Neutrinos in Core Collapse Supernovae Evan OConnor, Stockholm - - PowerPoint PPT Presentation

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Neutrinos in Core Collapse Supernovae Evan OConnor, Stockholm University Outline: SN theory & status Neutrino Signal Supernovae have a broad connection to the Universe Neutrinos & Gravitational Waves Nucleosynthesis Stellar

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Neutrinos in Core Collapse Supernovae

Evan O’Connor, Stockholm University

Outline:

  • SN theory & status
  • Neutrino Signal
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Cosmology High-Z & SCP

Evan O’Connor – TAUP 2019 2 of 24

Supernovae have a broad connection to the Universe

Stellar Evolution ESO Long gamma-ray burst Science/MacFadyen LIGO/VIRGO Neutron Star & Black Holes Hubble Galaxy Evolution Neutrinos & Gravitational Waves Nucleosynthesis Wikimedia/Jennifer Johnson Extreme Nuclear Physics

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Evan O’Connor – TAUP 2019 3 of 24

Supernova Types

Volumetric Supernova Survey: Li et al. (2010)

Core Collapse Thermonuclear

HST HST

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Evan O’Connor – TAUP 2019 4 of 24

Collapse Phase

  • Most massive stars core collapse during the

red supergiant phase

  • CCSNe are triggered by the collapse of the iron

core (~1000km, or 1/106 of the star’s radius)

  • Collapse ensues because electron degeneracy

pressure can no longer support the core against gravity

1000 Rsun

Iron Core 1000 km M ~ 1.4Msun

Protoneutron Star ~30km HST

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Evan O’Connor – TAUP 2019 5 of 24

Iron core collapse

sonic point

t = -5ms

r~1012 g cm-3

|---200 km---|

bounce

shock n n n n

r~1014 g cm-3

n

t = 0ms

|---20 km---|

CCSNe: The Stages

shock stagnation

stalled shock

n n n

|---200 km---|

t = ~100ms

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Evan O’Connor – TAUP 2019 6 of 24

Iron core collapse

sonic point

t = -5ms

r~1012 g cm-3

|---200 km---|

bounce

shock n n n n

r~1014 g cm-3

n

t = 0ms

|---20 km---|

shock stagnation

stalled shock

n n n

|---200 km---|

t = ~100ms

CCSNe: The Stages

t > ~200ms

n ne e- p n

|---150 km---|

n

Explosion

Require some mechanism to drive explosion

  • The prevailing mechanism is the

turbulence-aided neutrino mechanism

  • Neutrinos from core heat outer layers
  • Drives convection
  • Turbulence pressure support aids heating

and drives explosion

  • Very successful in 2D*, many

successful explosions

  • Success in 3D too: fewer simulations
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Evan O’Connor – TAUP 2019 7 of 24

The Core-Collapse Supernova Problem

Understanding the transition from an imploding iron core to an exploding star has been a persistent and difficult problem in astrophysics.

EO & Couch (2018b)

General Relativity Neutrino Transport & Interactions Nuclear Reactions 3D - (Magneto)hydrodynamics Nuclear Equation

  • f State

Progenitors

Requires:

Computational Physics

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Evan O’Connor – TAUP 2019 8 of 24

Burrows et al. (2019)

Explosion Successes in multiD – 3D

  • Similar progenitors
  • GR gravity
  • Non-rotating
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Evan O’Connor – TAUP 2019 9 of 24

Burrows et al. (2019) Lentz et al. (2015)

Explosion Successes in multiD – 3D

  • Similar progenitors
  • GR gravity
  • Non-rotating
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Evan O’Connor – TAUP 2019 10 of 24

Burrows et al. (2019) Lentz et al. (2015) Melson et al. (2015b)

Explosion Successes in multiD – 3D

  • Similar progenitors
  • GR gravity
  • Non-rotating
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Evan O’Connor – TAUP 2019 11 of 24

Burrows et al. (2019) Lentz et al. (2015) Melson et al. (2015b) Ott et al. (2018)

Explosion Successes in multiD – 3D

  • Similar progenitors
  • GR gravity
  • Non-rotating
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Evan O’Connor – TAUP 2019 12 of 24

  • When the matter reaches nuclear

density and the supernova shock forms, it liberates the nucleons from the nuclei

  • Recently freed and no longer

suppressed, protons now rapidly capture electrons, producing a burst of ne

e- n p ne

Neutronization Burst

from 3ms before bounce to 6 ms after (animation)

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Evan O’Connor – TAUP 2019 13 of 24

  • 2

2 4 6 8 10 12 14 16 18 20

t - tbounce [ms]

1 2 3 4 5 6

Luminosity [1053 erg/s] Iron core mass increasing -> Matter temperature increasing ->

ne nx

ne

_

  • ne’s take a bit of time (few ms)

before the density at the shock is low enough for the n’s to escape

  • anti-ne and nx neutrinos luminosity is
  • low. anti-ne are suppressed because

high electron degeneracy, nx because T is low

  • Little progenitor dependence,

universal* nature of collapse

Neutronization Burst

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Evan O’Connor – TAUP 2019 14 of 24

t – tbounce [s]

x3-4

Accretion Phase

Warren et al. (in prep) Compactness

Luminosity (1051 erg/s)

