Extreme Transients in the Multimessenger Era Philipp Msta Einstein - - PowerPoint PPT Presentation

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Extreme Transients in the Multimessenger Era Philipp Msta Einstein - - PowerPoint PPT Presentation

Feb 10, 2023 166 likes •815 views

Extreme Transients in the Multimessenger Era Philipp Msta Einstein fellow @ UC Berkeley pmoesta@berkeley.edu BlueWBlueWaters Symposium 2018 Sunriver Resort Core-collapse supernovae neutrinos turbulence (Binary) black holes accretion

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Philipp Mösta

Einstein fellow @ UC Berkeley

pmoesta@berkeley.edu

BlueWBlueWaters Symposium 2018 Sunriver Resort

Extreme Transients in the Multimessenger Era

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~

(Binary) black holes

accretion disks EM counterparts

Core-collapse supernovae

neutrinos turbulence

Extreme core-collapse

hyperenergetic/superluminous lGRBs heavy elements

Binary neutron stars

gravitational waves +EM sGRBs heavy elements

Extreme transients

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Extreme core-collapse

hyperenergetic/superluminous lGRBs heavy elements

Core-collapse supernovae

neutrinos turbulence

(Binary) black holes

accretion disks EM counterparts

Binary neutron stars

gravitational waves +EM sGRBs heavy elements

Extreme transients

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magnetic fields: lifetime, winds, outflows, jets nuclear EOS: EOS, nucleosynthesis, optical/EM signal neutrino transport: composition, heating/cooling, winds

Unique relativistic nuclear astrophysics laboratories

relativity gravitational waves, mergers, jets

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~

Astrophysics of extreme transients

Galaxy evolution

M82/Chandra/NASA

Heavy element nucleosynthesis Birth sites of black holes / neutron stars Neutrinos Gravitational waves

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New era of transient science

Image: PTF/ZTF/COO Image: LSST

  • Current (PTF

, DeCAM, ASAS-SN) and upcoming wide-field time domain astronomy (ZTF , LSST , …) -> wealth of data

  • adv LIGO / gravitational waves detected
  • Computational tools at dawn of new exascale era
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New era of transient science

Image: PTF/ZTF/COO Image: LSST

Transformative years ahead for our understanding of these events

  • Current (PTF

, DeCAM, ASAS-SN) and upcoming wide-field time domain astronomy (ZTF , LSST , …) -> wealth of data

  • adv LIGO / gravitational waves detected
  • Computational tools at dawn of new exascale era
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  • But not all stripped-envelope supernovae come with GRBs
  • Trace low metallicity environments
  • Some SLSNe share same characteristics
  • 11 long GRB – core-collapse supernova associations.
  • All GRB-SNe are stripped envelope, show outflows v~0.1c

Extreme Supernovae and GRBs

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  • Remnant lifetime and fate
  • sGRB engine: black hole vs magnetar, structure of the jet
  • Dynamical ejecta and disk outflows: composition and

amount of ejecta -> EM observations

Neutron star mergers, kilonovae and sGRBs

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Engine?

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Superluminous Hyperenergetic SNe lGRBs sGRBs? Kilonova

The engine(s) driving these transients

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Common engine?

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Common? Engine?

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Common engine?

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Progenitor

Engine?

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Common engine?

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Observations

Progenitor

Engine?

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Common engine?

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Observations

Progenitor

Engine?

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Common engine?

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Observations

Progenitor

Engine? MPRG objective: Establish mapping progenitor -> engine -> observations

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2000km Protoneutron star r~30km Iron core

Nuclear equation of state stiffens at nuclear density Inner core (~0.5 ) 


  • > protoneutron star +

shockwave M

2000km

Core collapse basics

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2000km

Outer core accretes onto
 shock & protoneutron star with O(1) /s Shock stalls at ~ 100 km

Reviews:
 Bethe’90 Janka+‘12

Protoneutron star r~30km Iron core

M

2000km

Nuclear equation of state stiffens at nuclear density Inner core (~0.5 ) 


  • > protoneutron star +

shockwave M

Core collapse basics

accretion

Lν

shock

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2000km

Core-collapse supernova problem: How to revive the shockwave?

