Blazars and Neutrinos C. Dermer (Naval Research Laboratory) Collaborators: A. M. Atoyan (Universite de Montreal) M. Bttcher (Rice University) R. Schlickeiser (Bochum U.) Erice, June 2002

Transformation Properties of External Radiation Fields, Energy Loss Rates and Scattered Spectra, and a Model for Blazar Variability, CD and R. Schlickeiser, ApJ, in press, August 20th, 2002 (astro-ph/020280)High Energy Neutrinos from Photomeson Processes in Blazars,A. Atoyan and CD, PRL, 87, 22, 1102 (2001)An Evolutionary Scenario for Blazar Evolution, M. Bttcher and CD, ApJ, 564, 86 (2002) X-ray Synchrotron Spectral Hardenings from Compton and Synchrotron Losses in Extended Chandra Jets 2002, CD and A. Atoyan, ApJ Letters, 2002, 568, L81

Outline IntroductionRadio GalaxiesBlazarsStandard Blazar ModelLeptonic ModelsRadiation Processes (see Dermer and Schlickeiser 2002)Electron Injection and Energy LossesModel for Blazar EvolutionHadronic ModelsPhotomeson ProductionNeutrino DetectionNeutral Beam FormationExtended Jets

The Evolution of Active GalaxiesThe nuclear activity in a galaxy evolves in response to the changing environment, which itself imprints its presence on the spectral energy distribution of the galaxy. External Photon field FSRQs, Intense n, n beamp + g p + p0 | n + p+ | 2 g> 1014 eV g Rays, cascadeFR IIsDilute clouds BL Lac objectsLow luminosity Weak jet No nsFR Is~

Radio Galaxies Fanaroff-Riley (1974) Classification Scheme

FR I: separation between the points of peak intensity in the two lobes is smaller than half the largest size of the source Edge-darkened, twin jet sources FR II: separation between the points of peak intensity in the two lobes is greater than half the largest size of the source. Edge-brightened hot spots and radio lobes, classical doubles

Morphology correlates strongly with radio power at 2x1025 W/Hz at 178 MHz ( 4x1040 ergs s-1), or total radio power of 1042 ergs s-1

Optical emission lines in FR IIs brighter by an order of magnitude than in FR Is for same galaxy host brightness

FR I: low luminosity, twin jet sourcesCyg A3C 2963C 465FR II: high luminosity, lobe dominated3C 173.1

Blazars (see lectures by R. Sambruna for more detail)Class of AGNs which includes optically violently variable quasars; highly polarized quasars, flat spectrum radio sources, superluminal sourcesBL Lac objects nearly lineless (equivalent widths < 5 : dilute surrounding gas)Flat Spectrum Radio Quasars (strong emission lines: dense broad line region clouds) Blazars: radio galaxies where jet is pointed towards us; radio galaxies = misaligned blazarsFR Is are parent population of BL Lac objects; FR IIs are parent population of FSRQsL ~5x1048 x (f/10-9 ergs cm-2 s-1) ergs s-1L ~1045 x (f/10-10 ergs cm-2 s-1) ergs s-1Mrk 421, z = 0.313C 279, z = 0.538(Urry and Padovani 1995)

Blazar SED SequenceEpk of synchrotron and Compton components inversely correlated with L Sambruna et al. 1996; Fossati et al. 1998Finding an order in the SEDs of blazars FSRQBL Lac

Standard Blazar Model Dermer and Schlickeiser 1994t-2 (tsc/0.01)Nonthermal electron synchrotron and Compton processes

Various sources of soft photons

Relativistic motion accounts for lack of gg attenuation

Multiwavelength Blazar SpectraLeptonic processes: Nonthermal synchrotron radiationSynchrotron self-Compton radiation,Accretion disk radiationDisk radiation scattered by broad-line clouds

Blazar VariabilityLocation of gamma-ray production site can be measured with GLAST

Blazar Sequence Comparison Evolution from FSRQ to BL Lac Objects in terms of a reduction of fuel from surrounding gas and dustFSRQBL Lac

What about Nonthermal Protons and Ions? Nonthermal particles;Intense photon fields

