deconfinement in compact stars jinr夸克禁闭解除致密星联合核研究所课件

Quark deconfinement in compact stars: Irene ParentiIrene Parenti Univ. of FerraraUniv. of Ferrara Italy Italy connection connection withwith GRBsGRBs InternationalInternational summersummer schoolschool: : “Hot points in “Hot points in AstrophysicsAstrophysics and and CosmologyCosmology” ” DubnaDubna, Russia, Russia 2 13 August 20042 13 August 2004 August 2004Irene Parenti INFN of FerraraINFN of Ferrara ItalyItaly Summary Short Short overviewoverview on on Gamma-RayGamma-Ray BurstsBursts ( (GRBsGRBs) ) DelayedDelayed nucleationnucleation of Quark of Quark MatterMatter HowHow toto generate generate Gamma-RayGamma-Ray BurstsBursts fromfrom deconfinementdeconfinement ConclusionsConclusions August 2004Irene Parenti ImplicationImplication forfor the mass and the mass and radiusradius of of compact compact starsstars Gamma-Ray Bursts (GRBs) Spatial distribution:Spatial distribution: isotropicisotropic Distance:Distance: cosmological (1-10)10cosmological (1-10)10 9 9 lyly Energy range:Energy range: 100 100 KeVKeV a few a few MeVMeV Emitted energy:Emitted energy: 101051 51 erg (beamed/jets) erg (beamed/jets) Duration:Duration: (0,01-300) s(0,01-300) s short short GRBsGRBs few ms 2 sfew ms 2 s long long GRBsGRBs 2 s few 100 s2 s few 100 s J.S.J.S. BloomBloom, , D.A.D.A. FrailFrail, S.R. , S.R. KulkarniKulkarni, , ApJApJ 594, 2003 594, 2003 August 2004Irene Parenti GRB and supernovae Connection between GRB and SupernovaeConnection between GRB and Supernovae EvidenceEvidence forfor atomicatomic lineslines in the in the spectraspectra of the of the X-rayX-ray afterglowafterglow time time delaydelay t between the Supernova t between the Supernova explosion and the Gamma-Ray Burst.explosion and the Gamma-Ray Burst. August 2004Irene Parenti Time delay from SN to GRB GRBGRB 990705990705 T 10 yr T 10 yr AmatiAmati et al., Science 290, 2000, 953 et al., Science 290, 2000, 953 GRBGRB 011211011211 T 4 daysT 4 days Watson et al., Watson et al., ApJApJ 595, 2003, L29 595, 2003, L29 GRBGRB 030227030227 T 3-80 daysT 3-80 days Reeves Reeves etaletal. , Nature 2002. , Nature 2002 August 2004Irene Parenti A two-stages scenario 1 1 stst explosion: explosion: SUPERNOVASUPERNOVA (birth of a NS)(birth of a NS) 2 2 ndnd “explosion”: “explosion”: CENTRAL ENGINECENTRAL ENGINE OF THE GRBOF THE GRB (ass. with the NS) (ass. with the NS) What is the origin of the 2What is the origin of the 2nd nd “explosion”? “explosion”? How to explain the long time delay How to explain the long time delay between the two events?between the two events? open open questionsquestions August 2004Irene Parenti A. A. DragoDrago, A. , A. LavagnoLavagno and G. and G. PagliaraPagliara PhysPhys. . Rev.Rev. D69 (2004) 057505 D69 (2004) 057505 when color superconductivity is taken in to account:when color superconductivity is taken in to account: The conversion process can be delayed due to the effects The conversion process can be delayed due to the effects of the surface tension between the HM phase and the QM of the surface tension between the HM phase and the QM phase. phase. The nucleation time depends The nucleation time depends drammaticallydrammatically on the central on the central pressure of the HS. pressure of the HS. As a critical-size drop of QM is formed the HS is As a critical-size drop of QM is formed the HS is converted to a QS or a converted to a QS or a HySHyS. . The conversion process releases: The conversion process releases: E Econv conv. . 10 1052 52 - 10 - 1053 53 erg erg Delayed collapse of a HS to a QS Z. Z. BerezhianiBerezhiani, I. , I. BombaciBombaci, A. , A. DragoDrago, F. , F. FronteraFrontera and and A. A. LavagnoLavagno ApJApJ. 