Neutron Star Merger Dynamics www.computational-relativity.org - - PowerPoint PPT Presentation

neutron star merger dynamics
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Neutron Star Merger Dynamics www.computational-relativity.org - - PowerPoint PPT Presentation

Neutron Star Merger Dynamics www.computational-relativity.org arXiv:2002.03863 David Radice October 27, 2020 GW170817 From LIGO Scientific Collaboration and Virgo Collaboration, Fermi GBM, INTEGRAL, IceCube Collaboration, AstroSat Cadmium


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David Radice — October 27, 2020

Neutron Star Merger Dynamics

arXiv:2002.03863

www.computational-relativity.org

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GW170817

From LIGO Scientific Collaboration and Virgo Collaboration, Fermi GBM, INTEGRAL, IceCube Collaboration, AstroSat Cadmium Zinc Telluride Imager Team, IPN Collaboration, The Insight-Hxmt Collaboration, ANTARES Collaboration, The Swift Collaboration, AGILE Team, The 1M2H Team, The Dark Energy Camera GW-EM Collaboration and the DES Collaboration, The DLT40 Collaboration, GRAWITA: GRAvitational Wave Inaf TeAm, The Fermi Large Area Telescope Collaboration, ATCA: Australia Telescope Compact Array, ASKAP: Australian SKA Pathfinder, Las Cumbres Observatory Group, OzGrav, DWF (Deeper, Wider, Faster Program), AST3, and CAASTRO Collaborations, The VINROUGE Collaboration, MASTER Collaboration, J-GEM, GROWTH, JAGWAR, Caltech- NRAO, TTU-NRAO, and NuSTAR Collaborations, Pan-STARRS, The MAXI Team, TZAC Consortium, KU Collaboration, Nordic Optical Telescope, ePESSTO, GROND, Texas Tech University, SALT Group, TOROS: Transient Robotic Observatory of the South Collaboration, The BOOTES Collaboration, MWA: Murchison Widefield Array, The CALET Collaboration, IKI-GW Follow-up Collaboration, H.E.S.S. Collaboration, LOFAR Collaboration, LWA: Long Wavelength Array, HAWC Collaboration, The Pierre Auger Collaboration, ALMA Collaboration, Euro VLBI Team, Pi of the Sky Collaboration, The Chandra Team at McGill University, DFN: Desert Fireball Network, ATLAS, High Time Resolution Universe Survey, RIMAS and RATIR, and SKA South Africa/MeerKAT ApJL 848:L12 (2017)

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From LIGO Scientific Collaboration and Virgo Collaboration, Fermi GBM, INTEGRAL, IceCube Collaboration, AstroSat Cadmium Zinc Telluride Imager Team, IPN Collaboration, The Insight-Hxmt Collaboration, ANTARES Collaboration, The Swift Collaboration, AGILE Team, The 1M2H Team, The Dark Energy Camera GW-EM Collaboration and the DES Collaboration, The DLT40 Collaboration, GRAWITA: GRAvitational Wave Inaf TeAm, The Fermi Large Area Telescope Collaboration, ATCA: Australia Telescope Compact Array, ASKAP: Australian SKA Pathfinder, Las Cumbres Observatory Group, OzGrav, DWF (Deeper, Wider, Faster Program), AST3, and CAASTRO Collaborations, The VINROUGE Collaboration, MASTER Collaboration, J-GEM, GROWTH, JAGWAR, Caltech- NRAO, TTU-NRAO, and NuSTAR Collaborations, Pan-STARRS, The MAXI Team, TZAC Consortium, KU Collaboration, Nordic Optical Telescope, ePESSTO, GROND, Texas Tech University, SALT Group, TOROS: Transient Robotic Observatory of the South Collaboration, The BOOTES Collaboration, MWA: Murchison Widefield Array, The CALET Collaboration, IKI-GW Follow-up Collaboration, H.E.S.S. Collaboration, LOFAR Collaboration, LWA: Long Wavelength Array, HAWC Collaboration, The Pierre Auger Collaboration, ALMA Collaboration, Euro VLBI Team, Pi of the Sky Collaboration, The Chandra Team at McGill University, DFN: Desert Fireball Network, ATLAS, High Time Resolution Universe Survey, RIMAS and RATIR, and SKA South Africa/MeerKAT ApJL 848:L12 (2017)

  • How did these binaries form?
  • How do neutron star mergers power gamma-ray bursts?
  • What are neutron stars made of? Nucleons, hyperons,

deconfined quarks?