Couch et al. (2019) & 200 1D models from

Learn about progenitor structure from neutrino observation of galactic supernova

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Evan O’Connor – TAUP 2019 15 of 24

Accretion Phase

Warren et al. (in prep) Couch et al. (2019) & 200 1D models from

Learn about neutron star mass from neutrino

  • bservation of galactic supernova

t – tbounce [s]

Compactness

Luminosity (1051 erg/s)

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Evan O’Connor – TAUP 2019 16 of 24

Global effort towards agreement

  • Want to demonstrate the community’s ability to simulate SN
  • Comparison of 6 core-collapse supernova codes
  • Very carefully control input physics and initial conditions to

ensure fair comparison

Journal of Physics: G 45 10 2018

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Evan O’Connor – TAUP 2019 17 of 24

Excellent Agreement in 1D

EO+ 2018 Si/O interface Si/O interface

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Evan O’Connor – TAUP 2019 18 of 24

Systematic Effects

Malmenbeck, O’Sullivan (2019) PoS- ICRC2019-975; arXiv:1909.00886 Implementation of detailed IceCube detector into SNOwGLoBES

  • Energy-dependent effective volume,

detector efficiency, deadtime, … *Normal Hierarchy: only adiabatic MSW

Sensitive dependence on energy spectrum shows areas where improvements are needed

https://github.com/SNOwGLoBES/

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Evan O’Connor – TAUP 2019 19 of 24

  • Standing Accretion Shock Instability (SASI) can impact
  • signal. Observable in Hyper-K or IceCube at 10kpc

Accretion Phase - SASI

Hyper-K design report (arXiv:1805.04163)

Neutrinos can reveal important dynamics of the supernova engine

EO & Couch (2018b)

data: Tamborra et al. (2013)

see also TAUP talk by T. Takiwaki

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Evan O’Connor – TAUP 2019 20 of 24

Rotation in Core-Collapse Supernovae

  • Rotation impacts neutrinos

and excites the newly formed protoneutron star

  • Correlated signal in GWs

and neutrinos

  • Use SNOwGLoBES + IceCube

to generate rates and realizations

Westernacher-Schneider, O’Connor, O’Sullivan+ (arXiv:1907.01138) see also TAUP talk by T. Takiwaki

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Evan O’Connor – TAUP 2019 21 of 24

Rotation in Core-Collapse Supernovae

  • Rotation impacts neutrinos

and excites the newly formed protoneutron star

  • Correlated signal in GWs

and neutrinos

  • Use SNOwGLoBES + IceCube

to generate rates and realizations

Westernacher-Schneider, O’Connor, O’Sullivan+ (arXiv:1907.01138) see also TAUP talk by T. Takiwaki

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Evan O’Connor – TAUP 2019 22 of 24

Rotation-induced Oscillations in neutrinos

  • Must be close to see such small
  • signal. In IceCube: ~1kpc

*Realizations take into account statistical noise and detector background noise Westernacher-Schneider, O’Connor, O’Sullivan+ (arXiv:1907.01138)

Neutrinos can reveal important dynamics of the supernova engine

(animation) (animation) (animation)

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Evan O’Connor – TAUP 2019 23 of 24

Transition from Accretion to Cooling Phase

Vartanyan et al. (2019)

  • 3D explosions by the Princeton group

(but also others) shows simultaneous accretion & ejection Luminosity 1052 erg/s

post bounce time [s]

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Evan O’Connor – TAUP 2019 24 of 24

Cooling Phase

  • How the protoneutron star cools relays

info about the EOS

  • Also the neutron star mass (see TAUP

talkby Y. Suwa)

  • <E> differences between ne and anti-ne is

important and can impact nucleosynthesis

Horowitz et al. (2016) Super-K like

x=

*Here x characterizes additional opacity due to nuclear pasta formation

x=5 x=5 x= x=

Neutrinos from the cooling phase shed light on key properties of PNS

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Evan O’Connor – TAUP 2019 25 of 24

Not all core collapses will succeed

LIGO

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Evan O’Connor – TAUP 2019 26 of 24

Black Hole Formation

with SNOwGLoBES 10kpc

Ln ~ 400 B/s!

O’Connor (2015)

MSW only

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Evan O’Connor – TAUP 2019 27 of 24

Summary

  • Core Collapse simulations in multiD explode via the turbulence-aided

neutrino mechanism, across codes and progenitors

  • Models predict several interesting neutrino-signal-related phenomena
  • Caveats: Models, Neutrino Oscillations, reversing detected signal, …
  • Neutronization Burst (Universal)
  • Neutrino mass ordering likely discernible from signal
  • Accretion Luminosity (probes progenitor/PNS mass)
  • SASI predicts large time variations in signal
  • Rotation predicts correlated neutrino and GW signals
  • Equation of State and PNS mass sets cooling curve over ~5-100s
  • Failed supernovae predict sharp cutoff on neutrinos
  • Many more….

TAUP talks by: A. Harada, K. Nakazato, S. Abbar, N. Yamamoto,

  • M. Mori, Y. Suwa, C. Kato, J. Migenda, M. Zaizen, T. Takiwaki