The Rotating Core-Collapse Supernova Dynamics and Neutrino - - PowerPoint PPT Presentation

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The Rotating Core-Collapse Supernova Dynamics and Neutrino - - PowerPoint PPT Presentation

Nov 06, 2022 307 likes •538 views

The Rotating Core-Collapse Supernova Dynamics and Neutrino Distributions by Full Boltzmann Neutrino Transport Akira Harada (University of Tokyo) Collaborators: W. Iwakami, H. OkawaS. Yamada (Waseda) H. Nagakura (Princeton), K. Sumiyoshi

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SLIDE 1

The Rotating Core-Collapse Supernova Dynamics and Neutrino Distributions by Full Boltzmann Neutrino Transport

Akira Harada (University of Tokyo) Collaborators: W. Iwakami, H. Okawa、S. Yamada (Waseda)

  • H. Nagakura (Princeton), K. Sumiyoshi (Numazu),
  • H. Matsuhuru (KEK)

High Energy Astrophysics 2018 2018/9/6@Hongo campus, University of Tokyo

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SLIDE 2
  • Gravitational Collapse→Core Bounce

→Stalled shock

  • Neutrino Heating Mechanism？

Core-Collapse Supernovae

Fe Si O,Ne,Mg C,O He H

PNS Shock ?

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SLIDE 3
  • Explosion failed in 1D ← confirmed by the Boltzmann

transport

  • The Boltzmann transport is also required for multi-D

simulations.

Boltzmann Neutrino Transport

Sumiyoshi+ (2005) Liebendoerfer+ (2001)

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SLIDE 4
  • Results of multi-D Boltzmann simulations
  • Collapse of the 11.2 M⦿ (Woosley+ 2002)

progenitor

  • Comparison of the equations of state is shown

Multi-D Boltzmann Simulation

LS - entropy 16 12 8 4

500 km

LS - |V| FS - entropy FS - |V| 3

x 109 (cm/s)

2 1

Nagakura+ (2018)

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SLIDE 5
  • Progenitor: 11.2 M⦿ (Woosley+ 2002)
  • EOS: Furusawa EOS (multi-nuclear species、

Relativistic Mean Field theory)

  • ν-reactions: Standard set of Bruenn (1985)

+GSI electron capture、Bremsstrahlung

  • Rotational velocity: Sheller rotation
  • Grid number:

Setup

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SLIDE 6

Entropy (rotating)

  • Evolution until ~ 200 ms after bounce
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SLIDE 7

Nagakura+ (2018)

Entropy (non-rotating)

  • Evolution until ~ 200 ms after bounce
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SLIDE 8

Time evolutions of shock radii

  • Evolution until ~ 200 ms after bounce
  • Comparison between rotating and non-rotating models.

50 100 150 200 250 300 350 400 0.05 0.1 0.15 0.2 shock radius rsh [km] time after bounce tpb [s] rotating non-rotating

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SLIDE 9

Trajectory of the PNS center

  • 1

1 2 0.05 0.1 0.15 0.2

  • ffset of PNS center dPNS [km]

time after bounce tpb [s] rotating non-rotating

  • Evolution until ~ 200 ms after bounce
  • Comparison between rotating and non-rotating models.
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SLIDE 10

Neutrino Distributions

  • Neutrino Distribution functions at ~ 10 ms after

bounce.

er eφ eθ er eφ eθ

~60 km ~170 km 1 MeV 4 MeV 19 MeV

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SLIDE 11

er eφ eθ

~170 km 1 MeV 4 MeV 19 MeV

Neutrino Distributions

  • Neutrino Distribution functions at ~ 10 ms after

bounce.

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SLIDE 12

Neutrino fluxes

  • φ-component of the neutrino flux at ~ 10 ms after bounce
  • The sign of the flux is different between in the fluid-rest-frame and in the

laboratory frame.

  • The Ray-by-Ray approximation can not capture this feature.

100 200 x [km] 100 200 1038 1039 1040 1041 1042 1043 1044 number flux in laboratory frame [cm−2s−1]

  • 4
  • 2

2 4 number flux in fluid rest frame [×1040 cm−2s−1]

Lab.

  • Fl. rest
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SLIDE 13

Eddington Tensor

  • Evaluating M1-closure method-Eddington tensor
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SLIDE 14

Eddington tensor

  • Eddington tensor at ~ 10 ms after bounce

rr-component Boltzmann M1-closure 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 rθ-component×10 Boltzmann M1-closure

  • 0.4
  • 0.3
  • 0.2
  • 0.1

0.1 0.2 0.3 0.4 rφ-component×10 Boltzmann M1-closure

  • 0.4
  • 0.3
  • 0.2
  • 0.1

0.1 0.2 0.3 0.4 rθ-component×10 Boltzmann M1-closure

  • 0.4
  • 0.3
  • 0.2
  • 0.1

0.1 0.2 0.3 0.4 θθ-component Boltzmann M1-closure 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 θφ-component×100 Boltzmann M1-closure

  • 0.6
  • 0.4
  • 0.2

0.2 0.4 0.6 rφ-component×10 Boltzmann M1-closure

  • 0.4
  • 0.3
  • 0.2
  • 0.1

0.1 0.2 0.3 0.4 θφ-component×100 Boltzmann M1-closure

  • 0.6
  • 0.4
  • 0.2

0.2 0.4 0.6 φφ-component Boltzmann M1-closure 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8

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SLIDE 15

Eddington tensor

  • Eddington tensor at ~ 10 ms after bounce
  • Tensors calculated by the distribution functions and the M1-closure

rφ-component×10 Boltzmann M1-closure

  • 0.4
  • 0.3
  • 0.2
  • 0.1

0.1 0.2 0.3 0.4 rr-component Boltzmann M1-closure 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8

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SLIDE 16

Eddington tensor

  • Eddington tensor at ~ 10 ms after bounce
  • Radial profiles of eigenvalues
  • ~20% errors in M1-closure method
  • 0.2

0.2 error 0.2 0.3 0.4 0.5 0.6 0.7 0.8 eigenvalue North-East Eddington factor lateral 1 lateral 2 rsh Boltzmann M1 50 50 100 150 radius r [km] 5

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SLIDE 17

Eddington tensor

  • 0.2

0.2 error 0.2 0.3 0.4 0.5 0.6 0.7 0.8 eigenvalue North-East Eddington factor lateral 1 lateral 2 rsh Boltzmann M1 50 50 100 150 radius r [km] 5

for M1

  • The Eddington factor does not necessarily

increase with the flux factor increasing.

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SLIDE 18

er eφ eθ

Near to the shock Far from the shock

Eddington tensor

  • The Eddington factor does not necessarily

increase with the flux factor increasing.

  • Comparison of distribution functions
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SLIDE 19

Eddington tensor

  • The flux factor
  • The Eddington factor
  • The distribution function at decreases

with getting closer to the shock→The flux factor increases and the Eddington factor decreases.

er eθ er eφ

Near to the shock Far from the shock

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SLIDE 20

Eddington factor

  • uter

inner

  • Prolateness of distribution
  • M1: prolateness is estimated from deviation of distribution

actual M1

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SLIDE 21
  • Collapse of rotating progenitor is simulated by

Boltzmann-Radiation-Hydro code.

  • Features which can not be reproduced by

approximate methods are discovered.

  • The accuracy of the M1-closure method is

evaluated.

Summary

er eφ eθ er eφ eθ

~60 km ~170 km