  • Was the gold in my wedding ring formed in a neutron star

merger? Was it swirling around in an accretion disk? Or was it tidally ejected prior to the cataclysmic collision?

Open questions

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WhiskyTHC

http://personal.psu.edu/~dur566/whiskythc.html

THC: Templated Hydrodynamics Code

  • Full-GR, dynamical spacetime*
  • Nuclear EOS
  • Effective neutrino treatment
  • High-order hydrodynamics
  • Open source!

* using the Einstein Toolkit metric solvers

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Neutron rich outflows

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Compact object + disk

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Neutron star merger evolution

GWs Viscosity Neutrinos

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The inspiral phase

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Gravitational waves

GW170817 — In the frequency domain vs theory prediction https://teobresums.github.io/gwevents/

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Gravitational waves

GW170817 — In the frequency domain vs theory prediction https://teobresums.github.io/gwevents/

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The CoRe database

Dietrich, DR, Bernuzzi+ CQG 35:LT01 (2018)

www.computational-relativity.org

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The CoRe database

Dietrich, DR, Bernuzzi+ CQG 35:LT01 (2018)

www.computational-relativity.org

Open Science

  • Outflow composition, mass, velocity
  • r-process nucleosynthesis results
  • Simulation code, postprocessing routines
  • Initial data and input files
  • Other data available on request
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Early postmerger evolution

z

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Dynamical mass ejection

DR, Galeazzi+ MRAS 460:3255 (2016) See also Bausswein+ 2013, Hotokezaka+ 2013, Wanajo+ 2014, Sekiguchi+ 2015, 2016, Foucart+ 2016, Lehner+ 2016, Dietrich+ 2016, DR+ 2018, …

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The kilonova in GW170817

From Villar et al. ApJL 851:L21 (2017)

M red

ej

' 0.05M, vred

ej

' 0.15c. M blue

ej

' 0.02M, vblue

ej

' 0.25c.

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Theory vs observations

0.05 0.10 0.15 0.20 0.25 0.30 0.35

hYe; eji

10°3 10°2 10°1 Mej [MØ]

Tot.Ej. Sec.Ej Blue kN [S] Red kN [S] LS220 DD2 SLy4 SFHo BLh

Dynamical ejecta

From Nedora, Bernuzzi, DR+, 2008.04333

Spiral-wave wind? Viscous wind?

−100 −50

50 100 X [km]

−100 −50

50 100 Z [km] BLh q=1.00 (SR), t − tmerg = 88 ms 0.05 0.10 0.15 0.20 0.25 0.30 0.35 0.40 0.45 Ye 10 20 30 40 50 s [kb/baryon]

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Disk formation I

Mchirp = 1.188 M

Bernuzzi, …, DR+, arXiv:2003.06015

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Disk formation II

Bernuzzi, …, DR+, arXiv:2003.06015

Prompt-BH with large disk!

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Disk masses

−3 −2 −1 log(Mdisk/MØ)

BHBΛφ DD2 LS220 SFHo Fit Fit

250 500 750 1000 1250 1500 ˜ Λ −1 1 ∆ log(Mdisk/MØ)

DR, Perego+ ApJL 852:L29 (2018); DR & Dai, Eur. Phys. J. A 55: 50 (2019)

See also Krüger+ 2020; Salafia+ 2020; …

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Equation of state constraints

200 400 600 800 1000 ˜ Λ PDF

GW Only GW + EM Prior

DR, Perego+ ApJL 852:L29 (2018); DR & Dai, Eur. Phys. J. A 55: 50 (2019)

See also Gamba+ 2020

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Equation of state constraints

