Gamma-Ray-Bursts in Nuclear Astrophysics

1. Gamma-Ray-Bursts in Nuclear Astrophysics Giuseppe Pagliara Dip. Fisica Politecnico di Torino INFN-Ferrara XI Convegno su Problemi di Fisica Nucleare Teorica - Cortona 2006

2. General features of GRBs • Duration 0.01-1000s • ~ 1 burst per day (BATSE) • Isotropic distribution - rate of ~2 Gpc-3 yr-1 • ~100keV photons • Cosmological Origin • The brightness of a GRB, E~1051ergs (beaming effect), is comparable to the brightness of the rest of the Universe combined. Very complex time-structure

3. “Two kinds of precursors” Prompt-emission precursor, few hundred of seconds SN-GRB connection, time delays from second to years

4. Rotating massive stars, whose central region collapses to a black hole surrounded by an accretion disk. Outflows are collimated by passing through the stellar mantle. Detailed numerical analysis of jet formation. Fits naturally in a general scheme describing collapse of massive stars. - Large angular momentum needed, difficult to achieve. SN – GRB time delay: less then 100 s. Can it explain long time delay precursors ? The Collapsar model

5. The Quark-Deconfinement Nova model

6. Delayed formation of quark matter in Compact Stars Droplet potential energy: Quark matter cannot appear before the PNS has deleptonized (Pons et al 2001) Quantum nucleation theory nQ* baryonic number density in the Q*-phase at a fixed pressure P. μQ*,μHchemical potentials at a fixed pressure P. σ surface tension (=10,30 MeV/fm2) I.M. Lifshitz and Y. Kagan, Sov. Phys. JETP 35 (1972) 206 K. Iida and K. Sato, Phys. Rev. C58 (1998) 2538

7. Quark droplet nucleation time“mass filtering” Critical mass for s= 0 B1/4 = 170 MeV Critical mass for s = 30 MeV/fm2 B1/4 = 170 MeV Age of the Universe! Mass accretion

8. Two families of CSs Conversion from HS to HyS (QS) with the same MB

9. How to generate GRBs The energy released (in the strong deflagration see Parenti talk) is carried out by neutrinos and antineutrinos. The reaction that generates gamma-ray is: The efficency of this reaction in a strong gravitational field is: [J. D. Salmonson and J. R. Wilson, ApJ 545 (1999) 859]

10. Hadronic Stars  Hybrid or Quark StarsZ.Berezhiani, I.Bombaci, A.D., F.Frontera, A.Lavagno, ApJ586(2003)1250 Drago, Lavagno Pagliara 2004, Bombaci Parenti Vidana 2004… Metastability due to delayed production of Quark Matter . 1) conversion to Quark Matter (it is NOT a detonation (see Parenti )) 2) cooling (neutrino emission) 3) neutrino – antineutrino annihilation 4)(possible) beaming due to strong magnetic field and star rotation + Fits naturally into a scheme describing QM production. Energy and duration of the GRB are OK. - No calculation of beam formation, yet. SN – GRB time delay: minutes  years depending on mass accretion rate

11. … back to the data Temporal structure of GRBs ANALYSIS of the distribution of peaks intervals

12. Excluding QTs Deviation from lognorm & power law tail (slope = -1.2) Probability to find more than 2 QT in the same burst Drago & Pagliara 2005 Analysis on 36 bursts having long QT (red dots): the subsample is not anomalous

13. Analysis of PreQE and PostQE Same “variability”: the same emission mechanism, internal shocks

14. Same dispersions but different average duration PreQE: 20s PostQE:~40s QTs:~ 80s Three characterisitc time scales No evidence of a continuous time dilation

15. Huge energy requirements No explanation for the different time scales It is likely for short QT Interpretation: 1)Wind modulation model: during QTs no collisions between the emitted shells 2) Dormant inner engine during the long QTs Reduced energy emission Possible explanation of the different time scales in the Quark deconfinement model It is likely for long QT

16. Quiescent times in very long GRBs High red-shift

17. … back to the theory In the first version of the Quark deconfinement model only the MIT bag EOS was considered …but in the last 8 years, the study of the QCD phase diagram revealed the possible existence of Color Superconductivity at “small” temperature and large density

18. More refined calculations CFL cannot appear until the star has deleptonized Ruster et al hep-ph/0509073 Two first order phase transitions: Hadronic matter Unpaired Quark Matter(2SC) CFL

19. Double GRBs generated by double phase transitions • Two steps (same barionic mass): • transition from hadronic matter to unpaired or 2SC quark matter. “Mass filtering” • 2) The mass of the star is now fixed. After strangeness production, transition from 2SC to CFL quark matter. Decay time scale τ few tens of second Nucleation time of CFL phase

20. Energy released Drago, Lavagno, Pagliara 2004 Bombaci, Lugones, Vidana 2006 Energy of the second transition larger than the first transition due to the large CFL gap (100 MeV)

21. … a very recent M-R analysis Color superconductivity (and other effects ) must be included in the quark EOSs !!

22. Are LGRBs signals of the successive reassesments of Compact stars? Low density: Hyperons - Kaon condensates…

23. Conclusions • A “standard model” the Collapsar model • One of the alternative model: the quark deconfinement model • Possibility to connect GRBs and the properties of strongly interacting matter! Collaborators: Alessandro Drago, Università Ferrara Andrea Lavagno, Dip. Fisica Politecnico di Torino

24. APPENDICI

25. Other possible signatures Origin of power law: SOLAR FLARES The initial masses of the compact stars are distributed near Mcrit, different central desity and nucleation times  of the CFL phase f((M)) For a single Poisson process Variable rates Could explain the power law tail of long QTs ? Power law distribution for Solar flares waiting times (Wheatland APJ 2000)

26. Probability of tunneling