The Isotropic Di ff usion Source Approximation for Multi-D Supernova - - PowerPoint PPT Presentation

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Nov 23, 2022 47 likes •299 views

MICRA Workshop August 21st, 2015, Stockholm, Sweden The Isotropic Di ff usion Source Approximation for Multi-D Supernova Simulations also with FLASH Kuo-Chuan Pan Universitt Basel, Switzerland The Basel Supernova Group: Friedrich-Karl

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The Basel Supernova Group:

MICRA Workshop August 21st, 2015, Stockholm, Sweden 1

Kuo-Chuan Pan Universität Basel, Switzerland

CSCS

UNI BASEL

The Isotropic Diffusion Source Approximation for Multi-D Supernova Simulations

Matthias Liebendörfer Takami Kuroda Rubén Cabezón Kevin Ebinger Friedrich-Karl Thielemann Marius Eichler Matthias Hempel Oliver Heinimann Andreas Lohs

“also with FLASH”

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RIKEN 2015.08

Basic Physics

Direct hydrodynamics mechanism always fail!
Neutrino-driven convection is the key

˙ M

Adapted from Janka 01

PNS

Rν Rgain RNS Rshock

˙ M

¯ νe νe p p n n e− e+

Kuo-Chuan Pan 2 MICRA 2015

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Kuo-Chuan Pan 3 MICRA 2015

Isotropic Diffusion Source Approximation (IDSA)

Opaque Transparent Semi-transparent

νe PNS

Liebendorfer+ 09

IDSA (Liebendorfer+ 09)

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Kuo-Chuan Pan 4

Multi-D Simulations with IDSA

Multi-dimensional simulations with the IDSA have been studied

by the Nippon groups

ZEUS+IDSA in spherical coordinates with Ray-by-Ray approach

Suwa+ 13 Nakamura+ 14 Takiwaki+ 14

MICRA 2015

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Kuo-Chuan Pan 5 MICRA 2015

Multi-D IDSA with FLASH

Opaque Transparent Semi-transparent

νe PNS

Liebendorfer+ 09

Rν(E, l) f s(E, l)

Spherical Symmetry:

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Kuo-Chuan Pan 6

FLASH+IDSA

2D cylindrical and 3D Cartesian coordinates with AMR: better PNS but noisy
Not “Ray-by-Ray” approach. We solve the diffusion source and trapped

particle component in multi-dimensions, but keep the streaming component in spherical symmetry (Similar to the Elephant code)

20 energy bins from 3 MeV to 300 MeV
Only for electron type neutrinos (Heavy neutrinos -> Leakage scheme)

Ott+ 12

Ray-by-Ray

This work

Full 3D

MICRA 2015

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Kuo-Chuan Pan 7

The FLASH code (v4.2.2)

Code Status:

Geometry: 1D spherical, 2D cylindrical, and 3D Cartesian (Similar to Couch+13)
Hydrodynamics: 3rd PPM with HLLC Riemann solver with AMR
Resolution: effective angular resolution (2D:~0.3-0.60 ,3D:~1-20 )
Simulation box: r= 0 to r= 10,000 km
Gravity: The new improved multi-pole solver (Couch+13; Newtonian or eff. GR)
EoS: Supernova EoS from http://stellarcollapse.org
Neutrino transport: Isotropic Diffusion Source Approximation (IDSA)
Collapse: IDSA or parametrized deleptonization (PD; Liebendorfer+05)
Postbounce: IDSA (Liebendorfer+09)

MICRA 2015

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Kuo-Chuan Pan 8

1D Code Comparison: FLASH v.s. AGILE

MICRA 2015

Shock Radius Neutrino Spectra

W2002 Progenitors + LS220 s15.0

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Shock Radius Neutrino Luminosity

