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Lecture 10: Bubbles and PNe September 26, 2011

Lecture 10: Bubbles and PNe September 26, 2011. III. Conduction Layer. Probe the thermal conduction layer High ions produced by thermal collisions. O VI N V C IV Si IV. UV Probes of the 10 5 K Gas. C IV N V O VI

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Lecture 10: Bubbles and PNe September 26, 2011

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  1. Lecture 10:Bubbles and PNeSeptember 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 105 K Gas C IV N V O VI ll (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105 1.8105 3.0105 Teff (K) >35,000 >75,000 >125,000

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

  5. S 308 - ideal for conduction study 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. HD 50896 * R: HG: [O III]B: X-ray

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

  12. Hot Gas in Planetary Nebulae X-ray emission detected by Chandra & XMM-Newton 2.7x106 K 3.0x106 K 1.7x106 K T = 1-3 x 106 K n  100 cm-3

  13. To Ensure Detection of Diffuse X-rays • Closed shell or lobes to confine hot gas. • Stellar winds – P Cygni profiles • Nearby, no large extinction • 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

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

  15. O VI of PNe detected in X-rays

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

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

  18. 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

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