Extreme Transients in the Multimessenger Era

Transcription

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

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

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

4 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

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

6 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 Image: PTF/ZTF/COO Image: LSST 6

7 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 Image: PTF/ZTF/COO Image: LSST 7

8 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

9 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

10 The engine(s) driving these transients Superluminous Hyperenergetic SNe lgrbs Engine? Kilonova 10 sgrbs?

11 Common? Engine? 11

12 Progenitor Engine? 12

13 Progenitor Observations Engine? 13

14 Progenitor Observations Engine? 14

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

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

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

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

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

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

21 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 erg Results in ms-period proto-magnetar Burrows

22 A multiphysics challenge Magneto-Hydrodynamics Gas/plasma dynamics 22

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

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

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

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

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

28 28

29 R-process nucleosynthesis in magnetar-driven explosions

30 3D Volume Visualization of Entropy PM, Richers

31 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 Sneden

32 Making the heaviest elements PM+ 17 Halevi, PM

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

34 3D dynamics open up diverse outcomes! Abundance solar B13 B12-sym B mass number A Heaviest elements reduced by factor 100 PM+14, PM+ 17, Halevi, PM Continued accretion -> Black hole GRB engine possible

35 Neutron star mergers Radice, Bernuzzi, PM 16 35

36 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

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

38 Situation after merger: Stability criterion Wavelength of FGM blue unstable B0 ~ 5x10 14 G 38

39 Merger remnant evolution amin Original hydro MHD B = 0 MHD B = Glow MHD B = Gmedium Replace plot t t merger [ms] PM+ 18 (in prep.) 39

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

41 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 41 to solving these puzzles

42 3) From simulations to observations

43 From simulations to observations State of the art now: Full star Detailed simulations full physics 0.1-1s inner core ~10000km Full 3D, full physics Current frontier: 1) Engine model from full-physics simulations 2) Simplified simulations with engine model to shock breakout PM, Tchekhovskoy 17 (in prep) 43

44 From simulations to observations State of the art now: 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 Future: Full-star simulations full physics shock breakout detailed light curves detailed spectra connect observations and engines map progenitor params 44

45 How do we form magnetars?

46 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 dynamically relevant global field? PM+ 15 Nature 46

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

48 PM+ 15 Nature 48

49 Growth at Large Scales E k,mag (t)[10 33 erg] ( ms 1 (t t map )) e (t t map)/t, t = 3.5 ms k = 4 k = 6 k = 8 k = 10 k = 20 k = 50 k = t t map [ms] PM+ 15 Nature saturation within 60ms 49

50 PM+ 15 Nature Global Field Structure dx=500m dx=50m PM+ 15 Nature t=0ms t=10ms t=10ms 50

51 PM+ 15 Nature Global Field Structure dx=500m dx=50m Magnetar formation? PM+ 15 Nature t=0ms t=10ms t=10ms 51

52 Core-collapse supernovae neutrinos turbulence (Binary) black holes accretion disks EM counterparts ~ Magnetic fields in high-energy astro Binary neutron stars gravitational waves EM counterparts sgrbs Extreme core-collapse hyperenergetic superluminous lgrbs 52

53 Core-collapse supernovae neutrinos turbulence (Binary) black holes accretion disks EM counterparts ~ Magnetic fields in high-energy astro Binary neutron stars gravitational waves EM counterparts sgrbs Extreme core-collapse hyperenergetic superluminous lgrbs 53

54 MRI 54

55 MRI Basics M C M i M o 55

56 MRI Basics 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 56

57 What s the situation in core-collapse? Stability criterion: 8 2 <! 2 BV + r d 2 dr < 0 [Balbus&Hawley 91,98, Akiyama+03, Obergaulinger+09] 57

58 Magnetorotational Mechanism MRI works locally Akiyama+03, Shibata+06 shearing box simulations Obergaulinger+09 But what about global field? Burrows

59 From simulations to observations State of the art now: 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 B i b i U i ~j ~ b... u i Get mean fields from 3D sim Squire, PM, Lecoanet 16 (in prep) 59

60 From simulations to observations State of the art now: 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 Get mean fields from 3D sim Daedalus simulation Squire, PM, Lecoanet 16 (in prep) 60

61 Magnetic field amplification: A 2D view dx=500m dx=200m dx=100m dx=50m 61

62 Energy Spectra a t t map = 10 ms E kin 50 m erg k 5/ E(k) [erg] E mag 500 m E mag 200 m E mag 100 m E mag 50 m E mag 50 m (t t map = 0 ms) k 62

63 Energy Spectra b erg k 5/3 E kin (k) t = 7 ms E(k) [erg] E mag (k) t = 0 ms t = 1 ms t = 2 ms t = 4 ms t = 6 ms t = 8 ms t = 10 ms k Turbulent saturated state after 3ms inverse cascade afterwards 63