Numerical simulations of radiation rocesses in AGN. Effect of chemical comosition Xavier Rodrigues DESY, Zeuthen, Germany Astroteilchenschule, Bärnfels October 14, 2016
Introduction > Question: origin & comosition of Ultra-High Energy Cosmic Rays > Likely dominated by extra-galactic sources [Allard et al. 2007 astro-h0512345] > Candidate: Active Galactic Nuclei (AGN) > Numerical model for hadronic interactions > Predict cosmic-ray (CR) and ν sectra > Study effect of heavyaverage elements of X max motivation: exerimental data X max (g/cm 2 ) Syst. 850 800 750 700 roton iron 650 600 EPOS-LHC QGSJetII-04 Sibyll2.1 AUGER, PRELIMINARY 17.0 17.5 18.0 18.5 19.0 19.5 20.0 log (E/eV) 10 [Auger Collaboration, ICRC 2015] Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 2
Physical model Blazar > CR acceleration in the jet > Consider a lasma blob along the jet of radius r = c t flare > B confinement of charged articles > n, ν escae directly Doler factor D relativistic jet suermassive black hole > Useful transforms: [Obs frame] Energy: E obs = Luminosity: L obs = [Jet rest frame] ( ) D E, 1 + z D4 (1 + z) 2 L relativistic Doler: D time dilation: D relativistic beaming: D 2 thin accretion disk Picture courtesy NASA, Dana Berry/Skyworks Digital Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 3 thick dust torus
Physical model Blazar Sectral Energy Distribution (SED) serves as target hoton field for CR interactions inverse Comton (letonic scenario) hadronic cascade (hadronic scenario) synchrotron self-comton accretion IR blue: L γ < 10 45.5 erg/s green: L γ < 10 45.5 erg/s red: L γ < 10 47.5 erg/s black: L γ > 10 48 erg/s Points: observation. Lines: models [Ghisellini 2013 arxiv:1309.4772] Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 4
Physical model hadronic rocesses Fermi-shock CR acceleration ower-law CR injection dn de = E α index α deends on shock comression ratio (tyically α = 2) Acceleration, synchrotron, escae time deend on magnetic field strength Examles of interactions π hotoion inv. Comton hoto disintegration n π, µ decay e air rod nuclear decay µ ν µ synchrotron π + ν µ ν e ē e If heavier nuclei are resent, 56 Fe 4 He 14 C 14 N n ν e e Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 5
Interaction framework > NEUCOSMA [Bearwald et al, AP 35 (2012) 508-529] numerical framework for nuclear cascades > Develoed for Gamma-Ray Bursts (GRB) aly to AGN > Numerically solve PDE system (1 eq. er article secies) N(E) t ==0 if steady state reached = N(E) ( b(e) N(E)) + Q(E) E t esc energy loss article escae π 0 article injection n π + Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 6
Preliminary results > Inut Blazar SED roosed in [Anchordoqui et al., AP 29 (2008) 1-13] > L γ = 10 45 erg/s () () > Γ = 10 1.5 > t obs flare = 104 s We will also consider > z = 0.1 > B = 0.9 G Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 7
Preliminary results > Pure roton injection: [X Rodrigues, A Fedynitch, D Boncioli, W Winter in rearation] Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 8
Preliminary results > Pure iron-56 injection: [X Rodrigues, A Fedynitch, D Boncioli, W Winter in rearation] Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 9
Preliminary results > Comarison of total neutrino sectra [X Rodrigues, A Fedynitch, D Boncioli, W Winter in rearation] Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 10
Outlook > Acceleration of heavy nuclei in AGN has a significant effect on the exected ν sectrum > Currently attemting to reroduce other ublished results > Next ste: robe arameter sace, articularly isotoic comosition > In the future: consider more sohisticated model to include hoton feedback (self-consistent icture of hotons rotons nuclei) Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 11
Backu Examle: treatment of γ π + in NEUCOSMA [W Winter, rivate note] Xavier Rodrigues Astroteilchenschule, Bärnfels October 14, 2016 Page 12