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

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Lister ~10  > 10 Fermi FSRQs 

Earlier on: isotropic explosion

   Later: energy crisis + collapsar scenario

      jet Blazars: collimation 1/  GRBs: collimation GRBs: collimation  jet

      jet Blazars: collimation 1/  GRBs: collimation GRBs: collimation  jet

      jet L ~ L’  4 L ~ L’ (  jet ) 2 Blazars GRBs

0 Molinari+ 2007

0

0  E k,iso n t peak 3 1/8 t peak

Ghirlanda Liang+ 2012

Blazars: the general picture

Torus ~1-10 pc Broad Line Region ~0.2 pc Within R BLR U BLR = const Within R Torus U IR = const  R BLR R Torus disk Big blazars L>0.01L Edd

BLR <<0.2 pc weak cooling SSC only “ADAF disk”  L<0.01L Edd BL Lacs

  R diss FSRQs: emission lines  many seed photons BL Lacs: no or weak lines

FSRQs BL Lacs  FSRQs  R diss FSRQs BL Lacs

  FSRQs FSRQsFSRQs

Blazars and GRBs: same efficiency

Collimation corrected Nemmen+ Science 2012 blazars GRBs

Fermi blazars, one p per e- GRBs

Jet launching Internal pressure or magnetic field? or magnetic field?

     n o R Jet opacity: blazars n o from M out     ~ P jet 1 P jet  1 L Edd Jet opacity: GRBs aT 0 4 kT 0 ~ n +     ~ P jet,51 M1M1M1M /23/4

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

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

Blandford & Znajek  U B ~  c R s This explains why P j ~ L d B ~ G in GRBs B ~ 10 4 G in blazars B ~ 10 9 G in galactic superluminals

synchro EC Small B torusdisk X-ray corona

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

M out /M in for blazars and for GRBs P jet =  M out c 2 L d =  M in c 2 for blazars:

M out /M in for blazars and for GRBs P jet =  M out c 2 L d =  M in c 2 for blazars:  P jet LdLdLdLd M out M in = ~ blazars

M out /M in for blazars and for GRBs P jet =  M out c 2 L d =  M in c 2 for blazars: for GRBs: M in ~ 0.1 M O t burst  P jet LdLdLdLd M out M in = M out M in =  c M O EkEkEkEk ~ 5.5x10 -4 2222 E k52 ~ blazars

Blazars and GRBs: a difference

Blazars: the redder the more powerful  cooling GRBs: the bluer the more powerful  heating??  ? “Amati” “Ghirlanda” E peak [keV] E [erg]

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

? Late prompt in GRBs?

blazars GBRs

Fossati et al. 1998; Donato et al The “blazar sequence” FSRQs BL Lacs BATIntegral

FSRQs Line strength Fossati et al. 1998; Donato et al. 2001

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

Sbarrato SDSS+1LAC Do we really need to divide blazars? 5x10 -4 EW<5A EW>5A Narayan & Yi 1995: L BLR /L Edd ~ Sharma+ 2007: L BLR /L Edd ~ M-  Plotkin+ 2011

Black hole masses (for FSRQs)

UVOT XRT Fermi GG, Tavecchio & Ghirlanda 2009 Low energy synchro peak: leave the disk naked! torus disk X-ray corona synchro SSC EC  M BH =2x10 9

BAT M BH =10 10

The jet cannot have less power than what required to produce the observed luminosity: P jet L obs 2222 > If P jet is twice as much,  halves. We can take that as the minimum P jet. This limit is model-independent.

  

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

Pause P jet ~ Mc 2, even larger than L dP jet ~ Mc 2, even larger than L d For all M/M EddFor all M/M Edd BL Lacs  ADAF FSRQs  SSBL Lacs  ADAF FSRQs  SS L BLR /L Edd divides BL Lacs from FSRQsL BLR /L Edd divides BL Lacs from FSRQs Matter, not magnetic, dominatedMatter, not magnetic, dominated

 P r = radiation ~ L obs /  2 P e = relat. electrons P p = protons P B = B-field R jet power and accretion luminosity ~10 17 cm Shakura-Sunjaev disk: L d P jet = P e +P p +P B

What is a blazar? A jetted AGN, whose jet is relativistic (  ~10) and is “pointing at us”. A jetted AGN, whose jet is relativistic (  ~10) and is “pointing at us”. To be more quantitative: To be more quantitative:  view   For each blazar, 2  2 radio-loud AGN pointing elsewhere: FR I and FRII radio- galaxies

3 months, 10  BL Lacs Flat Steep FSRQs LLLL Fossati et al. 1998; Donato et al. 2001

M/ M Edd GG, Maraschi, Tavecchio years– 4  Ackermann+ 2011

Molinari+ 2007

Isotropic Collimation corrected