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Blazars & GRBs

Blazars & GRBs. The fastest macroscopic objects of the Universe. Gabriele Ghisellini INAF-Osservatorio di Brera. G. < b app >~10  < G > > 10. Lister+ 2013. Fermi FSRQs. G. Earlier on: isotropic explosion. Later: energy crisis + collapsar scenario. G. G. G.

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Blazars & GRBs

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  1. Blazars & GRBs The fastest macroscopic objects of the Universe Gabriele Ghisellini INAF-Osservatorio di Brera

  2. G

  3. <bapp>~10  <G> > 10 Lister+ 2013 Fermi FSRQs G

  4. Earlier on: isotropic explosion

  5. Later: energy crisis + collapsar scenario G G G

  6. Blazars: collimation 1/G 1/G G G qjet G GRBs: collimation qjet G

  7. Blazars: collimation 1/G 1/G G G qjet G GRBs: collimation qjet G

  8. L ~ L’ G4 Blazars 1/G G G qjet G GRBs G L ~ L’ (G/qjet)2

  9. G=constt2 0 Molinari+ 2007

  10. G decreasing t-a 0 Molinari+ 2007

  11. 1/8 tpeak Ek,iso G ~ 3 n tpeak 0 Molinari+ 2007

  12. Ghirlanda+ 2012 Liang+ 2012

  13. Blazars: the general picture

  14. L>0.01LEdd Within RBLR UBLR= const Within RTorusUIR= const Big blazars RTorus Torus ~1-10 pc G RBLR disk Broad Line Region ~0.2 pc

  15. L<0.01LEdd SSC only weak cooling BL Lacs G BLR <<0.2 pc “ADAF disk”

  16. FSRQs: emission lines many seed photons BL Lacs: no or weak lines G G Rdiss

  17. FSRQs BL Lacs G G Rdiss FSRQs BL Lacs BL Lacs FSRQs

  18. FSRQs FSRQs BL Lacs BL Lacs G G BL Lacs FSRQs

  19. Blazars and GRBs: same efficiency

  20. Collimation corrected GRBs blazars Nemmen+ Science 2012 Collimation corrected

  21. GRBs Fermi blazars, one p per e-

  22. Jet launching Internal pressure or magnetic field?

  23. Jet opacity: blazars tT,0 = sTno R tT,0 ~ 0.5 no from Mout  Jet opacity: GRBs 3/4 Pjet,51 1 Pjet aT04 tT,0 ~ 1015 ~ n+  1/2 G1 LEdd M1 kT0

  24. Jet launching In GRBs we have 2 possibilities: - internal pressure: the huge optical depth traps photons inside - magnetic field In blazars: - internal pressure: the optical depth is small - magnetic field

  25. Jet launching In GRBs we have 2 possibilities: - internal pressure: the huge optical depth traps photons inside - magnetic field In blazars: - internal pressure: the optical depth is small - magnetic field Magnetic field: - Produced and amplified by the disk - Link with accretion

  26. Blandford & Znajek UB ~ rc2 @ Rs This explains why Pj ~ Ld B ~ 1015-1016 G in GRBs B ~ 104 G in blazars B ~ 109 G in galactic superluminals And yet: - Jets are not magnetically dominated in the emission region -very rapid PBPkin - the “right” amount of matter to have ~same G for all jets

  27. EC Small B synchro torus disk X-ray corona

  28. Fermi FSRQs Power in cold protons (1 per emitting e-) Power in rel. electrons Power in Poynting flux Power in radiation (model indipendent) Disk luminosity

  29. Mout/Min for blazars and for GRBs Pjet = GMoutc2 Ld = hMinc2 for blazars:

  30. Mout/Min for blazars and for GRBs Pjet = GMoutc2 blazars Ld = hMinc2 for blazars: h Pjet Min Mout ~ 10-2 = G Ld

  31. Mout/Min for blazars and for GRBs Pjet = GMoutc2 blazars Ld = hMinc2 for blazars: h Pjet Min Min Mout Mout ~ 10-2 = = G Ld for GRBs: 0.1 MO Min ~ tburst Ek52 Ek ~ 5.5x10-4 G2 G c20.1 MO

  32. Blazars and GRBs: a difference

  33. Blazars: the redder the more powerful  cooling “Ghirlanda” Epeak [keV] “Amati” GRBs: the bluer the more powerful  heating?? G? E[erg]

  34. Conclusions Jets are the most efficient engine of Nature Compare jet power and Ldisk as a function of the accretion rate. Normalize to Eddington.

  35. Late prompt in GRBs? 1644+57?

  36. GBRs blazars

  37. The“blazarsequence” FSRQs Fossati et al. 1998; Donato et al. 2001 BL Lacs BAT Integral

  38. FSRQs Line strength Fossati et al. 1998; Donato et al. 2001 BL Lacs

  39. FSRQs Next talk by Meyer M/MEdd Fossati et al. 1998; Donato et al. 2001 BL Lacs

  40. Narayan & Yi 1995: LBLR/LEdd ~ 10-3 Sharma+ 2007: LBLR/LEdd ~ 10-5 SDSS+1LAC EW>5A 5x10-4 Sbarrato+ 2011 EW<5A M-s;Plotkin+ 2011 Do we really need to divide blazars?

  41. Black hole masses (for FSRQs)

  42. MBH=2x109 Fermi EC G synchro UVOT XRT GG, Tavecchio & Ghirlanda 2009 torus X-ray corona disk SSC Low energy synchro peak: leave the disk naked!

  43. MBH=1010 BAT

  44. The jet cannot have less power than what required to produce the observed luminosity: Lobs Pjet > G2 If Pjet is twice as much, G halves. We can take that as the minimum Pjet. This limit is model-independent.

  45. GG/2 Pj.min = 2Lobs/G2

  46. 1 proton per electron  no pairs Having pairs would reduce Pjet. But where are they created?

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