Strange nuclear matter in core-collapse supernovae

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Michigan, USA EMMI Workshop on Dense Baryonic Matter

1 Strange nuclear matter in core-collapse supernovae I. Sagert Michigan State University, East Lansing, Michigan, USA EMMI Workshop on Dense Baryonic Matter in the Cosmos and the Laboratory Tuebingen, Germany -2 October 22

2 Phase diagram of strongly interacting matter Fig.: Fredrik Sandin

3 Hyperons in neutron stars Large uncertainties in YY interaction, TBF with hyperons Microcsopic calculations: Inclusion of hyperons softens the EoS (BHF, Schulze & Rijken PRC 84 (2)) Low maximum masses of hyperon stars (<.4 M ) Gravitational Mass [M ] Radius R [km] PSR J PSR J Hulse-Taylor 2.5 Quark meson-coupling model ( Rikovska-Stone et al., NPA, Vol 792 (27); Whittenbury et al., arxiv:24.264) 2 2 SU(3) non-linear sigma model (Dexheimer and Schramm, PRC, Vol. 8 (2)) Relativistic Mean Field (Bednarek and Manka, J. Phys. G, 36 (29), Weissenborn et al. NPA, Vol. 88 (22)) Figures: top: I. Vidana et al., EPL, Vol. 94, 2, bottom: J. Rikovska Stone et al., NPA, Vol 792, 27 M g [solar mass].5.5 F-QMC7 F-QMC!4 N-QMC7 N-QMC! R [km}.5.5 8

4 Quark matter in neutron stars Bag models: Ozel et al., ApJL 724 (2), Weissenborn et al., ApJL 74 (2) Nambu-Jona-Lasinio models: Bonnano & Sedrakhian, Astron. & Astrophys. 539 (22), Blaschke et al. Phys. Rev. C 8 (29) O(α 2 s ) Perturbative QCD: Kurkela et al. Phys. Rev. D 8 (2) Dyson-Schwinger: Klaehn et al. (Phys. Rev C 82 (2 ), Chen et al. (Phys. Rev. D 84, (2) ρ tr /ρ M O.97 M O.9 M O 2SC STARS CFL STARS Figures: Ozel et al., ApJL 724 (2), Bonnano & Sedrakhian, Astron. & Astrophys. 539 (22) M O δ = G v /G s

5 Quark matter in neutron stars - EoS 2 Gibbs Maxwell Hadronic model: RMF TM (M 2.2 M ) Quark model: Bag model p = ( Ω QM = ) i Ω i + 3µ4 4π 2 ( a 4 ) + B eff ( ) a 4 = 2αs π T q = T h, p q = p h, µ i q = µ i h µ s = µ d Local charge neutrality: Maxwell transition Global charge neutrality: Gibbs transition Mixed phase with quark fraction χ = V Q V Q +V H, < χ < pressure [MeV/fm 3 ] pressure [MeV/fm 3 ] Quark Hadronic Gibbs Maxwell Baryochemical potential µ b [fm -3 ] Hadronic density [fm -3 ] Quark

6 Hybrid star maximum masses with RMF TM a 4 =.4 Maximum Mass [M solar ] a 4 =.5 a 4 = M solar Maxwell, hybrid stars Maxwell, quark core.6 Gibbs, mixed core Gibbs, quark core.5.44 M solar n c ~. /fm 3 n c ~.2 /fm 3 n c ~.3 /fm 3.4 n c ~.4 /fm 3 n c ~.5 /fm 3 n c ~.6 /fm B eff /4 [MeV] PSR J For hadronic RMF TM: Massive hybrid stars with low n crit contain only a mixed phase S. Weissenborn, I. S., G. Pagliara, M. Hempel, J. Schaffner-Bielich, ApJL 74 (2)

7 Hybrid star maximum masses with RMF NL a 4 =.4 Maximum Mass [M solar ] M solar.44 M solar a 4 = B eff /4 [MeV] a 4 =. PSR J Maxwell hybrid stars Maxwell, quark core Gibbs, mixed core Gibbs, quark core n c ~. /fm 3 n c ~.2 /fm 3 n c ~.3 /fm 3 n c ~.4 /fm 3 n c ~.5 /fm 3 For hadronic RMF NL3: Massive hybrid stars with low n crit can contain a pure quark matter core S. Weissenborn, I. S., G. Pagliara, M. Hempel, J. Schaffner-Bielich, ApJL 74 (2)

8 Massive hybrid stars 2 Demorest et al. (2) Gibbs Quark fraction χ Mass [solar mass].5 Freire et al. (28) Hulse-Taylor PSR a 4 =. a 4 =.55 TM pressure [MeV/fm 3 ] Hadronic Quark density [fm -3 ] Stiff quark EoSs can be very similar to stiff nucleonic EoSs (Alford et al., ApJ 629 (25)) Not only the stars masses but also their radii are similar How to distinguish hybrid stars from neutron stars? Cooling? Viscosity? Supernovae p = f(n b, Y p, T)!

