1. Slide 1 CE through PN eyes June 29 th, 2005 Common Envelope Evolution through Planetary Nebula Eyes Orsola De Marco American Museum of Natural History Merging binaries. Simulations UKAFF Collaborators: H.E. Bond, M. Moe, M.-M. Mac Low, E. Sandquist, F. Herwig, R. Taam

2. Slide 2 CE through PN eyes June 29 th, 2005 The common envelope (CE) interaction and its progeny populations. The CSPN RV survey: can PN be by and large a CE phenomenon? CE simulations: the determination of the CE efficiency parameter (  and other parameters. post-CE populations (sdB and CSPN) to constrain CE simulations. Further/future simulations: common envelope mergers. Outline

3. Slide 3 CE through PN eyes June 29 th, 2005 RGB: R ~100-300 R o AGB: R ~ 500-1500 R o Common Envelope: A twice-in-a-lifetime opportunity R R

4. Slide 4 CE through PN eyes June 29 th, 2005 Common envelopeUnstable Roche Lobe overflow

5. Slide 5 CE through PN eyes June 29 th, 2005 A short-period binary, or… a merged star Depending on the efficiency of the energy transfer from the companion to the CE (  ), one might get:

6. Slide 6 CE through PN eyes June 29 th, 2005 The existence of a CE phase is inferred by the presence of evolved close binaries: CVs, Type Ia SN, LMXB, post-RGB sdB binaries, and... Binary CSPN, with P < 3-5 yr If you are interested in the CE interaction: Can we use the post-CE CSPN to constrain our understanding of the CE interaction? If you are interested in the PN for themselves: How many post-CE PN? How are they different from single or merged CSPN?

7. Slide 7 CE through PN eyes June 29 th, 2005 Summer 2004 observations added 16 data points to IC4593 resulting in a likely period of 5.1 day! (Other periods not yet determined) PN RV survey:10/11 RV variables ( De Marco et al. 2004 & H. Bond’s talk ): Most CSPN in close binaries !?

8. Slide 8 CE through PN eyes June 29 th, 2005 # of stars in the Galaxy: 2.1 x 10 11 ( Total mass: Kulessa & Lynden-Bell 1992; IMF: Kroupa et al. 1993 ) Primaries w/ lifetime shorter than age of Galaxy: 7.6% ( based on 9 Gyr: del Peloso et al. 2005 corresponding to M > 1.03 M o : Schaller et al. 1992; Bressan et al. 1993 ) Percentage of stars w/ companion: 60% ( Duquennoy & Mayor 1; ie # of binary systems=0.375x2.1x10 11 ) Binaries w/ 100 R o < a < 500 R o : 12% ( I.e. that enter CE on the AGB; Duquennoy & Mayor ) M 1 /M 2 > 0.2: 73% ( Duquennoy & Mayor 1991; I.e. secondary ejects the envelope even for low  ) Mean age of primaries: 1.15 Gyr ( Schaller et al. 1992; Bressan et al. 1993; for mean mass of 2.03M o from Kroupa IMF with limits 1.03M o and 10M o ) PN visibility time ~ 20,000 yr ( ESO catalogue ) # of post-CE binary CSPN ~ 9100 (OK within a factor of ~5) # of PN in the Galaxy (actual): ~3000 ( ESO catalogue + Parker & Phillips 1998 ) # of PN in the Galaxy (estimated): 7200 +/- 1800 ( Peimbert 1990 ) Despite uncertainty, 9100 post-CE binaries, is commensurate with the # galactic PN, lending circumstantial support to the RV survey. Could our finding be right and most/all PN derive from a CE? Rephrasing the question: Could most/all galactic PN derive from main sequence binaries that enter and survive an AGB CE?

9. Slide 9 CE through PN eyes June 29 th, 2005 Some population syntheses (e.g., Han et al. 1995) predict only ~20% of all PN in close-binaries. Is this inconsistent with our earlier accounting? Population syntheses count the fraction of all binary stars that enter and survive a CE. They do not count the absolute numbers. When plugging the star numbers into those simulations the 20% will result in absolute number of PN close to our estimate. In passing: if all stars that ascend the AGB make a PN, too many PN are predicted in the Galaxy (in the tens of thousands).

10. Slide 10 CE through PN eyes June 29 th, 2005 If the majority of CSPN are post-CE binaries: Where are the single (or merged) post-AGB stars? The total # of PN in the galaxy might be <10,000 rather than the often-quoted 20,000 (~3000 known). Single stars in the post-AGB-to-pre-WD phase might have an invisible PN (see Subag & Soker (submitted)). Can we quantify the population of “naked” post-AGB stars via their integrated UV flux in external galaxies?

