1. Lecture 10: Bubbles and PNe September 26, 2011

2. III. Conduction Layer - Probe the thermal conduction layer High ions produced by thermal collisions O VI N V C IV Si IV

3. UV Probes of the 10 5 K Gas C IV N V O VI  Å )  1548, 1550 1238, 1242 1031, 1037 Obs. HST STIS HST STIS FUSE I.P. (eV) 47.9 77.5 138.1 T (K) 1.0  10 5 1.8  10 5 3.0  10 5 T eff (K) >35,000 >75,000 >125,000

4. Interface of the WR Bubble S308 C IV Boroson et al. 1997, ApJ, 478, 638 N V S II

5. S 308 - ideal for conduction study HD 50896 * R: H  G: [O III] B: X-ray Boroson et al. (1997) detected N V absorption from the conduction layer. HST STIS observation of N V and C VI emission was scheduled, but STIS died. FUSE observations of O VI were awarded, and it died, too. Spitzer can observe Ne V, but it ran out cryogen.

6. FUSE Observations of NGC 6543 Gruendl, Chu, Guerrero 2004, ApJL

7. III. Conduction Layer - Probe the thermal conduction layer High ions produced by thermal collisions - NGC 6543: given the boundary conditions of hot interior and warm shell, thermal conduction appears to be consistent, but does not explain the low X-ray luminosity. Gruendl, Chu, Guerrero 2004, ApJL

8. Stars and Nebulae: Evolving Together Steffen & Schönberner (2006)

9. Stars and Nebulae: Evolving Together Steffen & Schönberner (2006)

10. Interacting-Wind Model of PNe

11. Hot Gas in Planetary Nebulae Guerrero et al. (2005) Chu et al. (2001) Gruendl et al. (2006) NGC 2392 NGC 6543 NGC 7026 X-ray emission detected by Chandra & XMM-Newton

12. Hot Gas in Planetary Nebulae X-ray emission detected by Chandra & XMM-Newton T = 1-3 x 10 6 K n  100 cm -3 3.0x10 6 K2.7x10 6 K 1.7x10 6 K

14. To Ensure Detection of Diffuse X-rays 1.Closed shell or lobes to confine hot gas. 2.Stellar winds – P Cygni profiles 3.Nearby, no large extinction 4.OVI, NV lines from interface layer NGC 246, NGC 3132 - no high ions, no X-rays High ions and diffuse X-rays from IC 418, NGC 2392, NGC 6826, NGC 7009

15. FUSE - Nebular OVI Emission NGC 7293 (Helix)NGC 6543 (Cat’s Eye) Stellar P Cygni profile  fast stellar wind Nebular O VI emission  hot gas from shocked wind O VI 1032 O VI 1037 Inside Nebula Outside Nebula Star Ly  1026

16. O VI of PNe detected in X-rays

17. O VI of PNe not detected in X-rays

18. Pressure-driven bubble with heat conduction at interface Bubble dynamics does not match L x (obs) / L x (expected) = 10 -1 to 10 -3  Adjust fast wind - wind velocity - mass loss rate  Reduce heat conduction Dynamically mix nebular material (mass-loading)  

19. What Next? Swept-up Shell Reasonably well understood Interface (conduction) layer Spatially-resolved high-dispersion UV spectra are needed Hot interior Spatially-resolved high-resolution X-ray spectra are needed