1. Oxygen Isotopes Anomalies of the Sun and the Original Environment of the Solar System Jeong-Eun Lee UCLA

2. collaborators  Edwin A. Bergin (Univ. of Michigan)  James R. Lyons (UCLA)

4.  Matter from stars (stellar winds of red giant stars and supernova explosions) is expelled to ISM.  The molecular clouds are sites for star formation.  Extensive chemical and physical processing of materials in the Solar nebula and planetary bodies destroys the ISM heritage.  But: Asteroids and comets have escaped significant alteration by the reprocessing. Primitive bodies such as comets, meteorites, and IDPs possibly preserve the oldest solar system solids material to provide opportunities to probe the astrophysical environment when the Sun formed. Primitive bodies such as comets, meteorites, and IDPs possibly preserve the oldest solar system solids material to provide opportunities to probe the astrophysical environment when the Sun formed. The solar system and ISM

5.  Complete isotopic homogenization is expected from the chemical and physical processing of solar system materials.  Thus: any surviving presolar material will have an exotic isotopic composition, which could not have resulted from processes occurring in the solar system. Exotic Isotopic Ratios measured from IDPs, Meteorites, and Comets (connected to ISM): D/H, 15 N/ 14 N, 18 O/ 16 O ( 17 O/ 16 O) D/H, 15 N/ 14 N, 18 O/ 16 O ( 17 O/ 16 O) Isotopic Anomalies

6. Oxygen Isotopes  Oxygen isotope production 16 O produced in stellar nucleosynthesis by He burning  provided to ISM by supernovae rare isotopes 17 O and 18 O produced in CNO cycles  novae and supernovae  Expected that ISM would have regions that are inhomogeneous  Is an observed galactic gradient (Wilson and Rood 1992)  Solar values 16 O/ 18 O  500 and 17 O/ 18 O  2600

7. Oxygen Isotopes  chemical fractionation can also occur in ISM  except for H, kinetic chemical isotopic effects are in general of order a few percent  distinguishes fractionation from nuclear sources of isotopic enrichment  almost linearly proportional to the differences in mass between the isotopes  Ex: a chemical process that produces a factor of x change in the 17 O/ 16 O ratio produces a factor of 2x change in the 18 O/ 16 O ratio  so if you plot  ( 17 O/ 16 O )/  ( 18 O/ 16 O ) then the slope would be 1/2

8. Oxygen Isotopes in Meteorites  In 1973 Clayton and co-workers discovered that calcium- aluminum-rich inclusions (CAI) in primitive meteorites had anomalous oxygen isotopic ratios.

9. Oxygen Isotopes in Meteorites  Earth, Mars, Vesta follow slope 1/2 line indicative of mass- dependent fractionation  primitive CAI meteorites (and other types) follow line with slope ~ 1 indicative of mass independent fractionation Terrestrial line Meteoritic line SMOW = standard mean ocean water

10. Oxygen Isotopes in Meteorites meteoritic results can be from mixing of 2 reservoirs Terrestrial line Meteoritic line - 16 O poor - 16 O rich Solar value? -The initial value of molecular cloud

11. 2 Disparate Measurements:   18 O =  17 O = -50 per mil  lowest value seen in meteorites  seen in ancient lunar regolith (exposed to solar wind 1-2 Byr years ago; Hachizume & Chaussidon 2005)   18 O =  17 O = 50 per mil  contemporary lunar soil (Ireland et al. 2006)  differences are very difficult to understand. Huss 2006 Considerable controversy regarding the Solar oxygen isotopic ratios. Oxygen Isotopes in the Sun

12. Theory  stellar nucleosynthesis  lack of similar trend seen in other elements  chemical reactions that are non-mass dependent (Thiemens and Heidenreich 1983)  known to happen in the Earth’s atmosphere (for ozone)  no theoretical understanding of other reactions that can link to CO and H 2 O  photo-chemical CO self-shielding  suggested by Clayton 2002 at in the inner nebula at the edge of the disk (X point)  active on disk surface (Lyons and Young 2005)  active on cloud surface and provided to disk (Yurimoto and Kuramoto 2004)

13. CO Photodissociation and Oxygen Isotopes 0.5 < A v < 2 C 18 O + h -> C + 18 O C 16 O 18 O + gr -> H 2 18 O ice C 16 O + h -> C + 16 O C 18 O + h -> C + 18 O A v < 0.5 A v > 2 C 16 O C 18 O

