David Blaschke Univ. Wroclaw & JINR Dubna

Transcription

1 David Blaschke Univ. Wroclaw & JINR Dubna Warszawa, 28 th November 2007

2 David Blaschke Univ. Wroclaw & JINR Dubna Mass & Spin Phase diagram Mass clustering = Phase transition High density EoS with Phase transition Masquerade and Cooling of Hybrid stars Phase diagram of dense matter Warszawa, 28 th November 2007

3 Young binary system: 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Masses of Neutron Stars in binaries - clustering vs. maximum Old binary system Lattimer, Prakash, PRL 94 (2005) updates

4 LMXB s show: Accretion (mass/spin evolution) X-ray bursts with quasiperiodic brightness oscillations (QPO s) further GRT effects (ISCO) Ω {khz] No Stationary Rotating Stars Ω max (N) Hadronic Stars over 100 million years about 60 million years N crit (Ω) 0.6 TG 1.0 TG Quark Core Stars N max (Ω) N [N sun ] Black Holes Poghosyan, Grigorian, D.B., ApJ 551: L73 (2001) ν [khz] Phase transition signal: Population clustering at N crit (Ω) QPO-phenomenon gives information about Mass-radius relation Rotation frequency Ω N plane Hertzsprung-Russell diagram for binaries!

5 Ω 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Double Neutron star: Masses in Double Neutron Stars - a Waiting Point phenomenon? Moment of Inertia Ω [khz] No Stationary Rotating Stars Hadronic Stars Quark Core Stars Black Holes N/N. N Ω [khz] DBHF (Bonn A) - NJL Neutron Stars M crit (Ω), =1.017 M crit (Ω), =1.020 M max (Ω) Ω max (M) J J B J (A) B B C J B Hybrid Stars B J (B) J Black Holes M [M sun ] E. van den Heuvel, arxiv: [astro-ph] D.B., T. Klähn, F. Weber, CBM Theory Book (2007)

6 Double core scenario: 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Baryon mass vs. gravitational mass - constraint or consistency? He v CO M G [M sun ] NLρδ D 3 C NLρ KVOR DD-F4 DBHF (Bonn A) BBG KVR APR98 FPS WFF without loss with 1% loss with 2% loss X X 1.23 J (B) v X X M N [M sun ] Dewi et al., MNRAS (2006) Podsiadlowski et al., MNRAS 361 (2005) 1243 D.B., T. Klähn, F. Weber, CBM Theory Book (2007)

7 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Cooling + Structure 2.5 PSR B B [MeV] E ,4 0,8 n [fm -3 ] NLρ NLρδ D 3 C DD-F4 KVR KVOR BBG DBHF E S 0 0,4 0,8 n [fm -3 ] E 0 + α 2 E S 0 0,4 0,8 n [fm -3 ] M [M sun ] typical neutron stars NLρ NLρδ D 3 C DD-F4 KVR KVOR BBG DBHF (Bonn A) n(r = 0) [fm -3 ] DU threshold for most hadronic EoS active in neutron stars with typical masses! Klähn, et al., PRC 74, (2006); [nucl-th/ ]

8 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling log 10 (T s [K]) Crab 3C58 Brightness Constraint Vela EoS: DBHF Crust: Tsuruta law Gaps: AV18 (Takatsuka et al.) CTA 1 M/M O = RXJ log 10 (t[yr]) log 10 (T s [K]) Crab 3C58 Brightness Constraint M/M O = Vela 5.8 EoS: DDF-4 CTA 1 Crust: Tsuruta law RXJ 1856 Gaps: AV18 (Takatsuka et al.) log 10 (t[yr]) DU threshold sensitivity to tiny mass variations; Description of Vela not possible with typical masses! S. Popov et al., PRC 74 (2006); D.B. and H. Grigorian, Prog. Part. Nucl. Phys. 59 (2007) 139

9 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling 40 DBHF DDF Popov et al. (2006) ,2 M [M O ] DU threshold: overpopulation of a small mass window; Hadronic cooling not fast enough to describe Vela with M < 1.5 M! D.B. and H. Grigorian, Prog. Part. Nucl. Phys. 59 (2007) 139; [astro-ph/ ]

