Equation of State Effects on the Birth of Compact Objects Andr da - - PowerPoint PPT Presentation

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Equation of State Effects on the Birth of Compact Objects Andr da - - PowerPoint PPT Presentation

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. . . . . . . . . . . . . . Introduction EOS BH formation Summary Equation of State Effects on the Birth of Compact Objects Andr da Silva Schneider E. OConnor, A. Betranhandy and S. Zha (Stockholm University) Compact

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Introduction EOS BH formation Summary

Equation of State Effects

  • n the Birth of Compact Objects

André da Silva Schneider

  • E. O’Connor, A. Betranhandy and S. Zha

(Stockholm University)

Compact Objects for All Lund, Sweden

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

Phase-diagram

Figures by Lavrik, FRIB, CERN, Gandolfi, Demorest, NICER, NASA GSFC & Caltech/MIT/LIGO Lab, Ott, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

From astrophysical observables to basic interactions?

? ?

Figures by Orduña, NASA GSFC & Caltech/MIT/LIGO Lab, and Kamiokande/IMB/Baskan

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Introduction EOS BH formation Summary

From basic interactions to astrophysical observables

10 11 12 13 14 15 R [km] 0.5 1.0 1.5 2.0 2.5 Mgrav [M⊙]

PSR J0348+0432 PSR J0030+0451 GW170817

Figures by Orduña, OpenStax-CNX, LIGO/Virgo, IUPAP

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Introduction EOS BH formation Summary

Simulations

Figures from Rosswog, Kiuchi, and Ott

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Introduction EOS BH formation Summary

Role of the EOS in CCSNe

  • When does collapse start, p+e− → n+νe.
  • Density which collapse halts.
  • Heat produced during collapse.
  • Mass/size of the PNS core.
  • Momentum transferred to the shock.
  • Rate νs are produced.
  • Gravitational wave signal.
  • PNS properties and cooling rate.
  • Cold NS star mass, radius and composition.
  • If PNS collapses to a BH and when.
  • ...
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Introduction EOS BH formation Summary

Equation of State EOS at T = 0: ε(n,y) = εis(x)+δ 2εiv(x)+O(δ 4) where δ = 1−2y, y =

np np+nn , and x = (n−nsat)/3nsat.

εis(x) = εsat + 1 2!Ksatx2 + 1 3!Qsatx3 +... , εiv(x) = εsym +Lsymx+ 1 2!Ksymx2 + 1 3!Qsymx3 +... , Empirical parameters may be constrained by experiments and/or theory and/or observations.

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Introduction EOS BH formation Summary

Effects of changes in incompressibility NS mass radius

10 11 12 13 14 R [km] 0.0 0.5 1.0 1.5 2.0 2.5 Mgrav [M⊙]

Antoniadis et al. Most et al. N¨ atill¨ a et al.

Ksat[MeV] : 200 215 230 245 260 Ksym[MeV] : −300 −200 −100 100

Schneider et al. Phys Rev C 96 065802 (2017)

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Introduction EOS BH formation Summary

Effects of changes in incompressibility Neutrino from core-collapse of a 20M⊙ star

0.0 0.2 0.4 0.6 0.8 1.0 t − tbounce [s] 30 40 50 60 70 Lν [1051 erg s−1]

¯ νe

Ksat[MeV] : 200 215 230 245 260 Ksym[MeV] : −300 −200 −100 100

Schneider et al. Phys Rev C 96 065802 (2017)

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Introduction EOS BH formation Summary

Equation of State EOS at finite T: ε(n,y,T) = εkin(n,y,T)+εpot(n,y). Kinetic energy term: εkin(n,y,T) = 1 n ( ¯ h2τn 2m⋆

n

+ ¯ h2τp 2m⋆

p

)

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Introduction EOS BH formation Summary

Effects of changes in effective mass NS mass radius

10 11 12 13 14 R [km] 0.0 0.5 1.0 1.5 2.0 2.5 Mgrav [M⊙]

Antoniadis et al. Most et al. N¨ atill¨ a et al.

m⋆ [mn] : 0.55 0.65 0.75 0.85 0.95 ∆m⋆ [mn] : −0.10 0.00 0.10 0.20 0.30

Schneider et al. Phys Rev C 96 065802 (2017)

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Introduction EOS BH formation Summary

Effects of changes in effective mass Neutrino from core-collapse of a 20M⊙ star

0.0 0.2 0.4 0.6 0.8 1.0 t − tbounce [s] 30 40 50 60 70 Lν [1051 erg s−1]