586 (2003) 1250. 586 (2003) 1250 Pure HS Pure HS Hybrid Star or Quark StarHybrid Star or Quark Star Possible central Possible central engine for GRBengine for GRB August 2004Irene Parenti The Quark-Deconfinement Nova model August 2004Irene Parenti Finite-size effects The formation of a critical-size drop of QM is The formation of a critical-size drop of QM is not immediate. not immediate. Its necessary to have an Its necessary to have an overpressure overpressure to form a to form a droplet having a size large enough to overcome thedroplet having a size large enough to overcome the effect of the surface tension.effect of the surface tension. A virtual droplet moves back and forth in the A virtual droplet moves back and forth in the potential energy well on a time scale:potential energy well on a time scale: 0 0 -1-110 10-23 -23 s s weak weak quark-flavor must be conservedquark-flavor must be conserved during the during the deconfinementdeconfinement transition.transition. August 2004Irene Parenti virtual droplet ofvirtual droplet of deconfineddeconfined quark quark mattermatter stable phasestable phase when p overcomes the when p overcomes the transition pointtransition point Quark deconfinement hadronichadronic matter in a matter in a metastablemetastable state state in a time in a time real droplet of real droplet of deconfineddeconfined quark quark mattermatter This form of This form of deconfineddeconfined matter has the same matter has the same flavor content of the flavor content of the -stable -stable hadronichadronic system system at the same pressure.at the same pressure. We call it: We call it: Q*-phaseQ*-phase. . Soon afterwards the weak interactions change the Soon afterwards the weak interactions change the quark flavor fraction to lower the energy.quark flavor fraction to lower the energy. The drop grows with no The drop grows with no limitation.limitation. real droplet of real droplet of strange matterstrange matter August 2004Irene Parenti Equation of State HadronicHadronic phasephase: : RelativisticRelativistic MeanMean FieldField TheoryTheory of of hadronshadrons interactinginteracting via via mesonmeson exchexch. . e.g. e.g. GlendenningGlendenning, , MoszkowskyMoszkowsky, PRL 67(1991), PRL 67(1991) Quark Quark phasephase: : EOS based on the MIT bag model EOS based on the MIT bag model for hadronsfor hadrons. . Farhi, Jaffe, Phys. Rev. D46(1992)Farhi, Jaffe, Phys. Rev. D46(1992) MixedMixed phasephase: : Gibbs construction for a Gibbs construction for a multicommulticom- - ponentponent system with two conserved “charges”. system with two conserved “charges”. GlendenningGlendenning, , PhysPhys. . Rev.Rev. D46 (1992) D46 (1992) August 2004Irene Parenti Hybrid star: mass-radius B=136,36 B=136,36 MeVMeV/fm/fm 3 3 Hybrid Star: configuration B=136,36 B=136,36 MeVMeV/fm/fm 3 3 Strange Star: mass-radius B=74,16 B=74,16 MeVMeV/fm/fm 3 3 Strange Star: configuration B=74,16 B=74,16 MeVMeV/fm/fm 3 3 Quantum nucleation theory I.M. I.M. LifshitzLifshitz and Y. and Y. KaganKagan, , SovSov. Phys. JETP 35 (1972) 206. Phys. JETP 35 (1972) 206 K. Iida and K. Sato, Phys. Rev. C58 (1998) 2538K. Iida and K. Sato, Phys. Rev. C58 (1998) 2538 Droplet potential energy:Droplet potential energy: n n QQ* * baryonic number density baryonic number density in the Q*-phase at a in the Q*-phase at a fixed pressure P. fixed pressure P. Q*Q* , , HH chemical potentials chemical potentials at a fixed pressure P. at a fixed pressure P. surface tension surface tension (=10,30 MeV/fm (=10,30 MeV/fm 2 2 ) ) August 2004Irene Parenti Matter in the droplet FlavorFlavor fractionsfractions are the are the samesame of of the the -stable-stable