10 M [M sun ] causality constraint NLρ NLρδ 4U D 3 C DD-F4 KVR KVOR BBG DBHF (Bonn A) APR (Dany Page) XTE J RX J1856 4U R [km] P [MeV fm -3 ] Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Flow constraint NLρ, NLρδ D 3 C DD-F4 KVR KVOR BBG DBHF (Bonn A) n [fm -3 ] Large Mass ( 2 M ) and radius (R 12 km) stiff EoS; Flow in Heavy-Ion Collisions not too stiff EoS! Klähn, D.B., Typel, Fuchs, Faessler, Grigorian, Miller, Roepke, Truemper, et al. PRC 74, (2006)

11 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling causality constraint PSR J RX J EXO M [M sun ] DBHF - Bonn A DU onset 0.2 z = 0.1 P [MeV fm -3 ] 10 2 Flow constraint DBHf - Bonn A R [km] Large Mass ( 2 M ) and radius (R 12 km) stiff EoS; But: DBHF has DU onset in typical mass regon! 10 1 Danielewicz et al., Science (2002) n [fm -3 ] Flow in Heavy-Ion Collisions not too stiff EoS! But: DBHF violates at high densities Klähn, D.B., Sandin, Fuchs, Faessler, Grigorian, Roepke, Truemper, [arxiv:nucl-th/ ] (2006)

12 C NU N O R T LO Introduction Hadronic Cooling Quark Substructure and Phases Hybrid Star Cooling Summary

13 Ch ira l Qu ark Mo del CL NU N O OTR Field Theo ry Introduction Hadronic Cooling Quark Substructure and Phases Hybrid Star Cooling Summary

14 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling 5. Summary Partition function for chiral Quark Field theory { β Z[T, V, µ] = D ψdψ exp dτ V d 3 x[ ψ(iγ µ µ m γ 0 µ)ψ L int ] Current-current coupling (4-fermion interaction) L int = M=π,σ,... G M( ψγ M ψ) 2 + D G D( ψ C Γ D ψ) 2 Bosonisation (Hubbard-Stratonovich Transformation) { Z[T, V, µ] = Dφ M D D D D exp φ 2 M 4G M M D Collective (stochastic) Fields: Mesons (φ M ) and Diquarks ( D ) Systematic Evaluation: Mean field + Fluctuations } } D G D 2 Tr lns 1 [{M M }, { D }] Mean-field Approximation: Order parameter for Phase transitions (Gap equations) Fluctuations (2. Order): Hadronic Correlations (Bound- & Scattering states) Fluctuations of higher Order: Hadron-Hadron Interaction

15 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling 5. Summary T [MeV] NQ χ 2SC =1 NQ-2SC g2sc 2SC gusc gcfl usc 200 CFL M s =175 MeV µ [MeV] Rüster et al, PRD 72 (2005) ; Blaschke et al, PRD 72 (2005) The phases are: NQ: ud = us = ds = 0; NQ-2SC: ud 0, us = ds = 0, 0 χ 2SC 1; 2SC: ud 0, us = ds = 0; usc: ud 0, us 0, ds = 0; CFL: ud 0, ds 0, us 0; Result: Gapless phases only at high T, CFL only at high chemical potential, At T MeV: mixed NQ-2SC phase, Critical point (T c,µ c )=(48 MeV, 353 MeV), Strong coupling, G D = G S, similar, no NQ-2SC mixed phase.

16 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling M [M sun ] causality constraint PSR J DBHF = 0.92, η V = 0.00 = 1.00, η V = 0.00 = 1.00, η V = 0.25 = 1.02, η V = 0.25 = 1.03, η V = RX J EXO z = 0.1 P [MeV fm -3 ] Flow constraint DBHF = 0.92, η V = 0.00 = 1.00, η V = 0.25 = 1.02, η V = 0.25 = 1.03, η V = R [km] n [fm -3 ] Large Mass ( 2 M ) and radius (R 12 km) stiff quark matter EoS; Note: DU problem of DBHF removed by deconfinement! and: CFL core Hybrids unstable! Flow in Heavy-Ion Collisions not too stiff EoS! Note: Quark matter removes violation by DBHF at high densities Klähn, D.B., Sandin, Fuchs, Faessler, Grigorian, Roepke, Truemper, [arxiv:nucl-th/ ] (2006)