14. CO Self-Shielding Models  active in the inner nebula at the edge of the disk (Clayton 2002)  only gas disk at inner edge, cannot make solids as it is too hot  active on disk surface and mixing to midplane (Lyons and Young 2005)  mixing may only be active on surface where sufficient ionization is present  cannot affect Solar oxygen isotopic ratio

15. CO Self-Shielding Models  active on cloud surface and provided to disk (Yurimoto and Kuramoto 2004)  did not present a detailed model  can affect both Sun and disk

16. Model  chemical-dynamical model of Lee, Bergin, and Evans 2004  use Shu 1977 “inside-out” collapse model  cloud mass of 3.6 M ◉  approximate pre-collapse evolution as a series of Bonner- Ebert solutions with increasing condensation  examine evolution of chemistry in the context of physical evolution  model updated to include CO fractionation and isotopic selective photodissociation  two questions  what level of rare isotope enhancement is provided to disk?  what is provided to Sun?

17. Temperature and Density Evolution in the Model

19.  18O Evolution with a Range of UV Enhancements

20. Issues  large enhancements in  18 O and  17 O are provided to the disk at all radii in the form of water ice.  This material is advected inwards and provided to the meteorite formation zone (r < 4 AU).  BUT: - the gas has an opposite signature - enriched in 16 O in the form of CO - gas and grain advection in the disk must be decoupled in some way to enrich inner disk in heavy oxygen isotopes relative to 16 O Icy grains drift inward due to gas drag (Cuzzi et al. 2004) Gas orbits more slowly than solids at a given radius Gas orbits more slowly than solids at a given radius –results in a headwind on particles that causes them to drift inwards

21. Model  Assume material provided at inner radius of our model (100 AU) is advected unaltered to the inner disk  Assume significant grain evolution has occurred and material fractionation has occurred (gas/ice segregation) in the disk.  time this fractionation begins is a variable  after fractionation begins assume that water is enhanced over CO by a factor of 5 - 10  constraints  the solar oxygen isotope ratios  the solar C/O ratio - need to assume (C/O) initial > (C/O) ◉

22. The Solar Oxygen Isotope Ratio M f = amount of solar mass affected by fractionation M f = 0.1 if fractionation begins 4 x 10 5 yrs after collapse  ( 18 O) ◉ = 50 per mil implies a slightly enhanced UV field (G 0 = 10) with M f ~ 0.1 M ◉  ( 18 O) ◉ = -50 per mil implies a weak (G 0 = 1) or a strong UV field (G 0 = 10 5 ) with M f ~ 0.1 M ◉ 1.8x10 5 2.7x10 5 3.6x10 5 time fractionation starts G 0 = 0.4 G 0 = 10 G 0 = 10 3 G 0 = 10 5

23. The solar C/O ratio G 0 = 0.4 G 0 = 10 G 0 = 10 3 G 0 = 10 5 All relevant solutions G 0 = 0.4, 10, and 10 5 can match solar C/O ratio if M f ~ 0.05 - 0.1 M ◉ 1.8x10 5 2.7x10 5 3.6x10 5 time fractionation starts

24. More constraints on G 0  Have 3 potential solutions with variable radiation field that depend on the solar value More constraints?  meteoritic and planetary isotope ratios  water ices in comets… Go=10 5 !!!

25. Our model of oxygen isotopes suggests the presence of a massive O star in the vicinity of the forming Sun 1 million years before collapse and that the Solar value is  ( 18 O) ◉ = -50 per mil. Our model of oxygen isotopes suggests the presence of a massive O star in the vicinity of the forming Sun 1 million years before collapse and that the Solar value is  ( 18 O) ◉ = -50 per mil. Looking Back in Time: Before the Sun was Born

26.  Recently the presence of the extinct radionuclide 60 Fe (  1/2 = 1.5 Myr) is inferred in meteorites with varied composition (Tachibana & Huss 2003; Mosteraoui et al. 2005; Tachibana et al. 2006)  cannot be produced by particle irradiation  abundance consistent with production in nucleosynthesis in a Type II supernova or an intermediate-mass AGB star and provided to the solar system before formation  probability of an encounter between Sun and intermediate mass AGB star is low (< 3 x 10 -6 ; Tachibana et al. 2006)  taken as strong evidence that Sun formed in a stellar cluster near an O star