hadronic system at thehadronic system at the same pressure:same pressure: The The pressurepressure neededneeded forfor phasephase transitiontransition isis muchmuch largerlarger thanthan thatthat withoutwithout flavorflavor conservationconservation. . August 2004Irene Parenti Nucleation time The The nucleation timenucleation time is the time needed to form is the time needed to form a critical droplet of a critical droplet of deconfineddeconfined quark matter. quark matter. It can be calculated for different values of the It can be calculated for different values of the stellar central pressure (and then of the stellar stellar central pressure (and then of the stellar mass, as implied by TOV).mass, as implied by TOV). August 2004Irene Parenti The nucleation time dramatically depends The nucleation time dramatically depends on the value of the stellar central pressure on the value of the stellar central pressure and then on the value of the stellar mass.and then on the value of the stellar mass. The critical mass of metastable HS We fixed the time of nucleation at 1 yr.We fixed the time of nucleation at 1 yr. The gravitational mass corresponding toThe gravitational mass corresponding to this nucleation time is called this nucleation time is called critical masscritical mass: : MMHS HS MMcr cr This HS are very unlikely This HS are very unlikely to to be observed.be observed. We assume that during the stellar conversion process We assume that during the stellar conversion process the total numbers of baryons in the star (and then the the total numbers of baryons in the star (and then the baryonic mass) is conserved.baryonic mass) is conserved. I. I. BombaciBombaci and B. and B. DattaDatta, , ApJApJ. 530 (2000) L69. 530 (2000) L69 The gravitational mass of the final star The gravitational mass of the final star is taken to be the mass in the stable is taken to be the mass in the stable configuconfigu- - ration corresponding to that baryonic mass.ration corresponding to that baryonic mass. August 2004Irene Parenti Two families of compact stars August 2004Irene Parenti Mass-Radius constraints X-rayX-ray bursterburster EXOEXO676 CottamCottam etet al., Nature 420, 2002 al., Nature 420, 2002 z=0z=0.35.35 X-rayX-ray pulsar pulsar 1E 1207.4-52091E 1207.4-5209 SanwalSanwal etet al.al. ApJApJ 574, 2002, L61 574, 2002, L61 z=0z=0.12-0.23.12-0.23 X-rayX-ray binarybinary 4U 1728-344U 1728-34 Li et Li et al.al. ApJApJ 527,1999,L51 527,1999,L51 VeryVery compact compact objectobject Mass-Radius constraints Energy released The total energy released in the stellar conversionThe total energy released in the stellar conversion is given by the difference between the gravitational is given by the difference between the gravitational mass of the initial mass of the initial hadronichadronic star (M star (Min in= =M Mcr cr) and the ) and the mass of the final hybrid or strange stellar mass of the final hybrid or strange stellar configuration (configuration (MMfin fin= =M MQS QS(M (M b b crcr): ): August 2004Irene Parenti The The reactionreaction thatthat generate generate gamma-raygamma-ray isis: : The The efficenceefficence of of thisthis reactionreaction in a strong in a strong gravitationalgravitational field is: field is: J. D. Salmonson and J. R. Wilson, J. D. Salmonson and J. R. Wilson, ApJApJ 545 (1999) 859 545 (1999) 859 How to generate GRBs The The energyenergy releasedreleased isis carriedcarried out out byby pairspairs of of neutrinosneutrinos antineutrinos. antineutrinos. August 2004Irene Parenti Conclusions Neutron stars (HS) are Neutron stars (HS) are metastablemetastable to to HS QS or to HS HS QS or to HS HySHyS E E convconv 10 1052 52 10 1