Reviews:
 Bethe’90 Janka+‘12

accretion

Lν

shock Protoneutron star r~30km Iron core 2000km

Nuclear equation of state stiffens at nuclear density Inner core (~0.5 ) 


  • > protoneutron star +

shockwave M

Core collapse basics

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2000km accretion

Lν

shock 2000km

Core collapse basics

Neutrino mechanism

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2000km 2000km Roberts+16 3D Volume 
 Visualization of

Entropy

Core collapse basics

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Magnetorotational mechanism

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[LeBlanc & Wilson ‘70, Bisnovatyi-Kogan ’70, Obergaulinger+’06, Burrows+ ‘07, Takiwaki & Kotake ‘11, Winteler+ 12]

Rapid Rotation + B-field amplification
 (need magnetorotational instability [MRI];
 difficult to resolve, but see, e.g, Obergaulinger+’09, PM+15) 2D: Energetic bipolar explosions Energy in rotation up to 1052 erg Results in ms-period proto-magnetar


Burrows+’07

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Gas/plasma dynamics Magneto-Hydrodynamics

A multiphysics challenge

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Gas/plasma dynamics Gravity Magneto-Hydrodynamics

General Relativity

A multiphysics challenge

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Gas/plasma dynamics

Nuclear EOS, nuclear 
 reactions & ν interactions

Gravity Magneto-Hydrodynamics

Nuclear and Neutrino Physics General Relativity

A multiphysics challenge

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Gas/plasma dynamics

Nuclear EOS, nuclear 
 reactions & ν interactions

Gravity

Neutrino transport

Magneto-Hydrodynamics

Nuclear and Neutrino Physics General Relativity Boltzmann Transport Theory

A multiphysics challenge

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Gas/plasma dynamics

Nuclear EOS, nuclear 
 reactions & ν interactions

Gravity

Neutrino transport

Fully coupled!

Magneto-Hydrodynamics

Nuclear and Neutrino Physics General Relativity Boltzmann Transport Theory

All four forces!

A multiphysics challenge

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Magneto-Hydrodynamics

Nuclear and Neutrino Physics General Relativity Boltzmann Transport Theory

Nuclear EOS, nuclear 
 reactions & ν interactions Neutrino transport

Fully coupled!

Additional Complication: Core-Collapse Supernovae are 3D

  • rotation
  • fluid and MHD instabilities, multi-D structure, spatial scales

Need 21st century tools:

  • cutting edge numerical algorithms
  • sophisticated open-source software infrastructure
  • peta/exa scale computers

All four forces!

A multiphysics challenge

Gas/plasma dynamics Gravity

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http://einsteintoolkit.org

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R-process nucleosynthesis in magnetar-driven explosions

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3D Volume 
 Visualization of

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Entropy

PM, Richers+ 14

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Jet-driven explosions proposed as site for r- process

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Neutron-rich nucleosynthesis in supernovae

Creating the heaviest elements

  • Low electron

fraction

  • Medium entropy
  • Low density
  • High

temperature

Sneden+ 08

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Making the heaviest elements

PM+ 17 Halevi, PM+ 18

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R-process in jet-driven supernovae

Halevi, PM 18+

B = 1013 G

with Goni Halevi

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3D dynamics open up diverse outcomes!

PM+14, PM+ 17, Halevi, PM+18

Heaviest elements reduced by factor 100

50 100 150 200

mass number A

10−8 10−6 10−4 10−2 100

Abundance

solar B13 B12-sym B12

Continued accretion -> Black hole GRB engine possible

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Radice, Bernuzzi, PM 16

Neutron star mergers

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stable neutron star:

  • low mass

prompt collapse to black hole:

  • soft EOS + high mass

3 outcomes

hypermassive neutron star + torus - delayed collapse to black hole:

  • everything in between?
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MC Mi Mo

Key for angular momentum transport:

Magnetorotational instability

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Stability criterion Wavelength of FGM

Situation after merger:

blue unstable B0 ~ 5x1014 G

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Merger remnant evolution

PM+ 18 (in prep.)

Replace plot

5 10 15 20 25 30 35 40 45 0.30 0.35 0.40 0.45 0.50 0.55 0.60 0.65

t − tmerger [ms] αmin

Original hydro MHD B = 0 MHD B = 5 × 1014 G low MHD B = 5 × 1014 G medium Original hydro MHD B = 0 MHD B = 5 × 1014 G low MHD B = 5 × 1014 G medium

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advanced LIGO - EM follow up

Image:PanSTARRS Aasi+ 2016, LIGO

GW + EM counterpart = detailed engine observations

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Summary

New (hyperenergetic/superluminous) transients challenge our engine models Need detailed massively parallel 3D GRMHD simulations to interpret observational data Magnetoturbulence and large-scale dynamo action create conditions for magnetar engine Robust r-process elements only from iron cores that were magnetized strongly precollapse High-performance computing and BlueWaters key to solving these puzzles

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3) From simulations to observations

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From simulations to observations

State of the art now: Current frontier:

Detailed simulations full physics 0.1-1s inner core ~10000km PM, Tchekhovskoy 17 (in prep)

Full 3D, full physics Full star

1) Engine model from full-physics simulations 2) Simplified simulations with engine model to shock breakout

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From simulations to observations

State of the art now:

Future:

Full-star simulations full physics shock breakout detailed light curves detailed spectra connect observations and engines map progenitor params

Detailed simulations full physics 0.1-1s inner core ~10000km

Current frontier:

1) Engine model from full-physics simulations 2) Simplified simulations with engine model to shock breakout

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How do we form magnetars?

