1. Terrestrial Planets. II. 1.Earth as a planet: interior & tectonics. 2.Dynamics of the mantle 3.Modeling terrestrial planets

2. Earth interior

3. Earth mantle convection simulation Labrosse & Sotin (2002)

4. Earth interior - mantle plumes

5. Earth - cooling

8. Earth interior - cooling

9. Super-Earths

10. Searching for Small Planets: after Gould et al. (2006) First ‘Super-Earth’ discovered GJ 876d: -- Mass ~ 7.5 Earths Also HD 69830b: -- Mass ~ 10 Earths NASA Kepler mission: … Radii in this range M = Mercury V = Venus E = Earth, etc.

11. What would we look for and could we measure it ? Illustrate with an example - planet GJ876d:

12.  GJ876: an M-dwarf (1/3 solar) with 3 planets  GJ876d - the first Super-Earth (~7.5 Earth mass) discovered (Rivera et al. 2005);  Several possible models of GJ876d ’s interior - could we distinguish among them ?  If so, what tolerances in Radius & Mass are needed ? What would we look for and could we measure it ? Illustrate with an example - planet GJ876d:

13. The models follow the techniques and many assumptions of Earth’s model: Interiors of Super-Earths Tsuchiya et al. (2004); Valencia, Sasselov, O’Connell (2006) TWO POINTS: - Given a wide range of cosmic compositions, the mineralogy and differentiation do not vary - Their mantles will consist mostly of the newly discovered high-P phase of perovskite - post-pv Schematic temperature profile

14. Post-Perovskite

15. Interiors of Super-Earths Valencia, Sasselov, O’Connell (2006) Earth-like Ocean Planet

16. Mass-Radius relations for 11 different mineral compositions (Earth-like): Interiors of Super-Earths Valencia, O’Connell, Sasselov (2005) 1M E 2M E 5M E 10M E

17. Theoretical Error Budget: Planet Radius Errors:  New high-P phases, e.g. ice-XI: -0.4%  EOS extrapolations (V vs. BM): +0.9%  Iron core alloys (Fe vs. FeS): -0.8%  Viscosity, f(T ) vs. const.: +0.2%  Overall the uncertainties are below 2% (at least, that’s what is known now)

18. Interior Structure of GJ 876d 20,000 12,000 4,000 2,0006,00010,000 RADIUS (km) DENSITY (kg/m 3 ) Valencia, Sasselov, O’Connell (2006) 7.5 M E

19. Interior Structure of GJ 876d Valencia, Sasselov, O’Connell (2006)

20. Interior Structure of Super-Earths Valencia, Sasselov, O’Connell (2006)

21. Interior Structure of Super-Earths Valencia, Sasselov, O’Connell (2006) Kepler error bar

22. Interior Structure of Super-Earths Valencia, Sasselov, O’Connell (2006)

23. What would we look for and could we measure it ? Could we measure the difference? - YES: We need at least 5% in Radius, and at least 10% in Mass. Work on tables for use with Kepler underway - masses 0.4 to 15 M E

24. New Earths Facility Synergy with KEPLER: Provide ability to reach RV amplitudes of about 20 cm /sec. Given P orb and phase from transit, this can translate to 10% masses in the Super-Earth and Earths regime. HARPS-NEF with Obs.Geneve on a large telescope (WHT)  Use to measure masses, hence mean densities, for KEPLER’s candidates.

25. New Earths Facility HARPS-South facts: Requires T and P control: 1 m/sec = 15 nm = 10 -3 pix = 0.01 K = 0.01 mbar Obs. Run on  Cen B: 52 cm/sec (one night, 80% of that was p-modes), Obs. Run on HD 69830d: 20 cm/sec (over entire run).

26. HARPS: HD 69830 b,c, & d Lovis, Mayor, Pepe, et al. (2006) Flux Wavelength (microns) significant part of the error bars due to stellar jitter - 20 to 80 cm/sec; for HD 69830d have residuals of 20 cm/sec over the 3-year run.