The Fossil History of the Solar System: Links to Interstellar Chemistry Edwin A. Bergin University of Michigan Jeong-Eun Lee UCLA James Lyons UCLA

Background: Oxygen Isotopes in the Solar System 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 16 O/ 17 O  2600

Background: Oxygen Isotopes in the Solar System 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 –so if you plot  ( 17 O/ 16 O)/  ( 18 O/ 16 O) then the slope would be 1/2 for more information see Clayton 1993, Ann. Rev. Earth. Pl. Sci.

Oxygen Isotopes in Meteorites In 1973 Clayton and co-workers discovered that calcium- aluminum-rich inclusions (CAI) in primitive chondrite meteorites had anomalous oxygen isotopic ratios. Definition: SMOW = standard mean ocean water -  ( 18 O) =  ( 17 O) = -50

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 meteoritic results can be from mixing of 2 reservoirs Terrestrial line Meteoritic line

Wither the Sun? Considerable controversy regarding the Solar oxygen isotopic ratios. 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

Theory: Isotope Selective Photodissociation Line DissociationContinuum Dissociation van Dishoeck and Black 1988H 2 O: Yoshino et al 1996+

How Does Isotope Selective Photodissociation Work? Line Dissociation van Dishoeck and Black 1988

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

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) –credible solution –mixing may only be active on surface where sufficient ionization is present –cannot affect Solar oxygen isotopic ratio active on cloud surface and provided to disk (Yurimoto and Kuramoto 2004) –did not present a detailed model –can affect both Sun and disk

Model chemical-dynamical model of Lee, Bergin, and Evans 2004 –cloud mass of 1.6 M ◉ –approximate pre-collapse evolution as a series of Bonner-Ebert solutions with increasing condensation on a timescale of 1 Myr –use Shu 1977 “inside-out” collapse model –examine evolution of chemistry in the context of physical evolution (i.e.. cold phase - star turn on - warm inner envelope) –vary strength of external radiation field -- parameterized as G 0, where G 0 = 1 is the standard interstellar radiation field. two questions –what level of rare isotope enhancement is provided to disk? –what is provided to Sun? Time Density Gas shielding

Basic Chemistry

 18 O Evolution with a Range of UV Enhancements

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 - it is 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.

Particle Drift in Viscous Disks Gas orbits more slowly than solids at a given radius –results in a headwind on particles that causes them to drift inwards Drift velocity depends on size –small grains (<< 1 cm) are coupled to the gas –meter-sized particles are the most rapidly drifting –large planetesimals experience decreasing drift speeds with size Inner nebula can be enriched in water vapor as icy bodies rapidly advect inward and evaporate inside the snow line. Cuzzi & Zahnle 2004 We are now seeing evidence for singificant dust evolution in systems as young as 1 Myr… (Bergin et al. 2004, Calvet et al. 2005; Furlan et al. 2006

Model Infall

Model Infall

Model Infall Ice coated grains sink to midplane make rocks, which feel headwind and fall into star

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). –time that rocks are formed and fractionation begins is a variable –after fractionation begins assume that water is enhanced over CO by a factor of constraints –meteoritic and planetary isotope ratios –the solar oxygen isotope ratios

The Solar Oxygen Isotope Ratio M f = amount of solar mass affected by fractionation M f = 0.1 assumes that fractionation begins 4 x 10 5 yrs after collapse G 0 = 0.4 G 0 = 10 G 0 = 10 3 G 0 = 10 5  ( 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 ◉ 1.8x x x10 5 time fractionation starts

Oxygen Depletion in the Inner Disk Have 3 potential solutions with variable radiation field that depend on the solar value Either: –Sun formed in a cluster with an O star –Sun formed bathed in a weak to moderate UV field What about the rocks? –over time the inner nebula becomes depleted in enriched water vapor and enhanced in CO vapor with low isotopic ratios –need a continuous source of replenishment of ices with highly enriched isotope ratios

Looking Back in Time: 1 Myr Before the Sun was Born The solar oxygen isotope ratio is uncertain –2 disparate solutions - each with significant implications for the formation of our Solar System 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 ; Tachibana et al. 2006) –taken as strong evidence that Sun formed in a stellar cluster near an O star We suggest that oxygen isotopes provide independent supporting evidence for 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

What is Provided to the Disk? 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  M ◉ 1.8x x x10 5 time fractionation starts