Talk at 12th Asia-Pacific Regional IAU Meeting (APRIM), Daejeon, Korea, August 20, 2014, https://doi.org/10.6084/m9.figshare.13698868

1. Kinematical Properties of
Kinematical Properties of
Planetary Nebulae
Planetary Nebulae
with WR-type Nuclei
with WR-type Nuclei
Ashkbiz Danehkar (Macquarie, Australia)
Ashkbiz Danehkar (Macquarie, Australia)
Wolfgang Steffen (UNAM, Mexico)
Wolfgang Steffen (UNAM, Mexico)
Quentin Parker (Macquarie/AAO)
Quentin Parker (Macquarie/AAO)
12
12th
th
Asia-Pacific Regional IAU Meeting , 19 August 2014, Daejeon, Korea
Asia-Pacific Regional IAU Meeting , 19 August 2014, Daejeon, Korea

2. • Introduction to Planetary Nebulae
Introduction to Planetary Nebulae
• Introduction to WR-type stars
Introduction to WR-type stars
• Planetary Nebula Morphology
Planetary Nebula Morphology
• Integral Field Spectroscopy
Integral Field Spectroscopy
• Discussion
Discussion
• Summary
Summary

3. Herwig 2005
NGC 6543

4. Why planetary nebula important?
• Chemistry
–Chemical contributors to the ISM
–Mixing processes at AGB phase
Life Elements
AGB Products

5. Why planetary nebula important?
• Morphology
–AGB mass-loss process
–Transition time from AGB to PN
–But, why most axisymmetric morphologies?

6. • Introduction to Planetary Nebulae
Introduction to Planetary Nebulae
• Introduction to WR-type stars
Introduction to WR-type stars
• PN Morphology
PN Morphology
• Integral Field Spectroscopy
Integral Field Spectroscopy
• Discussion
Discussion
• Summary
Summary

7. Central Stars of Planetary Nebulae
• Most H-rich surface abundances
• 25% H-deficient fast expanding atmospheres
• resembling massive Wolf-Rayet (WR) stars
• Most Carbon-sequence of Wolf-Rayet stars
• few Nitrogen-sequence of Wolf-Rayet stars
• few weak emission line stars (wels), weaker emission lines.
• some emission lines similar to PG 1159 star

8. Central Stars of PNe (CSPNe)
[WCL]
[WCL]
[WCE]
[WCE]
PG1159
PG1159
non-DAs
non-DAs
Bloecker 1995
• [WCL] late-type Teff = 20,000-80,000 K, V∞ =200-1000 km/s
• [WCE] early-type Teff = 80,000-150,000 K, V∞=1200-3500 km/s
• [WCL] → [WCE] → PG 1159 (Werner & Herwig 2006)

9. • Introduction to Planetary Nebulae
Introduction to Planetary Nebulae
• Introduction to WR-type stars
Introduction to WR-type stars
• Planetary Nebula Morphology
Planetary Nebula Morphology
• Integral Field Spectroscopy
Integral Field Spectroscopy
• Discussion
Discussion
• Summary
Summary

10. • Round (R) 22% of Galactic PNe
PN morphology
10
• Elliptical (E) 49%
• Bipolar/multi-polar/ring (B) 20%
• point-symmetric 10%

11. PN morphology
Balick et al. 1987,AJ,94,1641
• Round, Elliptical,
Bipolar/multipolar.
• Some included Point-
symmetric knots.

12. • Introduction to Planetary Nebulae
Introduction to Planetary Nebulae
• Introduction to WR-type stars
Introduction to WR-type stars
• Planetary Nebula Morphology
Planetary Nebula Morphology
• Integral Field Spectroscopy
Integral Field Spectroscopy
• Discussion
Discussion
• Summary
Summary

13. Integral Field Spectroscopy
Wide Field Spectrograph (WiFeS; Dopita 2007,2010):
• ANU 2.3-m Telescope, Siding Spring Observatory
• image-slicing Integral Field Unit (IFU)
• field-of-view of 25 arcsec x 38 arcsec
• spatial resolution element of 1.0 arcsec x 0.5 arcsec
• spectral resolution of R ~ 7000 (about 45 km/s FWHM).
ANU 2.3 WiFeS
Gemini 8.1 GMOS

14. Integral Field Spectroscopy
• Longslit Observation (PN Hb 4)
• IFU Observation (PN Hb 4)
Danehkar et al. (2014)

15. Integral Field Spectroscopy
• IFU Observation (PN M3-30)
• IFU Observation (PN IC 1297)
Danehkar et al. (2014)

16. Integral Field Spectroscopy
• Spatially-Resolved Kinematics (PN M3-30)
• Spatially-Resolved Chemistry (PN M3-30)
Danehkar et al. (2014)

17. Integral Field Spectroscopy
• Spatially-Resolved Kinematics (PN IC 1297)
• Spatially-Resolved Chemistry (PN IC 1297)
Danehkar et al. (2014)