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First global 3D MHD turbulence simulations

Does the MRI efficiently build up dynamically relevant global field?

  • 10 billion grid points (Millenium

simulation used 10 billion particles)

  • 130 thousand cores on Blue Waters
  • 2 weeks wall time
  • 60 million compute hours
  • 10000x more expensive than any

previous simulations

PM+ 15 Nature

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3D magnetic field structure

dx=500m dx=50m dx=200m dx=100m

PM+ 15 Nature

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PM+ 15 Nature

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Growth at Large Scales

saturation within 60ms

5 10 1 2 3 4 5 6 7

t − tmap [ms] Ek,mag(t) [1033 erg] (−2.05 + 0.75 ms−1 · (t − tmap)) · 1033

5 · 1032 e(t−tmap)/τ, τ = 3.5 ms k = 4 k = 6 k = 8 k = 10 k = 20 k = 50 k = 100

(−2.05 + 0.75 ms−1 · (t − tmap)) · 1033

5 · 1032 e(t−tmap)/τ, τ = 3.5 ms k = 4 k = 6 k = 8 k = 10 k = 20 k = 50 k = 100

PM+ 15 Nature

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Global Field Structure

t=0ms dx=500m dx=50m t=10ms t=10ms

PM+ 15 Nature PM+ 15 Nature

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Global Field Structure

t=0ms dx=500m dx=50m t=10ms t=10ms

PM+ 15 Nature

Magnetar formation?

PM+ 15 Nature

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(Binary) black holes

accretion disks EM counterparts

Extreme core-collapse

hyperenergetic superluminous lGRBs

Binary neutron stars

gravitational waves EM counterparts sGRBs

Core-collapse supernovae

neutrinos turbulence

Magnetic fields in high-energy astro

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Extreme core-collapse

hyperenergetic superluminous lGRBs

Binary neutron stars

gravitational waves EM counterparts sGRBs

Core-collapse supernovae

neutrinos turbulence

Magnetic fields in high-energy astro

(Binary) black holes

accretion disks EM counterparts

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MRI

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MRI Basics

MC Mi Mo

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  • Weak field instability
  • Requires negative angular velocity gradient
  • Can build up magnetic field exponentially fast
  • Extensively researched in accretion disks: ability to

modulate angular momentum transport and grow large scale field

MRI Basics

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Stability criterion:

[Balbus&Hawley 91,98, Akiyama+03, Obergaulinger+09]

What’s the situation in core-collapse?

−8Ω2 < ω2

BV + rdΩ2

dr < 0

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Magnetorotational Mechanism

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  • MRI works locally

Akiyama+03, Shibata+06

  • shearing box

simulations

But what about global field?

Obergaulinger+09

Burrows+’07

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From simulations to observations

State of the art now: Current frontier:

Detailed simulations full physics 0.1-1s inner core ~10000km Squire, PM, Lecoanet 16 (in prep) 1) Engine model from full-physics simulations 2) Simplified simulations with engine model to shock breakout

Bi bi ui U i

~ j ×~ b

...

Get mean fields from 3D sim

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From simulations to observations

State of the art now: Current frontier:

Detailed simulations full physics 0.1-1s inner core ~10000km Squire, PM, Lecoanet 16 (in prep) 1) Engine model from full-physics simulations 2) Simplified simulations with engine model to shock breakout

5 10 15 20 25
  • 20
  • 10
10 20
  • 5.0×10-7
5.0×10-7 1.5×10-6 2.5×10-6

Daedalus simulation Get mean fields from 3D sim

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Magnetic field amplification: A 2D view

dx=500m dx=50m dx=200m dx=100m

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Energy Spectra

1 10 100 1028 1029 1030 1031 1032 1033 1034 1035 1036 k E(k) [erg]

a

t − tmap = 10 ms Emag 500 m Emag 200 m Emag 100 m Emag 50 m Emag 50 m (t − tmap = 0 ms) Ekin 50 m 5 · 1036 erg · k−5/3 Ekin 50 m 5 · 1036 erg · k−5/3

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  • Turbulent saturated state after 3ms
  • inverse cascade afterwards

1 10 100 1028 1029 1030 1031 1032 1033 1034 1035 1036

b

k E(k) [erg] Emag(k) t = 0 ms t = 1 ms t = 2 ms t = 4 ms t = 6 ms t = 8 ms t = 10 ms 5 · 1036 erg · k−5/3 Ekin(k) t = 7 ms 5 · 1036 erg · k−5/3 Ekin(k) t = 7 ms

Energy Spectra