomic spectra, gravitation, thermodynamics) to astronomical contexts.

Solve quantitative problems combining radiative transfer, thermal physics, and spectral line analysis.

Consolidate all eight domains by reviewing the error logs and formula sheets from earlier weeks.

Complete two full-length timed mock exams under exam conditions and score them against the answer keys.

Identify the three weakest sub-topics from the mock results and re-derive their core formulas from first principles.

Write a final one-page summary sheet linking the key equations across all domains.