1. When stars collide: of planetary nebulae, jets and cosmic outbursts
Orsola De Marco
Macquarie University
Add photos of the people I am reviewing?
Collaborators: Jan Staff (Florida State)
Jean-Claude Passy (Bonn U)
Roberto Iaconi (Macquarie U)
Todd Hillwig (Valparaiso U)
Falk Herwig (U Victoria)
Thomas Reichardt (Macquarie U)

2. Stellar evolution for 1-8Mo stars
CRL 2688
Post-AGB star + pre PN
NGC 6543
pre WD star + ionised PN
~0.15 pc
AFGL 3068
Post AGB phase
~0.15 pc
AGB phase
~0.15 pc
WD cooling track

3. <~20% spherical
~20% bipolar
~60% ellipticals
Parker et al. 2006

4. We thought we had the solution to the formation of non-spherical PN …

6. Only <20% of the PN progenitor stellar population has companions that will interact on the AGB. But 80% of nebulae are non-spherical!

7. 20% of 1-8Mo stars can have a binary interaction on the AGB
… expect 20% of PN to be
non-spherical
If some single and non-interacting binary stars do not make a PN…
… the fraction of non-spherical PN can increase
Moe and De Marco, 2006, 2012

8. What can we say from observations
15-20% of all central stars of PN are short-period binaries
(Bond 2000; Miszalski et al. 2009)
There are likely more …
Artist: Dana Berry

9. The Kepler sample: 5 PN Merger No variability Likely binary Binary
De Marco et al. 2015
NGC 6826 (V ~ 11)
Bruce Balick
Abell 61 (V ~ 17)
Jim Shuder
Merger
No variability
Likely binary
Binary
Binary
Pa 5 (V ~ 16)
Kn 61 (V ~ 18)
Travis Rector
J (V ~ 14)
Aller et al 2013

10. What can we say from observations
15-20% of all central stars of PN are short-period binaries
(Bond 2000; Miszalski et al. 2009)
There are likely more … These are post-common envelope binaries De Marco et al. 2008, Hillwig et al. 2010,2014
Current scenarios predict only 5%
(Madappatt, De Marco, Villaver 2016)
Artist: Dana Berry

11. Shaping PN with common envelope interactions
Common envelope interactions promote equatorially-enhanced mass loss, magnetic fields and jets
Passy et al. 2012

12. Shaping PN with common envelope interactions
Jet masses and kinematics in post-common envelope PN allow us to determine the strength of the magnetic fields in common envelope interactions (Tocknell, De Marco & Wardle 2014)

13. A jet shaping model for OH231.8+4.2
Nebula around a 3.05Mo Mira (AGB star)
Well measured lobes momenta, energies and power
Kinematics give a lobe age of 800 years
Any other values of the momentum?

14. A jet shaping model
3D hydrodynamic model with an eccentric binary interaction + Roche lobe overflow, disk formation and common envelope merger
Characterization of disk mass and survival time scales
Analytical determination of jet
Speeds and momenta/energies/ power
Staff et al. 2016a
Any other values of the momentum?

15. Further implications of jet models
e Carinae: luminous blue variable, massive binary 150Mo + 30 Mo, 5.5 year period, 0.9 eccentricity

16. Connecting outflows and outbursts
NGC6826 (PN):
Common envelope merger outburst ~10,000 years ago, resolved outflow
V838 Mon:
Common envelope merger of a ~6Mo sub-giant star with companion, outburst 2002, no outflow yet
V1309Sco:
Common envelope merger of a 1.5Mo and 0.15Mo, outburst 2010, no resolved outflow yet

17. LSST will find many mergers and binary-induced outbursts

18. Prediction of BH merger rates
rest on shaky common envelope
Physics