17 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling I [M sun km 2 ] B PSR J A DBHF = 0.92, η V = 0.00 = 1.00, η V = 0.00 = 1.00, η V = 0.25 = 1.03, η V = 0.25 PSR J Redshift [z] DBHF = 0.92, η V = 0.00 = 1.00, η V = 0.00 = 1.00, η V = 0.25 = 1.02, η V = 0.25 = 1.03, η V = 0.25 EXO = 1.02, η V = M [M sun ] M [M sun ] Moment of Inertia objects with large masses necessary Surface redshift large values (> 0.5) troublesome for quark matter Alford et al., ApJ 629, 969 (2005); Klähn et al., nucl-th/

18 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling The energy flux per unit time l(r) through a spherical slice at distance r from the center is: l(r) = 4πr 2 k(r) (T eφ ) e 1 Φ 2M r r. The factor e Φ 1 2M r corresponds to relativistic corrections of time and distance scales. The equations for energy balance and thermal energy transport are: (le 2Φ ) = 1 N B n (ɛ νe 2Φ + c V t (T eφ )) (T e Φ ) = 1 le Φ N B k 16π 2 r 4 n where n = n(r) is the baryon number density, N B = N B (r) is the total baryon number in the sphere with radius r and N B r = 4πr2 n(1 2M r ) 1/2 F. Weber: Pulsars as Astrophys. Labs... (1999); D.B., Grigorian, Voskresensky, A& A 368 (2001) 561.

19 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Quark direct Urca (QDU) the most efficient processes d u + e + ν and u + e d + ν ɛ QDU ν α s uye 1/3 ζ QDU T9 6 erg cm 3 s 1, Compression u = n/n 0 2, strong coupling α s 1 Quark Modified Urca (QMU) and Quark Bremsstrahlung (QB) d + q u + q + e + ν and q 1 + q 2 q 1 + q 2 + ν + ν ɛ QMU ν ɛ QB ν ζ QMU T9 8 erg cm 3 s 1. Suppression due to the pairing QDU : ζ QDU exp( q /T ) QMU and QB : ζ QMU exp( 2 q /T ) for T < T crit,q 0.57 q e+ e e+ e+ ν+ ν ɛ ee ν = Ye 1/3 u 1/3 T9 8 erg cm 3 s 1, becomes important for q /T >> 1 d d u Quark PBF - ν e - u ν - e - u u BLASCHKE, GRIGORIAN, VOSKRESENSKY, ASTRON. & ASTROPHYS. 368 (2001) 561; JAIKUMAR, PRAKASH, PLB 516 (2001) 345 FLOWERS, ITOH, APJ 250 (1981) 750; SCHAAB, VOSKRESENSKY, SEDRAKIAN, WEBER, WEIGEL, A & A 321 (1997)591 YAKOVLEV, LEVENFISH, SHIBANOV, PHYS. USP. 169 (1999) 825; BAIKO, HAENSEL, ACTA PHYS. POLON. B 30 (1999) 1097 JAIKUMAR, ROBERTS, SEDRAKIAN, PRC 73 (2006) ; WANG, WANG, WU, PRC 74 (2006)

20 2. Hadronic Cooling 3. Quark Matter Phase Diagram 4. Hybrid Star Cooling 2SC phase: 1 color (blue) is unpaired (mixed superconductivity) Ansatz 2SC + X phase: X (µ) = 0 exp[α(1 µ/µ c )] Grigorian, D.B., Voskresensky, PRC 71 (2005) Model 0 [MeV] α I 1 10 II III IV 5 25 Popov, Grigorian, D.B., PRC 74 (2006) [MeV] n c [n 0 ] n 1S 0 p 1S 0 n 3P 2 q X (I) q X (II) q X (III) q X (IV) n [n 0 ] Pairing gaps for hadronic phase AV18 - Takatsuka et al. (2004) and 2SC + X phase

21 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling log 10 (T s [K]) Model I log 10 (t[yr]) 2SC + X phase, 0 = 1 MeV, α = 10 Too large mass for Vela required N Model I BSC S [cts s -1 ] Log N - Log S test fails Popov, Grigorian, D.B., PRC 74 (2006)

