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

Extreme Transients in the Multimessenger Era Philipp Mösta Einstein fellow @ UC Berkeley pmoesta@berkeley.edu BlueWBlueWaters Symposium 2018 Sunriver Resort

Core-collapse supernovae neutrinos turbulence (Binary) black holes accretion disks EM counterparts ~ Extreme transients Extreme core-collapse Binary neutron stars hyperenergetic/superluminous gravitational waves +EM lGRBs sGRBs heavy elements 2 heavy elements

Core-collapse supernovae neutrinos turbulence (Binary) black holes accretion disks EM counterparts ~ Extreme transients Extreme core-collapse Binary neutron stars hyperenergetic/superluminous gravitational waves +EM lGRBs sGRBs heavy elements 3 heavy elements

Unique relativistic nuclear astrophysics laboratories nuclear EOS: EOS, nucleosynthesis, optical/EM signal neutrino transport: composition, heating/cooling, winds magnetic fields: lifetime, winds, outflows, jets relativity gravitational waves, mergers, jets 4

Astrophysics of extreme transients Gravitational waves M82/Chandra/NASA ~ Neutrinos Galaxy evolution Heavy element nucleosynthesis Birth sites of black holes / neutron stars 5

New era of transient science • 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 6 Image: PTF/ZTF/COO Image: LSST

New era of transient science • 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 Transformative years ahead for our understanding of these events 7 Image: PTF/ZTF/COO Image: LSST

Extreme Supernovae and GRBs • 11 long GRB – core-collapse supernova associations. • All GRB-SNe are stripped envelope, show outflows v~0.1c • But not all stripped-envelope supernovae come with GRBs • Trace low metallicity environments • Some SLSNe share same characteristics 8

Neutron star mergers, kilonovae and sGRBs • 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 9

The engine(s) driving these transients Superluminous Hyperenergetic SNe lGRBs Engine? sGRBs? 10 Kilonova

Common? Engine? 11 Common engine?

Progenitor Engine? 12 Common engine?

Progenitor Observations Engine? 13 Common engine?

Progenitor Observations Engine? 14 Common engine?

Progenitor Observations Engine? MPRG objective: Establish mapping progenitor -> engine -> observations 15 Common engine?

Core collapse basics Protoneutron star Iron core r~30km Nuclear equation of state 2000km 2000km stiffens at nuclear density Inner core ( ~ 0.5 ) 
 M � -> protoneutron star + shockwave 16

Core collapse basics Protoneutron star Iron core r~30km Nuclear equation of state 2000km 2000km stiffens at nuclear density Inner core ( ~ 0.5 ) 
 M � -> protoneutron star + shockwave Reviews: 
 Bethe’90 L ν Outer core accretes onto 
 Janka+‘12 shock & protoneutron accretion star with O(1) /s M � shock Shock stalls at ~ 100 km 17

Core collapse basics Protoneutron star Iron core r~30km Nuclear equation of state 2000km 2000km stiffens at nuclear density Inner core ( ~ 0.5 ) 
 M � -> protoneutron star + shockwave Reviews: 
 Bethe’90 L ν Janka+‘12 Core-collapse accretion supernova problem: How to revive the shock shockwave? 18

Core collapse basics Neutrino mechanism L ν 2000km 2000km accretion shock 19

Core collapse basics 3D Volume 
 Visualization of Entropy 2000km 2000km 20 Roberts+16

Magnetorotational mechanism [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 10 52 erg Results in ms-period proto-magnetar 
 21 Burrows+’07

A multiphysics challenge Magneto-Hydrodynamics Gas/plasma dynamics 22

A multiphysics challenge Magneto-Hydrodynamics Gas/plasma dynamics General Relativity Gravity 23

A multiphysics challenge Magneto-Hydrodynamics Gas/plasma dynamics General Relativity Gravity Nuclear EOS , nuclear 
 Nuclear and Neutrino Physics reactions & ν interactions 24

A multiphysics challenge Magneto-Hydrodynamics Gas/plasma dynamics General Relativity Gravity Nuclear EOS , nuclear 
 Nuclear and Neutrino Physics reactions & ν interactions Boltzmann Transport Theory Neutrino transport 25

A multiphysics challenge Fully coupled! Magneto-Hydrodynamics Gas/plasma dynamics General Relativity Gravity Nuclear EOS , nuclear 
 Nuclear and Neutrino Physics reactions & ν interactions Boltzmann Transport Theory Neutrino transport All four forces! 26

A multiphysics challenge Fully coupled! Magneto-Hydrodynamics Gas/plasma dynamics General Relativity Gravity Nuclear EOS , nuclear 
 Nuclear and Neutrino Physics reactions & ν interactions Boltzmann Transport Theory Neutrino transport All four forces! 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 • 27 peta/exa scale computers •

http://einsteintoolkit.org 28

R-process nucleosynthesis in magnetar-driven explosions

3D Volume 
 Visualization of Entropy PM, Richers + 14 30

Neutron-rich nucleosynthesis in supernovae Creating the heaviest elements Jet-driven explosions proposed as site for r- process • Low electron fraction • Medium entropy • Low density • High temperature 31 Sneden+ 08

Making the heaviest elements PM + 17 Halevi, PM + 18 32

R-process in jet-driven supernovae B = 10 13 G 33 Halevi, PM 18+ with Goni Halevi

3D dynamics open up diverse outcomes! solar 10 0 B13 B12-sym 10 − 2 B12 Abundance 10 − 4 10 − 6 10 − 8 0 50 100 150 200 mass number A Heaviest elements reduced by factor 100 Continued accretion -> 34 Black hole GRB engine possible PM+14, PM+ 17, Halevi, PM+18

Neutron star mergers Radice, Bernuzzi, PM 16 35

3 outcomes stable neutron star: - low mass prompt collapse to black hole: - soft EOS + high mass hypermassive neutron star + torus - delayed collapse to black hole: - everything in between? 36

Key for angular momentum transport: Magnetorotational instability M C M i M o 37

Situation after merger: Stability criterion Wavelength of FGM blue unstable B 0 ~ 5x10 14 G 38

Merger remnant evolution 0.65 Original hydro Original hydro 0.60 MHD B = 0 MHD B = 0 MHD B = 5 × 10 14 G low MHD B = 5 × 10 14 G low 0.55 MHD B = 5 × 10 14 G medium MHD B = 5 × 10 14 G medium 0.50 α min Replace plot 0.45 0.40 0.35 0.30 0 5 10 15 20 25 30 35 40 45 t − t merger [ms] PM + 18 (in prep.) 39

advanced LIGO - EM follow up Image:PanSTARRS Aasi+ 2016, LIGO GW + EM counterpart = detailed engine observations 40

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 41

3) From simulations to observations

From simulations to observations Full star State of the art now: Detailed simulations Full 3D, full physics 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 43 PM , Tchekhovskoy 17 (in prep)

From simulations to observations Future: State of the art now: Detailed simulations Full-star simulations full physics full physics 0.1-1s shock breakout inner core ~10000km Current frontier: detailed light curves 1) Engine model from detailed spectra full-physics simulations 2) Simplified simulations connect observations and with engine model to engines shock breakout map progenitor params 44

How do we form magnetars?

First global 3D MHD turbulence simulations • 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 Does the MRI efficiently build up PM+ 15 Nature dynamically relevant global field? 46

3D magnetic field structure dx=500m dx=200m dx=100m dx=50m 47 PM+ 15 Nature

48 PM+ 15 Nature