1. WHAT MOLECULAR ABUNDANCES CAN TELL US ABOUT THE DYNAMICS OF STAR FORMATION Konstantinos Tassis Collaborators: Karen Willacy, Harold Yorke, Neal Turner (JPL/Caltech) Talayeh Hezareh (MPIfR) University of Crete

2. The Initial Stages of Star Formation How do cores form? Molecular clouds mainly magnetically supported Turbulence (sub-)Alfvenic Ambipolar Diffusion –Damps MHD turbulence below a critical scale (cloud fragmentation) –Formation of magnetically supercritical cores Supercritical cores contract dynamically Eventually, hydrostatic protostars are formed Molecular clouds supported by turbulence Turbulence (super-)Alfvenic magnetic fields weak Overdensities created by compression in converging flow regions –Some become jeans unstable (collapse) –Some reexpand (transient clumps) Eventually, hydrostatic protostars are formed in the collapsing cores Strong B FieldWeak B Field

3. Produce Toolkit for Connecting Observations to Theories Chemistry + Dynamics + Radiative Transfer + Free Parameters + Projection Effects  Observables Produce database of observables from all combinations Make freely available, easily accessible Uses for such a database: –Identify observables that discriminate between theories –Design observing strategies, future observatories –Provide initial conditions for star and planet formation

4. Coupling of chemistry and dynamics With B field No B field Dynamics (Fg, P) Dynamics (Fg, P) ρ,t ΧsΧs ΧsΧs Dynamics (Fg, P, F B ) Dynamics (Fg, P, F B ) ρ,t ΧsΧs ΧsΧs XeXe Chemistry affected by Dynamics but dynamics not affected by chemistry Chemistry affected by dynamics and vice versa when B-field included Ambipolar drift and other non-ideal MHD phenomena depend sensitively on chemistry

5. First Step: The Chemical Network 78 gas phase species + 33 grain ice mantle species (H, He, C, N, O, Si), 1553 reactions from UMIST Embedded cores (A v ≥ 3 mag), CO self-shielding Grains: MRN distribution of grains, negatively charged, fixed abundance, Grain Processes: freezeout, thermal desorption, cosmic-ray heating, & surface reactions Non-Equilibrium chemistry

6. First Step: Collection of Models Evolution Time: M/Φ in magnetic models Initial support phase in non-magnetic models CR ionization rate Elemental C/O Temperature Spherical Hydro Axially Symmetric 2fluid MHD

7. Degeneracies in Unresolved Cores Large chemical differentiation Large degeneracies Weak evolution: Average abundances dominated by the lower density outer parts Important Vs. Unimportant Magnetic Field: average chemical abundances cannot proclaim a winner Important Vs. Unimportant Magnetic Field: average chemical abundances cannot proclaim a winner

8. Central Parts Evolve n c = 10 4 cm -3 n c = 10 6 cm -3

9. Depletion Measure Fast – Slow contraction models clearly separated for: CO, HCO +, CO 2, NO, N 2 H + Model degeneracies for: CN, HCN, NH 3, H 2 CO, CH Important Vs. Unimportant Magnetic Field: observable Δ could tell them apart Important Vs. Unimportant Magnetic Field: observable Δ could tell them apart

10. Interesting Abundance Ratios Chemical Chronometers? Tassis, Willacy, Yorke, & Turner 2012, ApJ, 753, 29 Chemical Chronology: possible but rough Chemical Chronology: possible but rough

11. Coexistence of HCO+/HCN Ion-Neutral Pair used as a probe of AD Tassis, Hezareh, Willacy 2012

12. Other co-spatial Ion-Neutral Pairs: HCO+/CO Tassis, Hezareh, Willacy 2012

13. Other co-spatial Ion-Neutral Pairs: HCO+/NO Tassis, Hezareh, Willacy 2012

14. Other co-spatial Ion-Neutral Pairs: NO+/NO Tassis, Hezareh, Willacy 2012 3 new molecule pairs make direct AD observations possible 3 new molecule pairs make direct AD observations possible

15. The future Expand chemistry to include deuterated molecules, 10x reactions Advance to higher dimensionality models Predictions for line profiles (radiative transfer) Make results available online @ U. of Crete servers