Hadronic Models for Blazars and AGN Neutrinos at Rencontres de Moriond

1. Hadronic Models for Blazars And AGN Neutrinos Martin Pohl Iowa State University XXXXth Rencontres de Moriond

2. Introduction I A blazar seen from the side Cygnus A XXXXth Rencontres de Moriond

3. Introduction II Low-energy component: synchrotron High-energy component: leptonic or hadronic? XXXXth Rencontres de Moriond

4. Introduction III What do models have to explain? • high apparent luminosity • emission up to > 10 TeV • low-energy component cuts off at ~10 keV • similar power in keV and TeV band • system size R < D (1014 cm) XXXXth Rencontres de Moriond

5. Introduction IV Hadronic models for blazars come in 3 classes: • photo-hadron production • proton synchrotron radiation • proton-proton colliders ~1019 eV ~1012 eV XXXXth Rencontres de Moriond

6. Basic Issues I We need to store the particles! RL << R => BG D >> 300 E19 Severe constraint for photo-hadron production models proton-synchrotron models XXXXth Rencontres de Moriond

7. Basic Issues II How many interaction partner are around? Lobs ~ eobs D3 c R2 nph >> eobs D3 c RL2 nph • Electron spectrum: n(g)=n0g-2 • Lsyn ~ (10-10 erg/s) D3.5 BG1.5 n0 EkeV0.5 R3 • nH > n0 > (1012 cm-3) L44 / D6.5 BG1.5 EkeV0.5 XXXXth Rencontres de Moriond

8. Basic Issues III How do we get rid of particles? Energy losses? pg-models: t >> (105 sec) D2enir E192 / L44 BG2 p-sync-models: t ~ (1015 sec) / D BG2 pp-models: t ~ (106 sec) / D n9 XXXXth Rencontres de Moriond

9. Basic Issues IV The location of the X-ray synchrotron component p-sync-models: must be primary e- ! p-g-models: first generation EkeV ~ 108 D BG p-p-models: EkeV ~ 10-2 D BG Ep,TeV2 XXXXth Rencontres de Moriond

10. Models I Model the jet as individual clouds of dense plasma Beall & Bednarek; Dar & Shaviv; MP, Schlickeiser, (Vainio, Lerche) XXXXth Rencontres de Moriond

11. Models II Colliding flows! In the jet frame: isotropization and compression of interstellar particles XXXXth Rencontres de Moriond

12. Models III Two consequences: • Enrichment with hadrons of energy ~ G • Deceleration of the jet Result: • first half-cycle of relativistic shock acceleration • similar to external shocks in GRBs, but without • electron acceleration XXXXth Rencontres de Moriond

13. Models IV Radiation products fully defined by spectral evolution of the particles Reacceleration ? XXXXth Rencontres de Moriond

14. Models V Basic spectral form is reproduced G0=300 n~109 • Homogeneous • interstellar medium • Variability from deceleration XXXXth Rencontres de Moriond

15. Models VI Inhomogeneous interstellar medium Rapid variability from interaction with isolated gas cloud XXXXth Rencontres de Moriond

16. Neutrinos I Expected neutrino intensity Schuster, MP, Schlickeiser XXXXth Rencontres de Moriond

17. Neutrinos II Gamma-ray high state F(> TeV)=10-10 cm-2 s-1 IceCube => 1 event/month Muon localization error q~1.8deg background 4 evts/month XXXXth Rencontres de Moriond

18. Neutrinos III Can the neutrino signal from AGN be higher? Yes, if the gamma-ray spectrum extends to >> 10 TeV • atmospheric background is reduced • localization is better (~ 1 deg) • But check the location of the synchrotron peak The 2 AMANDA events associated with 1959+650 are most likely background XXXXth Rencontres de Moriond

19. Conclusions • Three classes of hadronic AGN models exist • p-p collision models appear best suited to explain • g-ray blazars • p-p models prefer low-energy (TeV-ish) hadrons • only TeV-ish neutrinos predicted • neutrino event rate would be low • p-g models could produce HE neutrinos, • but not TeV gamma-rays XXXXth Rencontres de Moriond

20. Backup Slide De-absorbed spectrum of Mrk 501 Based on HEGRA data Preliminary! XXXXth Rencontres de Moriond