1. The Diversity of Extrasolar Terrestrial Planets J. Carter-Bond, D. O’Brien & C. Tinney RSAA Colloquium 12 April 2012

2. Stars → building blocks → terrestrial planets In terms of extrasolar terrestrial planets, we generally consider other “Earth-like” planets –Metallic core, silicate mantle and crust –Atmosphere –Active on the planetary scale BUT extrasolar planetary systems are chemically and dynamically unusual! Since these different compositions may produce different planetary building blocks, what types of terrestrial planets may exist?

3. How common is Earth?

7. SiC SiO MgSiO 3 + SiO 2 MgSiO 3 + Mg 2 SiO 4 Mg 2 SiO 4 + MgO

8. SiC SiO MgSiO 3 + SiO 2 MgSiO 3 + Mg 2 SiO 4 Mg 2 SiO 4 + MgO

9. SiC SiO MgSiO 3 + SiO 2 MgSiO 3 + Mg 2 SiO 4 Mg 2 SiO 4 + MgO

10. SiC SiO MgSiO 3 + SiO 2 MgSiO 3 + Mg 2 SiO 4 Mg 2 SiO 4 + MgO

11. SiC SiO MgSiO 3 + SiO 2 MgSiO 3 + Mg 2 SiO 4 Mg 2 SiO 4 + MgO

12. SiC SiO MgSiO 3 + SiO 2 MgSiO 3 + Mg 2 SiO 4 Mg 2 SiO 4 + MgO WARNING: SOMEWHAT CONTROVERSIAL

13. SiC SiO MgSiO 3 + SiO 2 MgSiO 3 + Mg 2 SiO 4 Mg 2 SiO 4 + MgO

14. Chemistry meets Dynamics Most dynamical studies of planetesimal formation have neglected chemical constraints Most chemical studies of planetesimal formation have neglected specific dynamical studies Combine dynamical models of terrestrial planet formation with chemical equilibrium models of the condensation of solids in the protoplanetary nebulae

15. Dynamical simulations “produce” the terrestrial planets Use very high resolution n-body accretion simulations of terrestrial planet accretion (e.g. O’Brien et al. 2006) Incorporate dynamical friction Start with 25 Mars mass embryos and ~1000 planetesimals from 0.3 AU to innermost giant planet Neglects mass loss

16. Equilibrium thermodynamics predict bulk compositions of planetesimals Use spectroscopic photospheric abundances of 16 elements: H, He, C, N, O, Na, Mg, Al, Si, P, S, Ca, Ti, Cr, Fe, Ni Assign each embryo and planetesimal a composition based on formation region Adopt radial P-T profiles Assume no volatile loss during accretion, homogeneity and equilibrium is maintained

17. Equilibrium thermodynamics predict bulk compositions of planetesimals

18. Extrasolar “Earths” Terrestrial planets formed in ALL systems studied Most <1 Earth-mass Often multiple terrestrial planets formed

19. Extrasolar “Earths” Examine three ESP systems HD72659 – 0.95 M SUN G star, [Fe/H] = -0.14 3.30 M J planet at 4.16AU Gl777A – 1.04 M SUN G star, [Fe/H] = 0.24 0.06 M J planet at 0.13AU 1.50 M J planet at 3.92AU HD108874 – 1.00 M SUN G star, [Fe/H] = 0.23 1.30 M J planet at 1.05AU 1.07 M J planet at 2.75AU

20. Gl777 SiC SiO MgSiO 3 + SiO 2 MgSiO 3 + Mg 2 SiO 4 Mg 2 SiO 4 + MgO HD72659 HD108874

21. HD72659

22. 1.03 M Earth 0.95AU C/O = 0.40

23. Gl777

24. 1.10 M Earth 0.89AU C/O = 0.78

25. HD108874

26. 0.46 M Earth 0.38AU C/O = 1.35

27. HD72659Gl777HD108874 1.03 M Earth 0.95AU C/O = 0.40 1.10 M Earth 0.89AU C/O = 0.78 0.46 M Earth 0.38AU C/O = 1.35

29. What About Migration? Giant planet migration is believed to have occurred in many extrasolar planetary systems. Migration can move a large amount material both inwards and outwards → possibly change final planet composition.

30. Consider Three Scenarios 1.In-Situ formation (Jupiter-mass body doesn’t migrate from 1AU) 2.Jupiter-mass body migrates from 5AU to 1AU 3.Jupiter-mass body migrates from 5AU to 0.25AU

31. Consider Three Compositions 1.Solar 2.Gl777 (C/O = 0.78) 3.HD4203 (C/O = 1.85)

32. Solar Composition:

33. Gl777 Composition:

34. HD4203 Composition:

35. Water? Water is primarily present as water ice and serpentine Significantly less water in high C/O systems –Less water ice –Restricted water vapor distribution

36. Water? Migration can deliver massive amounts of water to the “dry” inner regions of the planetary systems. In-situ – no water delivered Migration – water and hydrous phases delivered to inner regions, refractories delivered to outer regions

37. Water?

38. Example: 3.05 M Earth at 0.91AU

39. Atmospheres Atmospheric formation is a complex process combining capture, outgassing, loss, etc. For close in planets with T eff > 1000K (within about 0.1AU), we can approximate an atmospheric composition by assuming equilibrium between the crust and atmosphere

40. Atmospheres T eff ~ 950KT eff ~ 270K

41. Atmospheres Solar Composition: 79% H 2 20% H 2 O 1% H 2 S CO and CO 2 with ices HD4203: 53% CO 42% H 2 21% CO 2 17%H 2 O 0.5%CH 4

42. Atmospheres Taken from Lissauer et al., 2011.

43. Biological Elements Lacking biological elements –N & P missing on all –H missing on in-situ Possible alternative delivery through migration and volatiles?

44. Biological Elements Condensates, Clathrates & Hydrates: CH 3 OHNH 3 CO 2 H 2 SPH 3 CH 4 CON 2 STAY TUNED!

45. Terrestrial Planets are likely to be relatively common Large range of stellar compositions suggests a wide range of terrestrial planets Final planet compositions depend somewhat on giant planet migration history Wide variety of biological, chemical and planetary implications

46. Frank Zappa There is more stupidity than hydrogen in the universe, and it has a longer shelf life. Frank Zappa