22 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling 100 log 10 (T s [K]) Model IV log 10 (t[yr]) 2SC + X phase, 0 = 5 MeV, α = 25 Temperature-age and Vela mass OK N BSC 10 1 Model IV S [cts s -1 ] Log N - Log S test passed Popov, Grigorian, D.B., PRC 74 (2006)

23 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Hybrid star cooling passes all modern tests: Temperature - age Log N - Log S Brightness constraint Vela mass (Population sysnthesis) Popov, Grigorian, D.B., PRC 74 (2006) D.B., H. Grigorian, PPNP (2007) Model I Model II Model III Model IV Popov et al. (2006) M [M sun ]

24 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Ansatz Color-spin-locking (CSL) gap: ˆ = (γ 3 λ 2 + γ 1 λ 7 + γ 2 λ 5 ) Aguilera et al., PRD 72 (2005) ; PRD 74 (2006) E i [MeV] i = 1 i = 3 i = 5 M = 330 MeV p [MeV] M = 400 MeV p [MeV] Phases of superfluid 3 He

25 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling ε ν /ε µ q = 400 MeV µ q = 425 MeV µ q = 450 MeV µ q = 475 MeV µ q = 500 MeV T/T c Color-spin-locking (iso-csl) gap: ˆ = (γ 3 λ 2 + γ 1 λ 7 + γ 2 λ 5 ) Aguilera et al., PRD 72 (2005) ; PRD 74 (2006) E i [MeV] i = 1 i = 3 i = 5 M = 330 MeV M = 400 MeV Neutrino Emissivity Berdermann, Ph.D. Thesis (Rostock, 2007) D.B., Berdermann, [hep-ph] p [MeV] p [MeV] Schmitt, Shovkovy, Wang, PRD 73 (2006)

26 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling Stable stars NQ g2sc 2SC Twins gusc usc gcfl NQ g2sc 2SC Stable stars gdsc gusc gcfl T [MeV] χsb s/n B =3 Twins CFL µ [MeV] 3.0 T [MeV] s/n B = CFL µ [MeV] Phase diagrams of charge neutral quark matter in β-equilibrium at strong coupling, η = 1.0, for fixed values of the electron neutrino chemical potential, µ ν = 0 (left-hand side) and µ ν = 200 MeV (right-hand side). F. Sandin, D.B., [arxiv:astro-ph/ ] PRD (2007) χsb

27 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling M G [M sun ] =1.02 DBHF, Y le =0.4 DBHF, Y le =0 DBHF+NJL, Y le =0.4 DBHF+NJL, Y le = n c [fm -3 ] Neutrinos trapped Neutrinos untrapped Neutrinos trapped Neutrinos untrapped M B [M sun ] M G [M sun ] M G [M sun ] The effect of neutrino untrapping (Y le = 0.4 0) on hybrid star configurations. The release of gravitational binding energy amounts to 0.04 M. Blue rectangle in lower right is the constraint by Podsiadlowski et al., MNRAS (2005) F. Sandin, D.B., T. Klähn, in preparation (2007)

28 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling =0.92 η V =0.0 T [MeV] NM (DD-F4) 2SC = 1.03 η V = 0.25 = η V = 0.00 = 0.75 η V = 0.00 CFL T [MeV] 50 NM (DDF4) 2SC CFL n B [fm -3 ] n B [fm -3 ] Phase diagrams for isospin-symmetric matter, for hybrid star maximum mass M max = 2.1 M (left-hand side) and M max = 1.7 M (right-hand side). D.B.,F. Sandin, T. Klähn, Proc. CPOD Conference (2007), in preparation.

