(Pulsational) Pair Instability SN Mathieu Renzo Collaborators: S. E. - - PowerPoint PPT Presentation

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(Pulsational) Pair Instability SN Mathieu Renzo Collaborators: S. E. - - PowerPoint PPT Presentation

Oct 07, 2022 157 likes •303 views

Anton Pannekoek Institute (Pulsational) Pair Instability SN Mathieu Renzo Collaborators: S. E. de Mink, Y. G otberg, E. Zapartas, Bin R. Farmer, P . Marchant, B. Paxton C osmos 1 / 7 Anton Pannekoek Institute Late mass loss BBH-merger

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SLIDE 1

Anton Pannekoek Institute

(Pulsational) Pair Instability SN

1 / 7

Bin

C

  • smos

Mathieu Renzo

Collaborators: S. E. de Mink, Y. G¨

  • tberg, E. Zapartas,
  • R. Farmer, P

. Marchant, B. Paxton

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SLIDE 2

Anton Pannekoek Institute

Late mass loss

BBH-merger EM counterpart ⇒ mass loss needs to be close to 2nd core-collapse

  • Flash spectroscopy of SNe

–

e.g., Khazov et al. 2016

  • narrow-lined SNe (Ibn & IIn)

–

e.g., Filippenko 1997, Smith 2016

  • CSM-powered SLSNe

–

e.g., Chevalier & Fransson 1994, Smith 2007

  • SN-impostors

–

e.g., Smith et al. 2008

  • ...

2 / 7

Observational evidence

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SLIDE 3

Anton Pannekoek Institute

Late mass loss

BBH-merger EM counterpart ⇒ mass loss needs to be close to 2nd core-collapse

  • Flash spectroscopy of SNe

–

e.g., Khazov et al. 2016

  • narrow-lined SNe (Ibn & IIn)

–

e.g., Filippenko 1997, Smith 2016

  • CSM-powered SLSNe

–

e.g., Chevalier & Fransson 1994, Smith 2007

  • SN-impostors

–

e.g., Smith et al. 2008

  • ...
  • Wave driven mass loss

–

e.g., Shiode & Quataert 2014, Fuller et al. 2017

  • Pulsational pair instability +

Core collapse

–

e.g., Barkat et al. 1967, Chatzopoulos & Wheeler 2012, Woosley 2017

  • ...

2 / 7

Observational evidence Theoretical ideas

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SLIDE 4

Anton Pannekoek Institute

Different behaviors with MZAMS and/or MHe

3 / 7

  • cf. Woosley 2017

IMF(M) ∝ M−2.3 MHe governs the fate, determines MBH

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SLIDE 5

Evolution during (P)PISN

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SLIDE 6

Radiation dominated: Ptot ≃ Prad MHe 32 M⊙

(Woosley 2017)

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SLIDE 7

Γ1 < 4/3 103 104 105 106 ρ [g cm−3] 108 109 T [K] Eγ < Ee±

Fermi

Eγ < 2mec2 non rel. e± pressure support MHe = 46 M⊙, Z = 0.001 Preliminary calculations with

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SLIDE 8
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SLIDE 9
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SLIDE 10
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SLIDE 11
  • 1. Pair production

γγ → e+e−

  • 2. Softening of EOS

triggers collapse Γ1 < 4

3

  • 3. Explosive

(oxygen) ignition

  • 7. BH
  • 5. ν-cooling

and contraction

  • 6. Entropy loss

and fuel depletion stabilize the core

  • 4a. Pulse with mass ejection
  • 4b. PISN: complete disruption
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SLIDE 12

Anton Pannekoek Institute

PPISN mass loss history

Example: MHe = 46 M⊙, Z = 0.001, no envelope

P R E L I M I N A R Y

0.0 0.1 0.2 0.3 0.4 0.5 0.6 time to CC [107 s] 32.55 32.60 32.65 32.70 32.75 32.80 32.85 32.90 Mass [M⊙] past wind mass loss Mtot Tc 9.00 9.25 9.50 9.75 10.00 10.25 log10(Tc/[K])

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SLIDE 13

Anton Pannekoek Institute

Discussion

Timed shortly before BH formation Sufficient amount of mass; Can increase eccentricity ⇒ decrease τGW; ... ✗ Can possibly unbind the binary; ✗ vejecta 103 − 104 km s−1; ✗ Still have to survive τGW. ✗ ...

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Can PPISN provide the mass aroung the BBH? Pros Cons

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SLIDE 14

Anton Pannekoek Institute

Discussion

Timed shortly before BH formation Sufficient amount of mass; Can increase eccentricity ⇒ decrease τGW; ... ✗ Can possibly unbind the binary; ✗ vejecta 103 − 104 km s−1; ✗ Still have to survive τGW. ✗ ...

7 / 7

Can PPISN provide the mass aroung the BBH? Pros Cons Bonus:

  • Naturally produces BHs of ∼ 30 M⊙
  • Can modify the BH mass function (2nd mass gap)

Correlation between MBH and EM signal?