Importance of external radiation field for photomeson production in FSRQs

Strong photomeson production

B and d

Photomeson NeutrinoProduction Calculationses(e) 640K1 0.2s = 380mbK2 0.5-0.6s = 120 mbdBtggBeqBob Tavecchio + 1998;Atoyan and Dermer 2001

NonthermalProton Spectrum Nonthermal proton power corresponds to average gray luminosity measured from 3C 279 Unlikely to produce UHECRs in the inner jets of blazarsProton power based on 3-week average spectral fluxes from 3C 279 in 1996 (Wehrle et al. 1998)

Photomeson production energy-loss timescaleDifferent Doppler factors d = 15d = 10d = 7 photomeson energy-loss timescales in observer frame for properties derived from 3-week average spectral fluxes from 3C 279 in 1996 (Wehrle et al. 1998) tvar = 1 day compare case with no external field

Atoyan and Dermer 2001

Evolution of the proton distributiond = 7 1 day3 day,10 day,21 day,30 day

Energy Distributions of Relativistic ProtonsDifferent Doppler factors d = 15d = 10d = 7Proton distribution after 3 weeks, with and without external fieldDots: no neutron escape

Nonthermal proton accumulation

Neutrino and g-Ray FluencesDifferent Doppler factors d = 15d = 10d = 7 Neutrino and g-ray fluences from 3C 279 based on 3-week average spectral fluxes observed in 1996 (Wehrle et al. 1998), with tvar = 1 day

Evolution of the Neutrino Fluxd = 71 day3 day,10 day,21 day,30 day

3-week average Neutrino FluxesDifferent Doppler factors Neutrino fluxes from 3C 279 based on 3-week average spectral fluxes observed in 1996 (Wehrle + 1998), with tvar = 1 day Compare average g-ray fluxes observed during this time: 5x10-10 ergs cm-2 s-1 ~ 10% efficiency in neutrinos compared to g rays what is kpe?d = 15d = 10d = 7

n Astronomy High Energy Neutrino Physicsm

X-rays from the Outer JetSambruna et al. 2001Wilson et al. 2000Wilson et al. 2001Schwartz et al. 2000; Chartas et al. 2000Pictor ACygnus A3C 273PKS 0637-752Pair halos(Aharonian, Coppi, and Vlk 1994

Neutrino detection with km2 exposureThree week average Pn men 100 TeV en en1/2 Gaisser, Halzen, and Stanev 1995-4d7

10

15

10

15

10No neutron escapeNo external radiation field

Neutrino detection with km2 exposureParameters derived from 2 day flare of 3C 279 in 1996; tvar = 1 day

d7

10

15

10

15

10No neutron escapeNo external radiation fieldPredict FSRQ sources of high energy neutrinos

Electromagnetic Cascaden,gHot SpotPhotons with energies > 100 TeV are attenuated by CMB and DIIRF background and materialize into e+-e- pairs and produces electromagnetic cascade

Neutron beam more highly directed than jet plasma; pre-accelerates IGM in FSRQs;Difference between FR I and FR II galaxies

Some beam energy is reprocessed into rays through Compton scattering, forming pair halos around radio-loud AGN (Aharonian, Coppi, & Vlk 1994)

Rest of beam energy emerges as X-ray synchrotron jet

Larger magnetic field in hot spot reprocesses directed electron-positron beam energy into synchrotron radiation?Blazar energy in 30-100 TeV rangeinjected into IGM IGMn,gInner JetSMBH

Evolution of Luminous and Active Galaxies

Evolution of Blazars

Radio Jet Formation Scenariowill be tested by Neutrino Telescopes(Neutrinos from FSRQs rather than BL Lacs)and Gamma Ray Telescopes (g-ray halos around FR II galaxies, but not around FR I galaxies;Statistics of BL Lacs and FSRQs)

Galaxy Evolution Dark matter halos collapse from initial spectrum of density fluctuations Press-Schechter formalism for collapse on different mass scales Hierarchical structure formation (bottom-up) Cluster accretion and subcluster interactions Infrared luminous galaxies Galaxy mergers and fueling: evolution of active galaxies Black Hole/Jet Physics Formation of jets in FR II and FRI radio galaxies: importance of neutral beams Extended X-ray emission from jet sources Neutrino and g-ray test

Sensitivity of High Energy TelescopesChandraASCAHESS