¯ νe

m⋆ [mn] : 0.55 0.65 0.75 0.85 0.95 ∆m⋆ [mn] : −0.10 0.00 0.10 0.20 0.30

Schneider et al. Phys Rev C 96 065802 (2017)

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Introduction EOS BH formation Summary

Effects of changes in effective mass Shock radii for CCSNe with increasing effective mass

0.0 0.1 0.2 0.3 0.4 t − tbounce [s] 100 200 300 400 500 Rshock [km]

Average shock radius Max/min shock radius

SLy40.6 SLy40.7 SLy40.8 SLy40.9 SLy41.0 LS220

Schneider et al. Phys Rev C 96 065802 (2017)

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Introduction EOS BH formation Summary

Collapse of a 40M⊙ star

0.0 0.5 1.0 1.5 2.0 2.5 Mgrav [M⊙] 2 4 6 s [kB baryon−1]

s = 4.0 kB baryon−1

200 400 600 800

t − tbounce[ms]

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Introduction EOS BH formation Summary

BH formation Maximum NS mass Mmax

grav for NS with constant entropy s.

1 2 3 4 5 6

s [kB baryon−1]

2.0 2.2 2.4 2.6 2.8 3.0

MPNS

grav [M⊙]

P(4)

SNM[MeV fm−3] :

100.0 112.5 125.0 137.5 150.0 P(4)

PNM[MeV fm−3] :

160.0 180.0 200.0 220.0 240.0

EOSs have distinct T = 0 form but same T dependence. Schneider et al. arXiv:2001.10434

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Introduction EOS BH formation Summary

BH formation PNS mass MPNS

grav and most common entropy ˜

s inside PNS.

1 2 3 4 5 6

s [kB baryon−1]

2.0 2.2 2.4 2.6 2.8 3.0

MPNS

grav [M⊙]

P(4)

SNM[MeV fm−3] :

100.0 112.5 125.0 137.5 150.0 P(4)

PNM[MeV fm−3] :

160.0 180.0 200.0 220.0 240.0 s40WH07

EOSs have distinct T = 0 form but same T dependence. Schneider et al. arXiv:2001.10434

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Introduction EOS BH formation Summary

BH formation PNS collapse path in MPNS

grav −˜

s space and BH formation point.

1 2 3 4 5 6

s [kB baryon−1]

2.0 2.2 2.4 2.6 2.8 3.0

MPNS

grav [M⊙]

P(4)

SNM[MeV fm−3] :

100.0 112.5 125.0 137.5 150.0 P(4)

PNM[MeV fm−3] :

160.0 180.0 200.0 220.0 240.0 s40WH07

EOSs have distinct T = 0 form but same T dependence. Schneider et al. arXiv:2001.10434

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Introduction EOS BH formation Summary

BH formation Mmax

grav(s) and MPNS grav −˜

s paths for multiple progenitors.

1 2 3 4 5 6

s [kB baryon−1]

2.0 2.2 2.4 2.6 2.8 3.0

MPNS

grav [M⊙]

P(4)

SNM[MeV fm−3] :

100.0 112.5 125.0 137.5 150.0 P(4)

PNM[MeV fm−3] :

160.0 180.0 200.0 220.0 240.0 s50WH07 s25WH07 z25WHW02 s40WH07 u40WHW02 u75WHW02

EOSs have distinct T = 0 form but same T dependence. Schneider et al. arXiv:2001.10434

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Introduction EOS BH formation Summary

BH formation Mmax

grav(s) and MPNS grav −˜

s paths for multiple progenitors.

1 2 3 4 5 6

s [kB baryon−1]

2.0 2.2 2.4 2.6 2.8 3.0

MPNS

grav [M⊙]

m⋆ [mn] : 0.55 0.65 0.75 0.85 0.95 ∆m⋆ [mn] : −0.10 0.00 0.10 0.20 0.30 s50WH07 s25WH07 z25WHW02 s40WH07 u40WHW02 u75WHW02

EOSs have same T = 0 form but distinct T dependence. Schneider et al. arXiv:2001.10434

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Introduction EOS BH formation Summary

  • SNe (and NS mergers) are hot!
  • Temperature effects have large contributions to

core-collapse dynamics, but are still poorly constrained.

  • PNS path towards BH formation is almost EOS

independent in MPNS

grav −˜

s space.

  • Simplifies CCSNe studies that compare multiple EOSs.
  • SNe neutrino and GW signals can be used to constrain

temperature dependence of the EOS.