9 Conditions in a core collapse supernova - 5 M Baryon density, log (! [g/cm 3 ]) Typical conditions after core-bounce: T MeV Y p.3 n b n Typical supernova EoSs cover: T : ( ) MeV Y p :..5 n b : ( 5 5 g ) cm 3 Temperature, T [MeV] Figure: Fischer et al., ApJS 94, 39 (2): Phase space covered in a core collapse simulation for a 5 M progenitor Baryon density, n [fm 3 Y e ] B

10 Conditions in a core collapse supernova - 4 M Baryon density, log (! [g/cm 3 ]) Typical conditions after core-bounce: T MeV Y p.3 n b n Typical supernova EoSs cover: T : ( ) MeV Y p :..5 n b : ( 5 5 g ) cm 3 Temperature, T [MeV] Figure: Fischer et al., ApJS 94, 39 (2): Phase space covered in a core collapse simulation for a 4 M progenitor Baryon density, n [fm 3 Y e ] B

11 Supernova observables Neutrino signal, gravitational waves, impact on nucleosynthesis,... SN987A: Supernova explosion of 2M progenitor Detection of 24 neutrinos during ca. 3 s Estimated for emitted energy: 2 53 erg Next galactic supernova: IceCube and Superkamiokande will observe 3 neutrinos Figures: Hirata et al., Phys. Rev. D, Vol. 38, 2 (988)

12 Quark and hyperon matter in core collapse supernovae Migdal, Chernoustan, Mishustin, Phys. Lett. B 83 (979) Takahara and Sato, Astrophys. and Space Science 9 (986) Drago and Tambini, Journal of Phys. G 25 (999) Gentile et al., Astrophys. Journal 44 (993) Pons et al., ApJ 53 (999), Pons et al., Phys.Rev.Lett. 86 (2) Nakazato et al., Phys. Rev. D 77 (28) Sumiyoshi et al., ApJL, 69 (29) I.S. Fischer et al., Phys. Rev. Lett. 2 (29)... Ishizuka et al., Journal of Phys. G 35 (28) Shen et al., Astrophys. Journal Suppl. 97 (2) Oertel, Fantina, and Novak, Phys. Rev. C 85 (22)

13 Hyperons in core-collapse of light progenitor stars E/B-M N (MeV) µ-m N (MeV) TM EOSY EOSY! n p Neutron Star Shen EOS EOSY n T= MeV, Y C =.4 p " B (fm -3 ) " B (fm -3 ) Shen et al. supernova EoS (RMF TM, M max 2.M ) extended to hyperons and thermal pions (M max.6m ) (U (N) Λ, U(N) Σ, U(N) Ξ ) =(-3MeV, +3MeV, -5MeV) Figure: Ishizuka et al., JPG. 35 (28)

14 Hyperons in core-collapse of light progenitor stars T (MeV) EOSY, Y C =.4 S/B= 5 Y/B= % % 2. % ρ B (fm -3 ) Simulation an adiabatic collapse of an iron core from 5 M progenitor No neutrino transport Small hyperon fraction. % has no effect on the supernova dynamics Figure: Ishizuka et al., JPG. 35 (28)

15 Hyperons in core-collapse SNe of massive progenitor stars 5 4 < E! > [MeV] 3 2 2x 53 L! [erg/s]..5. time after bounce [sec].5 Core-collapse supernova simulation of 4M progenitor with hyperon EoS from Ishizuka et al., JPG. 35 (28) Comparison to H.Shen EoS and Lattimer-Swesty EoS (K = 8 MeV) Hyperons appear around 5ms after core bounce and accelerate black hole production Figure: Sumiyoshi et al., ApJL, 69 (29)

16 Hyperons in core-collapse SNe of massive progenitor stars Variation of stiffness in hyperon EoS via Σ hyperon potential A = U (N) Σ =-3MeV; R = U(N) Σ =+3MeV Softening due to appearance of hyperons (M max.6m ) earlier black hole formation Figure: Nakazato et al. ApJ, 745 (22)

17 Quark matter in core-collapse SNe of massive progenitor stars Shen et al. EoS with strange quark matter and thermal pions Quark bag model: B /4 29 MeV (M max.8 M ) Core-collapse supernova simulation of 4M progenitor Black hole formation.7ms after onset of phase transition Nakazato et al., Astrophys. J. 72 (2), Ohnishi et al., Phys. Lett. B 74 (2)