6 8 10 12 14 16 R1.4 [km] PDF

GW Only GW + EM Prior NICER

DR, Perego+ ApJL 852:L29 (2018); DR & Dai, Eur. Phys. J. A 55: 50 (2019)

See also Gamba+ 2020

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Equation of state constraints

6 8 10 12 14 16 R1.4 [km] PDF

GW Only GW + EM Prior NICER

6 8 10 12 14 16 R1.4 [km] PDF

GW Only GW + EM Prior NICER

  • Potential to constrain the EOS and/or q: the basic

physics is understood and included in the simulations

  • Modeling uncertainties appear to be under control
  • Need to explore the parameter space: EOS, mass

ratios, etc.

DR, Perego+ ApJL 852:L29 (2018); DR & Dai, Eur. Phys. J. A 55: 50 (2019)

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Long-term evolution

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End of the GW-driven phase

4.0 4.5 5.0 5.5 6.0 6.5 J [G c°1M 2

Ø]

10°2 10°1 100 101 102 103 J/ ˙ JGW [s]

BHBΛφ DD2 LS220 SFHo DD2 – (1.35 + 1.35)MØ – M0 DD2 – (1.35 + 1.35)MØ – M0

DR, Perego, Bernuzzi, Zhang, MNRAS 481:3670 (2018)

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Secular evolution: NS remnants

3 4 5 6 7 8 9 J [G c°1M 2

Ø]

2.50 2.75 3.00 3.25 3.50 3.75 4.00 Mb [MØ]

BHBΛφ

BH HMNS SMNS MNS RNS RNS

2.32 2.54 2.75 2.95 3.16 3.36 3.55 M [MØ]

DR, Perego, Bernuzzi, Zhang, MNRAS 481:3670 (2018)

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Spiral-wave wind (I)

20 40 60 80 100 t tmerg [ms] 0.0 0.5 1.0 Mej [102M]

DD2 Dyn. DD2 Wind LS220 Dyn. LS220 Wind

From Nedora, Bernuzzi, DR+, ApJL 886:L30 (2019)

50 100 150 Mass number, A 10−4 10−3 10−2 10−1 Relative final abundances

DD2 Dyn. DD2 Dyn.+Wind LS220 Dyn. LS220 Dyn.+Wind

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Spiral-wave wind (II)

100 101 time [days] 16 18 20 22 24 AB magnitude at 40 Mpc g band 100 101 time [days] z band 100 101 time [days] Ks band

LS220 DD2 AT2017gfo

0.5 1.0 1.5 2.0 2.5 3.0 Mej [102M]

Viscous wind?

From Nedora, Bernuzzi, DR+, ApJL 886:L30 (2019)

Promising, but incomplete, and not the only possible explanation

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Future Challenges

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Neutrino physics

From Sekiguchi+ 2011 From Miller+ 2019 See also: Dessart+ 2008, Perego+ 2014, Just+ 2015, Metzger+ 2014, Foucart+ 2016, Siegel & Metzger 2018, Fujibayashi+ 2017, 2020 …

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MHD turbulence

Mösta, DR+, ApJL 2020 Kiuchi+ 2014 Siegel & Metzger 2018 See also Price & Rosswog 2006; Andreson+ 2008; Etienne+ 2011; Endrizzi+ 2014; Giacomazzo+ 2015; Ruiz+ 2016; Palenzuela+ 2016; Fernandez+ 2018; Ciolfi+ 2019; …

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Merger outcome

4 5 6 J [G c1M2

]

2.850 2.875 2.900 2.925 2.950 2.975 3.000 Mb [M] BLh* q=1.00 (SR)

JADM JGW Expected Evolution Mb, J evolution (3D data) extrapolation (every 50 ms) RNS

2.59 2.62 2.64 2.67 2.69 2.72 M [M]

From Nedora, Bernuzzi, DR+, 2008.04333

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  • Inspiral and early postmerger are better understood, but there is

still a vast parameter space volume to explore.

  • We can already do multimessenger astrophysics!
  • The physics becomes increasingly complex on longer timescales

in the postmerger. Higher resolution, longer, and more sophisticated simulations are needed.

Conclusions