1 / 41

Injection of Small Bodies into the ISM by Planetary Nebulae.

Injection of Small Bodies into the ISM by Planetary Nebulae. Bob O’Dell University of Chicago 18 April 2007. NGC 6720- The Ring Nebula. IC 4406- The Retina Nebula. NGC 2392 The Eskimo Nebula. NGC 6853 WFPC2. Final.Dec16XV.tif. Helix-Both FOV. Helix Close-up. Helix-Very Closeup.

marrim
Télécharger la présentation

Injection of Small Bodies into the ISM by Planetary Nebulae.

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Injection of Small Bodies into the ISM by Planetary Nebulae. Bob O’Dell University of Chicago 18 April 2007

  2. NGC 6720-The Ring Nebula

  3. IC 4406-The Retina Nebula

  4. NGC 2392The Eskimo Nebula

  5. NGC 6853 WFPC2

  6. Final.Dec16XV.tif

  7. Helix-Both FOV

  8. Helix Close-up

  9. Helix-Very Closeup

  10. Helix CharacteristicsDistance=213 pc. Angular Size~10’Age ~15,000 yearsWell imaged in optical lines (HST-ACS & CTIO-MOSAIC), infrared (HST-NIC3-H2), and Radio (21-cm of HI, CO)

  11. Ionization Structure

  12. GO 9489 Slit

  13. Slitless.fourlines

  14. NewProfiles

  15. HenneyConstTemp

  16. HenneyVariableT

  17. Predicting the Surface Brightness of the Knot Cusps. • The most simplistic model argues that the surface brightness should drop with r-2, which meant this should be the upper limit to an observed SH~-2 relation.

  18. ObservedSurface Brightness

  19. Predicting the Surface Brightness of the Knot Cusps. • The most simplistic model argues that the surface brightness should drop with r-2, which meant this should be the upper limit to an observed SH~-2 relation. • Due to advection of neutral material into the ionized cusp, not all photons reach the ionization front of the cusps (Lopez-Martin et al. 2001, ApJ, 548, 288) so that the upper limit should be lower.

  20. Predicted Surface Brightness

  21. Knot Characteristics • Total Number about 3,500-20,000. • Mass from extinction~3x10-5 Suns. • Total mass about 0.1-0.6 Suns. • The central star mass is about 0.6 Suns. • The original mass is about 3 Suns. • A significant and possibly majority fraction of the mass is concentrated in knots.

  22. Evolution of Knots • Initiated at the ionization front via an instability (R-T, Capriotti 1973). • Shaped by the radiation field of the star, starting out as broad and becoming comet-like in appearance.

  23. Final Evolution ofa Central Star.

  24. Shadows behind the Knots. • The first order theory has been worked out already (Canto et al. 1998, ApJ, 502, 695. • Since the knots are optically thick to LyC, they cast an ionization shadow. • Some ionization occurs because of LyC photons scattered by the ambient nebula.

  25. The Bulk of the Mass is in theNeutral Region of the Knots. • Densities inferred from the optical are about 106 cm-3. • Only one study of a heavy molecule (CO). • H2 is expected to be the dominant form of hydrogen in the outer parts of the knots.

  26. The Bulk of the Gas is in the Neutral Region and H2 is the strongest emission from there.

  27. The H2 Levels

  28. The NIC3 FOV inGO 10628

  29. Northern FOV inMultiple Lines.

  30. Profiles of 378-801 in the Emission Lines.

  31. Mechanisms Proposed to Power the H2 Emission. • Shocks driven by a high velocity wind from the central star.

  32. Mechanisms Proposed to Power the H2 Emission. • Shocks driven by a high velocity wind from the central star. • Pumping by the FUV continuum followed by decay (the Solomon process).

  33. The H2 Levels

  34. Mechanisms Proposed to Power the H2 Emission. • Shocks driven by a high velocity wind from the central star. • Pumping by the FUV continuum followed by decay (the Solomon process). • Photodissociation by x-rays followed by collisional heating of the gas.

  35. Mechanisms Proposed to Power the H2 Emission. • Shocks driven by a high velocity wind from the central star. • Pumping by the FUV continuum followed by decay (the Solomon process). • Photodissociation by x-rays followed by collisional heating of the gas. • Photodissociation by EUV (the LyC) followed by collisional heating.

  36. The Energy Balance. • IN: X-ray(<124 A) 4x10-11 ergs cm-2 s-1 • IN: FUV (912-1200 A) 7x10-9 ergs cm-2 s-1 • IN: EUV (124-912 A) 8x10-8 ergs cm-2 s-1 • Out: Ionized Gas Lines 5x10-9 ergs cm-2 s-1 • Out:H2 Emission Lines 4x10-9 ergs cm-2 s-1

  37. The Population Distribution.

  38. The EUV Driven Model. • This must have a density >105 cm-3. • It must have a collisionally heated gas of about 990 K. • It must have a zone where H2 still exists and yet there are LyC photons . • The key physics is in advection, which was necessary for explaining the surface brightness in Ha and the electron temperature increase in the ionized gas zone.

  39. Evolution of Knots-I • Will they survive the expulsion phase? • Almost certainly they will survive the high LyC luminosity phase of the central star since the photoevaporation time is about 15,000 years and it must decrease as the star gets fainter.

  40. Evolution of Knots-II • The question then is whether they will survive destruction by the diffuse UV radiation field of the ISM before being incorporated into GMC’s. • There is ample and growing evidence for small scale structures in the ISM. This process could be the source.

  41. Helix Reading • 3-D Model-O’Dell et al. 2004,AJ,128,2339& RMxAAC, 23, 5. • 3-D Model-Meaburn et al. 1998,MNRAS,294,201& 2005,MNRAS,360,963. • Knot Ubiquity-O’Dell et al. 2002,AJ,123,3329. • Knot Basics-O’Dell & Burkert, 1997,IAU180, 332. • Detailed Knot Modeling-O’Dell, Henney, & Ferland 2005,AJ,130,172. • H2 Observations-Meixner et al. 2005,AJ,130,1784. • H2 Energetics-O’Dell, Henney, & Ferland 2007, AJ, 133, 2343.

More Related