18 Quark matter in core-collapse SNe of light progenitors - Stiff EoS Onset Mixed Phase 55 5 Pure Quark Phase! central evolution Baryon Density,! [ 4 g/cm 3 ] 2 Baryon Density,! [ 4 g/cm 3 ] Y p =.5 Temperature [MeV] Y p =.3 Y p =.2 Pressure [MeV/fm 3 ] 5 5 s =. k /baryon B s =.5 k B /baryon s = 2. k B /baryon Baryon Density [fm 3 ] Baryon Density, n B [fm 3 ] Shen EoS & phase transition to quark matter with PNJL model (M max 2 M ) Deconfinement to up and down quark matter, strangeness appears later D Supernova simulation of a 5 M progenitor GR hydrodynamics and Boltzmann neutrino transport in D (Liebendoerfer et al. 24) Due to high critical density no phase transition during post-bounce accretion phase Fischer et al., Physics of Atomic Nuclei 75 (22)

19 Quark matter in core-collapse SNe of light progenitors - Soft EoS 2 Steiner et al. 22 TM Demorest et al. 2 Mass [solar mass].5 B55α s 3 B62 B65 Freire et al. (28) Hulse-Taylor PSR Pressure [MeV/fm 3 ] Y p =.3, s=2 k B Quark fraction B /4 =62MeV,α s =. B /4 =65MeV,α s =. B /4 =55MeV,α s = Density [fm -3 ] Shen et al. EoS with quark bag model Ω QM = i=u,d,s,e Ω µ i + α 4 s + 4π 3 B Progenitors:.8 M, 3 M, and 5 M D GR hydrodynamics and Boltzmann neutrino transport (Liebendoerfer et al. 24) B /4 = 62MeV, 65MeV and B /4 = 55MeV & α s =.3 Sagert et al., PRL 2, 8 (29); Fischer et al., ApJS 94, 39 (2)

20 Second Shock Wave from Phase Transition Velocity [ 4 km/s] ms ms ms ms ms 26.2 ms 2 3 Mixed phase is present after core-bounce Collapse of the proto neutron star due to transition to pure quark matter 2ms - 4ms after core bounce Formation of second shock wave which leads to the explosion of the star Figure: I.S, T.Fischer, M. Hempel, G. Pagliara, J. Schaffner-Bielich, F.K. Thielemann, M. Liebendoerfer, PRL 2 (29)

21 First and Second Neutrino Bursts Luminosity [ 53 erg/s] ! e anti! e! µ/" Time after bounce [s] rms Energy [MeV] ! e anti! e! µ/" Time after bounce [s] Second shock wave passes neutrinospheres second neutrino burst dominated by antineutrinos For B /4 =65MeV second neutrino burst is 2 ms later than for B /4 =62MeV Fig: T.Fischer, Neutrino luminosities and rms neutrino energies, at 5km for M progenitor

22 Parameter study (Fischer et al., ApJS 94, 39 (2)) Prog. B /4 t pb ρ c T c M pns E expl M max M MeV ms 4 g/cm 3 MeV M 5 erg M u , α s = Higher critical density: More massive proto neutron star with deeper gravitational potential Stronger second shock and larger explosion energies Second neutrino burst later with larger peak luminosities More massive progenitor: earlier onset of phase transition and more massive proto neutron star

23 Quark matter in core-collapse SN of light progenitors - stiff EoS Mass [solar mass] 2.5 Steiner et al. 22 B55α s 3 B62 B65 TM Demorest et al. 2 Freire et al. (28) Hulse-Taylor PSR B45α s 7 B39α s 7 Temperature T [MeV] ms - 5ms post-bounce B /4 = 62 MeV B /4 = 65 MeV B /4 = 55 MeV, α s =.3 B /4 = 45 MeV, α s =.7 B /4 = 39 MeV, α s = Density n b [fm -3 ] For B /4 = 45 MeV & Collapse of 5 M and 3 M progenitors Phase transition too late s after bounce No second collapse For B /4 = 39 MeV: Earlier phase transition, but no second collapse

24 Quark matter in core-collapse SN of light progenitors - stiff EoS 2 Steiner et al. 22 TM Demorest et al. 2 Mass [solar mass].5.5 B55α s 3 B62 B65 Freire et al. (28) Hulse-Taylor PSR B45α s 7 B39α s 7 Pressure [MeV/fm 3 ] Y p =.3, s=2 k B Quark fraction Density [fm -3 ] For B /4 = 45 MeV & Collapse of 5 M and 3 M progenitors Phase transition too late s after bounce No second collapse For B /4 = 39 MeV: Earlier phase transition, but no second collapse

25 Second collapse & stiff hybrid EoS (?) NL3 Mass [solar mass] 2.5 Demorest et al. 2 Freire et al. (28) Hulse-Taylor PSR TM B45α s 7 Steiner et al. 22 B39α s 7.5 NL3, B43α s Choose stiffer hadronic EoS (NL3) Stronger phase transition and pure quark matter Caution : NL3 parameter set is too stiff with regard to heavy-ion data Caution 2: Mass-Radius relation for relevant density region look very similar

