1. Hadronic cascades in GRBs and AGNs Katsuaki Asano (Tokyo Tech.) Collaboration with S.Inoue, P.Meszaros M.Kino

2. GRB Standard Picture Internal Shock External Shock ISM

3. GRB 090510 Short GRB Precursor Delay z=0.903 E iso =10 53 erg 8keV-260keV 260keV-5MeV >100MeV >1GeV 31GeV, 3.4GeV

4. GRB 090510; Spectra Band+ Extra PL

5. GRB 090902B E iso =4x10 54 erg @ z=1.822 Abdo et al. ApJ 706, L138

6. Extra Component in 090902B

7. Extra Component=Afterglow? GRB 090510 2009

8. Monte-Carlo Method R ΔR=R/Γ 2 Photons: Luminosity L Power-law injection of protons Energy density of photons U γ Energy density of magnetic field U B =f B U γ Energy density of Accelerated protons U p =f p U γ

9. Method t ………. dt Emission (Synch. IC) pγ Yes or No? Yes -> π + or π 0 Proton Neutron Proton π + π - π 0

10. Cross Sections n +  processes also Inelasticity

11. Iterative Method To estimate pγ, Inv.Comp., γγ processes, we need a photon field. During the dynamical timescale, the photon field is assumed to be steady. Photon Field By hand Calculation Photon Field Result Calculation Photon Field Result …

12. Cascade Processes ｐ＋ γ→n+π ＋ π＋→μ＋ +νμπ＋→μ＋ +νμ μ ＋ →e ＋ + ν μ + ν e ｐ＋ γ→p+π 0 π 0 →γ + γ ｐ＋ γ→p + e - + e + γ ＋ γ→e - + e + Synchrotron + Inv.Comp.: p, π ±,μ ±,e ± →γ Synchrotron Self-absorption: γ ＋ e → e Iterative Method -> Both photon field and cascade processes are solved consistently.

13. Highest Energy The Larmor radius R L =e E p /B < shell width Δ=R/Γ. The acceleration time ξR L /c < cooling time. The energy of particles is limited by two conditons. Cooling Processes: Proton Synchrotron+IC Photoproduction of pions Bethe-Heitler

14. Proton acceleration efficiency We need 6-8 10 43 ergs/Mpc 3 /yr to explain UHECRs See e.g. Murase, Ioka, Nagataki, Nakamura 2008 We may need Up/Uγ>20. If GRB rate is 0.05 Gpc -3 /yr, Up/Uγ>100

15. Proton Dominated? Energy Gamma keV Proton E -2.0 PeV-EeV E 2 n(E) To make gamma-rays from protons contribute enough, the proton energy largely exceeds the gamma-ray energy?? Efficent for pion production

16. Distortion due to proton cascade Lepton distribution E Primary Electrons Pairs from Cascade f B =1.0 e-SY Up=Uγ

17. Double break f B =1.0 e-SY

18. Double break 2

19. Much More Protons Primary Electron Components

20. Energy-dependence

21. B-dependence

22. GRB 090510; Spectra Band+ Extra PL

23. Cascade due to photopion production 3.4GeV R=10 14 cm  =1500 Synchrotron and Inverse Compton due to secondary electron-positron pairs Band component  -absorption Asano, Guiriec & Meszaros 2009

24. The maximum energy is determined by the dynamical timescale. A long cooling timescale -> low efficiency of pion- production The cooling timescales (comoving frame) of protons due to synchrotron, inverse Compton, Bethe-Heitler, and photopion production are plotted. The dynamical timescale is R/  c.

25. Proton Synchrotron R=10 14 cm Even in this case, secondary pairs contribute

26. Proton synchrotron case Synchrotron is the most efficient in this case. We suppress E max to avoid too much secondary photons. t acc =ξR L /c

27. Neutrinos from GRB 090510 We may need >10 -2 erg/cm 2 to detect with IceCube. “Bright” Neutrino

28. GRB 090902B Hadronic Model 4.6-9.6s α=-0.07, β=-3.9 Photosperic?

29. Naked Eye GRB GRB080319B Hadronic In preparation E iso ～ 10 54 erg

30. GRBs GeV Photon detection -> Γ>1000 Extra Component -> Afterglow? Hadronic? High Γ -> Lower Photon Density, Magnetic Field ->Lower Effciency for Photopion Production Hadronic Models require >10 55 erg/s for GRB 090510 Ref. E iso ～ 10 55 erg in gamma-rays for GRB080916C

31. Gamma-rays from hypernovae Soderberg et al. 2006

32. Particle Acceleration in Winds Relativistic component Γβ ～ 1, E k ～ 10 50 erg

33. Proton Cooling in Hypernova A*=5

34. Secondary Photons Muon-Decay Origin Absorbed Proton SY Origin

35. Hypernovae Secondary emission from hyeprnovae –X-ray due to cascade from muon decay –GeV emission from proton synchrotron –“Delayed” TeV emission HN Rate ～ 500 Gpc -3 yr -1

36. Compact Radio-Loud AGN CSOs (Compact symmetric objects ) Radio lobe nuclei 3C 84 ~10 pc Size < 500 pc 120 kpc FRII radio galaxies Evolution?? e.g., Carvalho et al. 1985; Fanti et al. 1995; Begelman 1996; Readhead et al. 1996, … Velocity of Hot Spot: ～ 0.1 c for ～ 20 CSOs CORALZ(COmpact RA-dio sources at Low-Redshift): 10 40 -10 42 erg/s HFPs(high frequency peakers): 10 43 -10 45 erg/s

37. Gamma-Rays from Compact Radio AGNs Core of Seyfart 2 gal. NGC 1275 (M BH =3*10 8 M sun ) z=0.0176 Other radio bubbles (Pedler+91, Vermeulen+96) Asada+06 5 pc VSOP view of 3C84 Chandra view of Perseus Cluster (Fabian) 3C84 (NGC1275) Fermi (>200MeV)

38. SSC Model

39. EGRET Fermi UMRAO Abdo+09 COS-B Long Term Evolution

40. Nagai+09, submitted Born! β app = 0.23 Lobe Generation VERA

41. Nagai+09, submitted freq. dependent? (need further studies) Lobe Velocity

42. Nagai+09, submitted Smoking-gun of “core-outburst” Wide-view (~kpc) Core (~pc) Radio Light Curve

43. Hadronic Model for Compact Radio AGNs 2pc 10pc UV: L=3x10 45 erg/s, T=10eV Disk Proton Injection L=5x10 46 erg/s Adiabatic Expansion v exp =0.1c B=0.1G

44. Spectrum UV D=100Mpc

45. Hadronic Contributions

46. SED of mini radio-lobe (t_age=t_inj) Kino & Asano in prep VLBI obs. Stars/Dusts overlapped ICM/ Hot-disk overlapped With/Without protons is distinguishable at γ domain!

47. SNR(?) Case Electron Injection has been already stopped?

48. Pure Hadronic Case