1. X-Ray Emission from Planetary Nebulae and Their Central Stars: A Status Report Joel Kastner Rochester Institute of Technology w/ help from lots of other folks, including: Rudy Montez, Young Sam Yu (RIT grad students) Noam Soker, Ehud Behar, Bruce Balick, Adam Frank, Eric Blackman, Orsola DeMarco, Pat Huggins…

2. Chandra & XMM-Newton: The story so far Since 2000, X-ray imaging of PNe by the Chandra and XMM-Newton X-ray observatories has provided new & compelling observational evidence for hot bubbles, highly energetic jets, and/or “active” PN cores –Eight planetaries observed by Chandra and XMM have been detected as diffuse X-ray sources thus far Kastner et al. (2000, 2001, 2003); Chu et al. (2001); Montez et al. (2005); Guerrero et al. (2002, 2005); Gruendl et al. 2006) –An additional handful have been detected as X-ray point sources e.g. NGC 6534, 7293; Guerrero et al. (2001)

3. X-rays and the structure of PNs Two key areas where Chandra & XMM-Newton X-ray imaging spectroscopy observations yield important/unique insight into PN shaping: 1. Diffuse X-ray sources: origin and evolution of wind interaction regions X-ray hot bubbles: quasi-spherical central star wind interacting w/ former AGB wind –a la Kwok et al. 1978 Collimated, X-ray-luminous outflows & jets: evidence for disks and/or binarity –Subject of next talk by M. Guerrero; also see poster by R. Montez 2. Central X-ray point sources: magnetic fields, disks, and binarity in PN cores

4. 1. Diffuse X-ray sources in PNs Two “classes” emerging: –Hot bubbles BD+303639; NGC 40, 2392, 3242, 6543, 7009, 7026 –Collimated jets & outflows NGC 7027, Menzel 3, Hen 3- 1475 NGC 2346 is an X-ray NONdetection (Gruendl et al. 2006) X-ray images (blue): XMM & Chandra X-ray/visual image overlays: M. Guerrero Montage: B. Balick

5. You Won’t Believe This… Chandra target: the WR-type PN Hen 2-99 …not detected… But a second WR-type PN, NGC 5315, is in the field: and it’s detected! NGC 5315 spectrum shows enhanced Ne, depleted Fe…just like BD +303639 (see poster by Young Sam Yu)

6. Diffuse X-ray sources: properties “Hot Bubbles” Object V w (km/s) dM/dt (M sun /yr) T x (K) L x (erg/s) WR type? H2?H2? NGC 5315*24001.5x10 -6 2.6x10 6 2.2x10 32 Y… BD +3036397001.6x10 -6 2.7x10 6 1.6x10 32 YY NGC 702635004.6x10 -7 1.1x10 6 1.5x10 32 YN NGC 654319004.0x10 -8 1.7x10 6 1.0x10 32 Y*N NGC 700927003.0x10 -10 1.8x10 6 3.0x10 31 NN NGC 23924201.8x10 -8 2.0x10 6 2.6x10 31 NN NGC 4010001.8x10 -6 8.0x10 5 1.5x10 30 YN NGC 3242……(Unpubl.) NN “Jets” Object V w (km/s) T x (K) L x (erg/s) WR type? H2?H2? NGC 7027…3.0x10 6 1.2x10 32 …Y Hen 3-147523005.0x10 6 4.0x10 31 N… Menzel 3400:6.0x10 6 2.4x10 31 NY * ”Hot bubble” discovered spectroscopically; requires spatial confirmation via on-axis Chandra imaging

7. Characteristics of planetaries that are diffuse X-ray sources Hot bubble sources: –High frequency of WR-type central stars Large L w (i.e. large product dM/dt x V w 2 ) –“Closed” morphologies No classical bipolars among hot bubble X-ray sources Only one hot bubble X-ray source is also an H 2 source –Dense, dusty molecular tori are rare Collimated outflow & Jet sources: –High frequency of H 2 detections Dense, dusty molecular tori are common –Higher T x than hot bubble sources?

8. Hot bubble X-ray sources: trends X-ray temperature and present central star V w are uncorrelated –Other effects (evolution of V w, heat conduction, adiabatic cooling, …) are important Weak correlation between L x and L w –However, NGC 40 is a conspicuous outlier

9. Hot bubble X-ray sources: trends (cont.) Both T x and L x are anticorrelated w/ central bubble radius –Are we seeing the temporal evolution of PN hot bubbles? And has NGC 40’s bubble recently “popped”?

10. 2. X-ray Point Sources at PN cores We have been systematically revisiting all Chandra observations of PNe to place constraints on pt. source X-ray luminosities –~0.5” spatial resolution of Chandra essential to distinguish between diffuse & pt.-like emission –Technique: determine X-ray flux (or background noise level, i.e. upper limits) within Chandra PSF at position of PN central star

11. Results: X-ray Point Sources at PN cores Point sources detected in ~30% of PNe observed by Chandra (not including symbiotic Mira systems) –Detections (4): NGC 246, 4361, 6543, 7293 Typical Lx ~ 10 30-31 erg/s NGC 246, 4361 far softer than typical coronal sources –Nondetections (10): NGC 40, 3132, 7027; BD+30; Hen 2-99, 3-1475; M 1-16, 2-9; MyCn 18; Water Lily Typical Lx limits: < 10 29-30 erg/s

12. PN X-ray pt sources vs. T Tauri stars (Orion cluster T Tauri X-ray luminosities: Feigelson et al. 2005) Orion TTS: <0.3 M o 0.3-1.0 M o 1.0-3.0 M o PN nondetections (~70%) Comparison suggests that cores of many (most?) PNs – including some in classical bipolars - are neither highly magnetic nor display significant star-disk magnetic interactions.

13. X-ray point sources are common (ubiquitous?) among symbiotic Miras X-ray pt. sources detected in 5 of 6 systems –R Aqr, CH Cyg, Hen 2- 104, Mz 3, & Mira itself OH 231.8+4.2 only nondetection: X-rays highly absorbed? –Wide range of (highly variable) source L x ~ 10 28 erg/s to ~ 10 32 erg/s R Aqr (Chandra & NOT) (Thanks, Romano…) Menzel 3 (Chandra & HST) Blue: optical Red: X-rays

14. X-rays from PNe: Summary Diffuse X-ray sources –PNe w/ “hot bubble” X-ray emission tend to have closed morphologies and very energetic present-day central star winds Wind “inflates” and heats bubble, which eventually pops…? –But T x and L x better correlated with bubble size (therefore age) than present central star wind velocity or wind kinetic energy Supports models in which X-ray bubble is initiated very early in PN evolution and/or mechanisms like heat conduction can moderate T x X-ray point sources –Majority of “classical” PNs lack them suggests central star systems are usually magnetically inactive –Symbiotic Miras almost always have them Indicative of star-disk interactions and/or accretion onto central WD companions?