26 Second collapse & stiff hybrid EoS (?) Y p T=.MeV T=25.MeV T=52.4MeV T=MeV... n b [/fm 3 ] E/V B (MeV fm 3 ) c) BHF, x p =.4 B =2, "=.4 B =4, "=.7 B =4 (ws) B =2, "=.4 B =4, "=.7 B =4 (ws) B as = ! (fm 3 ) Quark EoS that is more flexible at higher densities and can stiffen Density dependent Bag constant [ (Burgio et al. Phys.Lett. B526 (22)) ( ) ] 2 B(ρ) = B as + (B B as) exp β ρ ρ Soft mixed phase and stiff high density quark EoS Right Figure: Burgio et al. Phys.Lett. B526 (22)

27 Summary & Conclusion Variety of studies for quark matter and hyperons in neutron stars and core-collapse supernovae Need more input on high density nuclear matter and hyperon interactions from heavy ion experiments Softening of the quark or hyperon EoS impacts the duration and spectrum of the supernova neutrino signal But: EoSs have to be stiff at high density! Only a few studies use EoSs which reproduce a neutron star mass of M NS =.97 ±.4M Will we be able to distinguish between effects from (stiff) hyperonic, quark,or hadronic EoSs? All supernova EoSs containing hyperons or quarks assume weak equilibrium with respect to strangeness production Is this a valid assumption? If not - how do we evolve strangeness in astrophysical simulations? With T. Fischer M. Hempel M. Liebendoerfer A. Mezzacappa G. Pagliara J. Schaffner-Bielich F.-K. Thielemann

28 Low critical density - Neutron stars vs. heavy ion collision 6 5 u,d,s quark matter, B /4 =65MeV, m s =MeV, a 4 =. Y p =. Y p =.3 Y p = Y p =.3, uds Y p ~.5, ud 4 4 T [MeV] 3 T [MeV] n b [fm -3 ] n b [fm -3 ] Neutron stars & supernovae Heavy ion collisions Proton Fraction Y p.3.5 Strangeness production weak interaction: d s s s Phase transition to uds quark matter ud quark matter

29 Low critical density - Neutron stars vs. heavy ion collision 8 u,d,s quark matter, B /4 =39MeV, m s =MeV, a 4 =.55 Y p =. Y p =.3 Y p = Y p =.3, uds Y p ~.5, ud 4 T [MeV] 6 4 T [MeV] n b [fm -3 ] n b [fm -3 ] Neutron stars & supernovae Heavy ion collisions Proton Fraction Y p.3.5 Strangeness production weak interaction: d s s s Phase transition to uds quark matter ud quark matter

30 Core-collapse and second shock Mixed phase of quarks and hadrons appears at core bounce in the center Velocity [km/s] log (Baryon Density [g/cm 3 ]) Electron Fraction!4! x (a) (b)!!spheres 2 3 (c) 443 ms Quark Flag Fig: T.Fischer, B /4 = 65 MeV, M progenitor

31 Core-collapse and second shock Velocity [km/s] log (Baryon Density [g/cm 3 ]) Electron Fraction!4! x (a) (b)!!spheres 2 3 (c) 443 ms 448.s ms Quark Flag Velocity [km/s] log (Baryon Density [g/cm 3 ]) Electron Fraction!4! x (a) (b)!!spheres 2 3 (c) 443 ms ms ms Quark Flag Fig: T.Fischer, B /4 = 65 MeV, M progenitor

32 Core-collapse and second shock Velocity [km/s] log (Baryon Density [g/cm 3 ]) Electron Fraction!4!!4 x (a) (b)!!spheres 2 3 (c) ms ms Quark Flag Velocity [km/s] log (Baryon Density [g/cm 3 ]) Electron Fraction!4!!4 x (a) (b)!!spheres 2 3 (c) ms ms ms Quark Flag Fig: T.Fischer, B /4 = 65 MeV, M progenitor

33 Core-collapse and second shock Velocity [km/s] log (Baryon Density [g/cm 3 ]) Electron Fraction x (a) !.4!! (b)!!spheres 2 3 (c) Quark Flag Velocity [km/s] log (Baryon Density [g/cm 3 ]) Electron Fraction x (a) !.4!! /aius [km] (b)!!sfgeres 2 3 /aius [km] (c) J e increase 2 3 /aius [km].5 Kuark Flag Fig: T.Fischer, B /4 = 65 MeV, M progenitor

Progress of supernova simulations with the Shen equation of state

Progress of supernova simulations with the Shen equation of state Nuclei K. Sumi yoshi Supernovae Numazu College of Technology & Theory Center, KEK, Japan Crab nebula hubblesite.org Applications of nuclear