Hadronic Models for Blazars And AGN Neutrinos Martin Pohl Iowa State University

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