1. Kinematics & Dynamics of Disk Galaxies James Binney Oxford University

2. Outline Spiral structure Warps Mass of the gas disk Baryon domination Bar-halo interaction Bars & pseudobulges

3. Spiral Structure More than icing on the cake It heats the disk Dehnen & Binney 98

4. & structures it Famaey et al 04 Dehnen 1998

5. Rag-bag streams Hyades-Pleiades gp (red) not coeval Sirius gp (magenta) lower Z and even wider dispersed ages Hercules gp (green) Si gp

6. Stream assembly Sellwood & Binney (02) Set up disk to excite single transient pattern

7. S&B (02) E-  p L=const Stars cross CR on horse-shoe orbits

8. S&B (02) Heating restricted to ILR

9. Unconstrained simulation NGC 4062 in H Puerari et al 2000

10. S&B (02) Result: much migration Impacts Z distribution in solar nhd

11. (04)

12. Impact on gas Gas clouds should also migrate Will reduce metallicity gradients Need to revisit models of chemical evolution (Schoenrich 06)

13. Warps Warps long thought to be probe of DM halos (Binney 78…) Key fact: halos are responsive Halo @ r quickly aligns with disk @ r (& becomes misaligned with halo at r’) NGC 5055 by Tom Oosterloo

14. Consequently, normal-mode theory fails (Binney Jiang & Dutta 98) Lines of nodes

15. BJD (98) Warp doesn’t damp; it winds up

16. So what is the answer? Jiang & Binney (99) generated a warp by adding halo particles in an inclined torus Shen & Sellwood (05) do a similar job with higher precision: larger disk, of stars not rings, tenfold increase in # halo stars, larger torus

17. Shen & Sellwood (05) NGC 4013 from Bottema (96)

18. Key is to apply torque to outer disk by distorting outer halo Changes in cosmic inflow pattern will do this Precession of torqued disk/inner-halo generates leading spiral in outer lon Briggs (90) rules obeyed Has MOND an equally plausible explanation?

19. The Gas Disk Is the gas disk really the more fundamental? NGC 2403 by Tom Oosterloo

20. Gas Gas is the source of new stars and thus spirals How much is there? How much H 2 ? HI correlated with FUV Is HI just a photo-dissociated skin on H 2 ? (Allen et al 97; Allen 2004) M101 HI + FUV (Braun)

21. Stars far out Young stars (& dust) seen at 23-33 kpc in M31 (Cuillandre et al 02) Stars traced to 10R d in NGC 300 (Bland-Hawthorn et al 05) Stars surely form from cold dense gas Thus from H 2 Is there serious gas mass in extended disks?

22. Remember HI scaling (Swaters 99, Hoekstra et al 01)

23. Conclusions Spirals don’t just heat, they churn the disk Effects visible in local n(v) Phenomenon has big implications for (i) diagnosing local spiral structure (ii) models of chemical evolution Warps almost certainly reflect misalignment of inner & outer halo Plausibly generated by cosmic infall There must be H 2 outside the optical disk; could it be dynamically important?