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The Trouble with Triples: Difficulties with the triple scenario and - PowerPoint PPT Presentation

Feb 16, 2024 •97 likes •279 views

The Trouble with Triples: Difficulties with the triple scenario and how they might be overcome Joseph OBrien Antognini August 5, 2015 The trouble with triples... ? Kozai Thompson (2011) Katz & Dong (2012) Kushnir et al. (2013) The

  1. The Trouble with Triples: Difficulties with the triple scenario and how they might be overcome Joseph O’Brien Antognini August 5, 2015

  2. The trouble with triples... ? Kozai Thompson (2011) Katz & Dong (2012) Kushnir et al. (2013)

  3. The trouble with triples... Kozai + Stellar tidal friction Kozai evolution oscillations e.g., Mazeh & quenched Shaham ‘79, Wu & Murray ‘03, Fabrycky & Tremaine ‘07

  4. Population synthesis of triples confirms our concerns... Hamers+ 2013 Hamers+ 2013

  5. Avoiding the trouble with triples ? Scattering? Asymmetric mass loss?

  6. WD kick uncertainties ● How does an adiabatic force change the orbital inclination? ● Are the kicks actually adiabatic? ● Are the kicks in one direction, or is there a random walk? ● What, me worry?

  7. How much do WD kicks have to change the inclination? R ☉ R WD

  8. How much do WD kicks have to change the inclination? MIEK R ☉ (Shappee & Thompson 2013)

  9. Scattering with Fewbody (Fregeau et al. 2004) ● Performed ~ 400 million N-body calculations (Antognini & Thompson, 2015) ● KS regularization (Kustaanheimo & Steifel 1965) ● Energy conservation tolerance of 10 -3 (Portegies Zwart & Boekholt 2014; Boekholt & Portegies Zwart 2014) ● Check for convergence in max impact parameter

  10. Dynamically formed triples are... extremely compact ~ uniform in inclination (Antognini+ 2015) (Antognini+ 2015)

  11. Scattering processes are strongly velocity dependent (Antognini+ 2015)

  12. Rate estimate pretty well ??? ? known now ?

  13. Assumptions about N in the field ● 10 10 white dwarfs in the Galaxy (Napiwotzki 2009) ● 10% of WDs are in WD-WD binaries (Holberg 2009) ● 20% of WD-WD binaries have tertiaries ⇒ 2 x 10 8 WD-WD binaries with tertiaries

  14. Rate estimate in the field Hopeless. Even more Ellipticals?? hopeless.

  15. Assumptions about N in open clusters ● 10 5 open clusters in the Galaxy (Piskunov et al. 2006) ● The typical system is in an open cluster with 300 members (Porras et al. 2003) ⇒ 3 x 10 6 triples in open clusters

  16. Rate estimate for open clusters Within a factor of ~ 10 Too high? Too low?

  17. Summary ● Still unclear how to avoid coalescence on the main sequence ● Scattering does not work in the field. Open clusters are complicated. WD kicks need to change the inclination by >15° ● A survey for the community: By show of hands, what fraction of SNe Ia happen in triples? None of them <<10% ~ 10% All of them

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