18. Integral Field Spectroscopy
• Spatially-Resolved Kinematics (PN Th 2-A)
• Spatially-Resolved Chemistry (PN Th 2-A)
Danehkar et al. (2014); see Poster P2-24

19. Integral Field Spectroscopy
Danehkar et al. (2014), in preparation
• Kinematical Properties of Planetary Nebulae with WR-type Nuclei
• Kinematic modelling using SHAPE (Steffen & Lopez 2006; Steffen et al. 2011)

20. • Introduction to Planetary Nebulae
Introduction to Planetary Nebulae
• Introduction to WR-type stars
Introduction to WR-type stars
• Planetary Nebula Morphology
Planetary Nebula Morphology
• Integral Field Spectroscopy
Integral Field Spectroscopy
• Discussion
Discussion
• Summary
Summary

21. PN morphology: Problems?
Bipolar and Elliptical Morphology
• Generalized Interacting Stellar Winds (GISW) theory
– Kwok et al. (1978), Kahn & West (1985)
– Unable to predict complex axisymmetric shape
• Rotating Stellar Winds + Strong Magnetic Fields
– Garcıa-Segura 1997; Garcıa-Segura&Lopez 2000;
Frank&Blackman 2004
– single star may not supply enough angular momentum
for complex axisymmetric PNe (Soker 2006)
• Binary System, e.g. AGB star + white dwarf → common envelope
– Miszalski et al. 2009; De Marco 2009; Nordhaus et al. 2010
– nearly 30% of bipolar PNe contain post-CE binaries (Miszalski et al. 2009)
– alignments between the nebular shells and the binary orbital inclinations (e.g.
Mitchell et al. 2007; Jones et al. 2010, 2012; Tyndall et al. 2012; Huckvale et al.
2013).

22. PN morphology: Problems?
Binary system
• Direct Envelope Ejection
Outflow is predominately equatorial.
• Dynamo Driven Ejection
Outflow is aligned around the rotation
axis and is magnetically collimated.
• Disk Driven Ejection
Shred Secondary
Outflow is aligned with rotation axis
Nordhaus & Blackman 2006,MNRAS,370,2004

23. PN morphology: Problems?
Fast, low-ionization emission regions (FLIERs)
• Visible in [N II] 6584 and [S II] 6724 more than
in [O III] 5007 and Hα 6563 emission
• in opposite pairs on the both sides of
the central star
• moving with velocities much larger than
the main structure (40–200 km/s)
• How the density and velocity structures contrast
between the FLIERs and the main body?
– Possiblly axisymmetric mass-loss through a Common
Envelop and angular momentum deposition of the
binary system (Soker 1990; Soker& Harpaz (1992;
Nordhaus & Blackman 2006).
– Or combination of rotating stellar winds and strong
magnetic fields (Garcıa-Segura et al. 1999; Garcıa-
Segura & Lopez 2000)

24. WR Stellar Evolution: Problems?
• Radiation pressure is too small to remove H-rich outer layer
• There is a gap between [WCL] and [WCE]
• Born-again scenarios:
– AFTP. AGB Final Thermal Pulse occurs at the end of the AGB
– LTP. Late Thermal Pulse occurs when the star moves from the AGB phase
towards the white dwarf.
– VLTP. Very Late Thermal Pulse
occurs when the star is on the
white dwarf cooling track.
• Alternatively, mass-loss
to a binary companion
• or stellar merger

25. • Introduction to Planetary Nebulae
Introduction to Planetary Nebulae
• Introduction to WR-type stars
Introduction to WR-type stars
• Planetary Nebula Morphology
Planetary Nebula Morphology
• Integral Field Spectroscopy
Integral Field Spectroscopy
• Discussion
Discussion
• Summary
Summary

26. Summary
• PN asymmetric morphology: Elliptical (49%), Bipolar(20%)
– Generalized Interacting Stellar Winds (GISW)?
– Rotating Stellar Winds + Strong Magnetic Fields?
– Binary System?
• FLIERs: point-symmetric jets on the both sides
– Moving faster than the main shell expansion
– Low-ionization Structures, low densities
– Mostly in PNe with hot central stars
• H-deficient stellar atmospheres (25% of total)
– Born-again scenarios?
– Binary channel?
• Problems to solve
 Asymmetric morphology of PNe
 H-deficient atmospheres of CSPNe

27. Acknowledgements
Acknowledgements
• Travel Grant from the Astronomical Society of Australia.
Travel Grant from the Astronomical Society of Australia.
• IAU Travel Grant from the 12th Asia-Pacific Regional IAU
IAU Travel Grant from the 12th Asia-Pacific Regional IAU
Meeting.
Meeting.
Thank you for your attention!
Thank you for your attention!

28. Planetary Nebula (PN) morphology
HST imaging
• Round, Elliptical,
Bipolar/multipolar.