11. Slide 11 CE through PN eyes June 29 th, 2005 The CE phase plays a fundamental role in CVs, Type Ia SN, LMXB, post-RGB sdB stars in close binaries, and close-binary CSPN. Despite past work, out theoretical understanding of the CE interaction is still rudimentary. In particular: what is  ? We know it is not constant, but a function of stellar and system parameters. Without knowing , population synthesis models cannot predict/explain period distributions and other characteristics of, e.g., CVs, Type Ia SN progenitors. Past work in common envelope theory: Ostriker 1975, Paczynski 1976 (proposal) eg, Rasio & Livio 1996 (analytical) eg, Taam & Sandquist 2000 (numerical) Past work in common envelope observations: e.g. Hillwig et al. 2002, Drake & Sarna 2003 Sarna et al. 1995, Bleach et al. 2000

12. Slide 12 CE through PN eyes June 29 th, 2005 Companion's orbit AGB star 6 AU Code: Burkert & Bodenheimer 1993 Method: Sandquist et al. 1998 The determination of  De Marco et al. 2003 & in prep. 3D nested grid hydro code. Self gravity only (no B fields). Primary calculated via 1D code (Herwig), and mapped into the cartesian grid. Companion and AGB star core are point masses, separation ~3 AU, P~3 yr Max resolution in inner grid 1.75x10 11 cm; cf. primary radius = 10 13 cm, core radius ~ 10 8 cm, companion radius <~10 10 cm

13. Slide 13 CE through PN eyes June 29 th, 2005 4 common envelope tests 1 Main Sequence Mass = 1.5 M o Bottom of the AGB Top of the AGB - Thermal Pulse Bottom of the AGB Top of the AGB - Thermal Pulse 10

14. Slide 14 CE through PN eyes June 29 th, 2005 A short-period binary, or… a merged star Reminder: depending on the efficiency of the CE, the outcome can be: The efficiency is measured by:  =  E Bin /  E g Hence:  ~ 1 is more likely to result in a close binary.  << 1 is more likely to result in a merger.

15. Slide 15 CE through PN eyes June 29 th, 2005 Results: the outcome is a very sensitive function of initial parameters, including the evolutionary state of the primary.  highly variable, while population studies assume it is constant!

16. Slide 16 CE through PN eyes June 29 th, 2005 The period distribution of post-CE populations, is a sensitive function of . Period distribution of WD+MS post-CE systems from the theoretical population synthesis models of Han et al. 1995 (Fig 4) Less efficient:  0 More efficient:  1

17. Slide 17 CE through PN eyes June 29 th, 2005 Theoretical period distributions using the new  values can be compared to the period distributions of post-CE populations such as: 3 d < P < 100 d % Period 10 Bond 2000 P < 3 d Post-RGB: sdB stars binaries Maxted et al. 2001 Morales-Rueda et al. 2003 or post-AGB: CSPN De Marco et al. (2004) and work in progress. ? This calibration makes population simulations more reliable to understand the action of magnetic breaking or gravitational wave radiation in “tightening” binaries leading to the onset of phenomena like CV behaviour or type Ia SN.

18. Slide 18 CE through PN eyes June 29 th, 2005 CE outcome is a sensitive function of the exact evolutionary status of the primary. Bottom-AGB Top-AGB: TP10 Orbital planePerpendicular plane … with 68% of the envelope lost in ~10 yr and a resulting binary. The mass lost (unbound mass on the grid) has a bipolar configuration (PN morphology?) A 0.1-M o companion has little effect on a bottom-of-the-AGB star, but is devastating for a top-of-the-AGB one …

19. Slide 19 CE through PN eyes June 29 th, 2005 1) What happens to the companion in the final phase of the spiral-in? useful in: (i) can low mass companions eject the envelope? (formation of CVs with BD companions [Politano 2004]) (ii) can a planet change into a more massive object by accreting (e.g., Siess & Livio 1999)? 2) What happens when companions merge with the primary’s core? useful in: (i) Blue stragglers (Saffer et al. 2000) (ii) R Coronae Borealis stars (Clayton 1996) (iii) Wolf-Rayet central stars (De Marco & Soker 2002) (iv) SN Type Ia (Langer et al. 2000) (v) Other types of SN??? (suggestion by E.F. Brown) We will also address (code FLASH [Fryxell et al. 2000]):

20. Slide 20 CE through PN eyes June 29 th, 2005 CSPN might be predominantly in close period binaries. If so, the # of PN in the Galaxy might be better explained, than if single stars readily make PN. CE calculations assist population syntheses that predict the characteristics of binary classes (CV, SN Type Ia). Binary CSPN population used to constrain models. New generation of simulations is underway, to understand accreting secondaries and mergers. Summary

21. Slide 21 CE through PN eyes June 29 th, 2005 Thank you! Please send questions to: orsola@amnh.org