1. SIO224 Internal Constitution of the Earth Fundamental problem: the nature of mass and heat transfer in the mantle and the evolution of the Earth

3. Seismology:1D and 3D structure of the Earth Geochemistry: bulk composition of the Earth; heat production; geochemical tracers of “mantle reservoirs” Mineral physics: thermoelastic properties of materials at high T and P (equations of state); phase transformations; rheology of mantle materials Geodynamics: flow models, geoid constraints, mantle convection, effects of phase transformations and viscosity variations on convection, thermochemical convection, thermal history. Ingredients for a unified mantle model

4. Origin of the solar system

19. Planetary migration (Nice model) Giant planets have migrated over time, Uranus and Neptune were closer in but migrated out after Saturn and Jupiter went into 2:1 resonance Jupiter also migrated slightly inward – interactions with left over material led to late heavy bombardment Issues with this – still being debated

20. Exosolar systems 1202 known systems, 480 known to have multiple planets (two have 7 planets) Some problems for standard theory: orbits not often circular and not coplanar and not all orbit in same direction! Maybe planetary interactions are generally more important than in our solar system

21. Formation of the moon

28. Main problem is simulations show that moon is dominantly composed of impactor mantle but oxygen isotopes of moon and Earth are identical Can fix by having higher velocity impactor or make impactor more similar to proto- Earth

29. Meteorites and the composition of the Earth

38. Timing of core/moon formation

40. Principles of Isotope Geology: Conventional radiogenic isotope systematics used in geology: 147 Sm - 143 Ndt 1/2 = 10.6 x 10 10 yrs 87 Rb- 87 Srt 1/2 = 48.8 x 10 9 yrs 238 U- 206 Pbt 1/2 = 4.47 x 10 9 yrs 235 U- 207 Pbt 1/2 = 0.704 x 10 9 yrs 232 Th- 208 Pbt 1/2 = 14.01 x 10 9 yrs 187 Re - 187 Os t 1/2 = 42.3 x 10 9 yrs 176 Lu - 176 Hft 1/2 = 35.7 x 10 9 yrs

41. The Law of Radioactive Decay The basic equation: -  - dN dt N or dN dt =N # parent atoms time  1½¼1½¼ D* = Ne t - N = N(e t -1)  age of a sample (t) if we know: D* the amount of the daughter nuclide produced N the amount of the original parent nuclide remaining  the decay constant for the system in question (= ln 2/ t ½ ) More conventionally, D (present) = D o + D*

42. These systematics are being used as chronometers a)model age b)isochron age and as petrogenetic tracers….

46. Hf is enriched in the silicate mantle after core formation

48. More realistic calculations with multiple impacts lead to slightly longer times for core formation

52. Solar Systems Form by Accretion