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30 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling 5. Summary 10 2 Supernova evolution in the phase diagram temperature T [MeV] 10 1 Nuclear matter 2SC density ρ [g cm -3 ]

31 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling 5. Summary 10 2 Supernova evolution in the phase diagram temperature T [MeV] 10 1 Nuclear matter 15 M sun (Harald Dimmelmeier) 2SC density ρ [g cm -3 ]

32 2. Hadronic Cooling + Structure 3. Quark Substructure + Phases 4. Hybrid Star Structure + Cooling 5. Summary 10 2 Supernova evolution in the phase diagram 40 M sun (Tobias Fischer) temperature T [MeV] 10 1 Nuclear matter 15 M sun (Harald Dimmelmeier) density ρ [g cm -3 ]

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34 Discovery: Sept. 18, 2006 in NGC 1260 (Perseus) Distance: 72 Mpc=238 Mill. Ly (Smith et al.: astro-ph/ ) Light curve: 70 days rise time Energy release: erg= 10 bethe Progenitor star: 150 M? Engine: Quark-star formation? (Leahy & Ouyed: [astro-ph])

35 Supernova 1987A - 20 years later: Big mystery of rings! Double degenerate core in common envelope? 2.14 ms periodic signal Explanation for 99% of GRB? Middleditch, [astro-ph] CAMK Warsaw,

36 What has happened here?? Supernova 1987A - 20 years later: Big mystery of rings! Double degenerate core in common envelope? 2.14 ms periodic signal Explanation for 99% of GRB? Middleditch, [astro-ph] CAMK Warsaw,

37 1. Astrophysik kompakter Sterne 2. Quantenfeldtheorie dichter Materie 3. Quarkmaterie in Neutronensternen 4. Ausblick: Astro-Hadron Physik Exploration of the Hadron-Quark Phase transition: Relativistic Heavy ion collisions Nuclotron (NICA start 2013) NUKLOTRON 3 Baryon Density n [0.16 fm ] Mixed Phase: Quark - Hadron coexistence Precursor effects of the chiral phase transition?

38 1. Astrophysik kompakter Sterne 2. Quantenfeldtheorie dichter Materie 3. Quarkmaterie in Neutronensternen 4. Ausblick: Astro-Hadron Physik Exploration of the Hadron-Quark phase transition: Relativistic heavy ion collisions FAIR SIS300 (after 2014) 3 Baryon Density n [0.16 fm ] Is there a critical point? Signals of Chiral Symmetry (massless quarks)? Effects of Color Superconductivity (pseudogapphase)?

39 1. Astrophysik kompakter Sterne 2. Quantenfeldtheorie dichter Materie 3. Quarkmaterie in Neutronensternen 4. Ausblick: Astro-Hadron Physik Optical and Radio telescopes: Neutron stars (since at least 10 8 years) Arecibo (Puerto Rico): 305 m

40 1. Astrophysik kompakter Sterne 2. Quantenfeldtheorie dichter Materie 3. Quarkmaterie in Neutronensternen 4. Ausblick: Astro-Hadron Physik Optical and Radio telescopes: Neutron stars (since at least 10 8 years) Very Large Array (Socorro, NM): 27m x 25m

41 1. Astrophysik kompakter Sterne 2. Quantenfeldtheorie dichter Materie 3. Quarkmaterie in Neutronensternen 4. Ausblick: Astro-Hadron Physik X-ray satellites: Neutron stars (since at least 10 8 years) Chandra (since 1999):

42 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling 5. Summary THEORY OF EOS WITH CONSTRAINTS Nuclear Matter - Quark Matter Phase transition depends on details of the modeling, e.g. Coupling Constants, Form Factors Improve by using DSE Models Phase transition weakly first order, Masquerade effect Stable Neutron Stars with 2-Flavor Quark Matter Core possible EXPERIMENTAL OBSERVABLES Observation of Compact Star Configurations: Very massive stars (M > 2M ) require stiff EoS Large compact stars (R > 12 km) require stiff EoS Mass clustering in double neutron stars: observation of the quark matter onset? Cooling Evolution: Hadronic DU process should not occur: sensitive star mass dependence! Quark matter core all quarks gapped, min 30 kev, 2SC+X oder CSL phase? CFL phase unlikely, critical density (and gaps) too large, gcfl only at T > 50 MeV OUTLOOK Include hadronic fluctuations (bound and scattering states) at finite density: Quark Exchange (Pauli Blocking)

43 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Wroclaw

44 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Wroclaw Complex Physics of Compact Stars, Karpacz, February karp44

45 2. Hadronic Cooling 3. Quark Substructure and Phases 4. Hybrid Star Cooling Wroclaw Complex Physics of Compact Stars, Karpacz, February karp44