Kuo-Chuan Pan 9

1D Code Comparison: Eff. GR

MICRA 2015

O’Connor+ 15

Preliminary

s15s7b2 (W1995) + LS180

Preliminary

Marek+06 Shock Radius Neutrino Luminosity

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Kuo-Chuan Pan 10

The Bruenn rates (1985) in IDSA

s15 (W2007) + LS220

Preliminary

Lentz+ 12 Lentz+ 12 Shock Radius Neutrino Luminosity

MICRA 2015

Shock Radius

Preliminary Neutrino Luminosity Neutrino Luminosity

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Kuo-Chuan Pan 11

2D Code Comparison

MICRA 2015

Suwa +14 Hanke 14

The 2007 (WHW) Progenitors

Bruenn +13 Dolence+15

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Kuo-Chuan Pan 12

2D Code Comparison

MICRA 2015

Suwa +14 Hanke 14

The 2007 (WHW) Progenitors

Bruenn +13 Dolence+15

Preliminary

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Kuo-Chuan Pan 13

2D Code Comparison

MICRA 2015

Hanke 14 Dolence+15

NR+ShenEoS GR+LS220

FLASH+IDSA Melson+15

s20 s20 s15

NR+LS220

Preliminary Preliminary

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Kuo-Chuan Pan 14

2D: W2002 Progenitors

FLASH+IDSA+DD2

MICRA 2015

DD2 vs. LS220 The HS(DD2) EoS The new SN EoS HS (DD2) shows a better agreement with nuclear experiments (Kruger+13; Fischer+14; Hempel+15) Pan+15

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Kuo-Chuan Pan 15

2D Results: SASI

MICRA 2015

SASI Amplitude Pole Entropy

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Kuo-Chuan Pan 16

2D Results: Convection-Driven

MICRA 2015

Anisotropic Velocity Brunt-Vaisala Frequenciy

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Kuo-Chuan Pan 17

2D vs. 3D

s11.2 (W02)

Takiwaki+14

u9.6 (W15)

Melson+15 Muller+13 Lentz+15

s15.0 (W07)

MICRA 2015

s20.0 (W07)

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Kuo-Chuan Pan 18

3D FLASH-IDSA results

s15.0 IDSA

3D IDSA+PD
15Msun (WHW+02)
HS (DD2) EoS
Newtonian
Resolution: 1.80
Only 0.5M cpu-hours

Pan+ in prep.

MICRA 2015

s15.0 w PD

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Kuo-Chuan Pan 19

3D simulations with the 15.0 progenitor

Lentz+15

s15.0 (W07)

Pan+ in prep.

s15.0 (W02) DD2 LS220

Note that the physics employed and the progenitors used are different

MICRA 2015

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Kuo-Chuan Pan 20

2D vs. 3D (conti.)

MICRA 2015

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Kuo-Chuan Pan 21

Neutrino Heating in 3D

2D 3D 150 ms 250 ms 300 ms

MICRA 2015

500 km

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Kuo-Chuan Pan 22

Conclusions

MICRA 2015

Our IDSA implementation seems robust (or too optimistic; all 2D and

3D models exploded) with diagnostic explosion energies ~0.1-0.5 B (at ~400ms)

Neutrino interactions (e.g. NES) during collapse are important in Multi-D
Neutrino-driven convection with little SASI (W2002 Progenitors)
DD2 is slightly easier to explode than LS220
3D seems harder to explode than 2D
IDSA is promising to achieve high-resolution 3D simulations (good for

progenitor studies, long-term evolutions and nuclear synthesis)

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Kuo-Chuan Pan 23

EoS Dependence

MICRA 2015

2D 1D

~50ms ~600km

9 EoS from StellarCollapse with the s15.0 (W2002) progenitor

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Kuo-Chuan Pan 24

3D Code comparison

MICRA 2015

Elephant

3D IDSA Cartesian mesh NR/ eff. GR

SPHYNX

ASL/IDSA SPH 3D Newtonian

FLASH

1-3D IDSA AMR NR/eff. GR

fGR_M1

M1 Nested meshes 3D full GR

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Kuo-Chuan Pan 25

2D vs. 3D

Time = 200 ms Time = 300 ms Time = 400 ms Time = 400 ms

Lentz+15

MICRA 2015