Blazars and NeutrinosBlazars and Neutrinos

C. Dermer (Naval Research Laboratory)

Collaborators: A. M. Atoyan (Universite de Montreal)M. Böttcher (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. Böttcher 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 Outline

1. Introduction1. Radio Galaxies2. Blazars3. Standard Blazar Model

2. Leptonic Models1. Radiation Processes (see Dermer and Schlickeiser 2002)2. Electron Injection and Energy Losses3. Model for Blazar Evolution

3. Hadronic Models1. Photomeson Production2. Neutrino Detection3. Neutral Beam Formation

4. Extended Jets

The Evolution of Active GalaxiesThe Evolution of Active Galaxies

The 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, beam

p + p + 0

| n + + | 2

eV Rays, cascade

FR IIs

Dilute clouds

BL Lac objects

Low luminosity

Weak jet

’sFR Is

FR I: low luminosity, twin jet sources

Cyg A

3C 2963C 465

FR II: high luminosity, lobe dominated

Radio Galaxies 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

3C 173.1

Blazars 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 sources

• BL Lac objects – nearly lineless (equivalent widths < 5 Å: 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 blazars

FR Is are parent population of BL Lac objects; FR IIs are parent population of FSRQs

L ~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-1

Mrk 421, z = 0.313C 279, z = 0.538

(Urry and Padovani 1995)

Blazar SED SequenceBlazar SED Sequence

Epk of synchrotron and Compton components inversely correlated with L

Sambruna et al. 1996; Fossati et al. 1998

Finding an order in the SEDs of blazars

FSRQ

BL Lac

Standard Blazar Model

Dermer and Schlickeiser 1994

-2 ≡ (sc/0.01)

•Nonthermal electron synchrotron and Compton processes

•Various sources of soft photons

•Relativistic motion accounts for lack of attenuation

Multiwavelength Blazar SpectraMultiwavelength Blazar SpectraLeptonic processes: Nonthermal synchrotron radiation

Synchrotron self-Compton radiation,

Accretion disk radiation

Disk radiation scattered by broad-line clouds

Blazar VariabilityBlazar Variability

Location of gamma-ray production site can be measured with GLAST

Blazar Sequence ComparisonBlazar Sequence Comparison

•Evolution from FSRQ to BL Lac Objects in terms of a reduction of fuel from surrounding gas and dust

FSRQ

BL Lac

What about Nonthermal Protons and Ions?What about Nonthermal Protons and Ions?

Nonthermal particles;Intense photon fields

Importance of external radiation field for photomeson production in FSRQs

Strong photomeson production

0, pnp

B and Photomeson NeutrinoProduction Calculations

)

640

K1 0.2 = 380b

K2 0.5-0.6 = 120 b

Beq

Bob

Tavecchio + 1998;Atoyan and Dermer 2001

NonthermalProton Spectrum

eVE

rGBcmr

N

sergsL

p

bL

ppp

p

p

1918

max6

2

1448

1010

)(/)101.3(

)(

102

• Nonthermal proton power corresponds to average –ray luminosity measured from 3C 279

• Unlikely to produce UHECRs in the inner jets of blazars

Proton power based on 3-week average spectral fluxes from 3C 279 in 1996 (Wehrle et al. 1998)

Photomeson production energy-loss timescale

Different Doppler factors

= 15 = 10

= 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 distribution

= 7 1 day3 day,10 day,21 day,30 day

Energy Distributions of Relativistic ProtonsDifferent Doppler factors

= 15

= 10

= 7Proton distribution after 3 weeks, with and without external field

Dots: no neutron escape

Nonthermal proton accumulation

np

Neutrino and -Ray FluencesDifferent Doppler factors

= 15

= 10

= 7 • Neutrino and -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 Flux

= 7

1 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 -ray fluxes observed during this time:

5x10-10 ergs cm-2 s-1

• ~ 10% efficiency in neutrinos compared to rays

• what is kpe?

= 15

= 10 = 7

Astronomy

High Energy Neutrino Physics

X-rays from the Outer Jet

Sambruna et al. 2001Wilson et al. 2000Wilson et al. 2001

Schwartz et al. 2000; Chartas et al. 2000

Pictor A Cygnus A

3C 273

PKS 0637-752

Pair halos(Aharonian, Coppi, and Völk 1994

Neutrino detection with km2 exposure

Three week average

P

100 TeV

Gaisser, Halzen, and Stanev 1995

-4

7

10

15

10

15

10No neutron escape

No external radiation field

Neutrino detection with km2 exposure

Parameters derived from 2 day flare of 3C 279 in 1996; tvar = 1 day

7

10

15

10

15

10No neutron escape

No external radiation field

Predict FSRQ sources of high energy neutrinos

Electromagnetic Cascade

n,

Hot Spot

Photons 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, & Völk 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,

Inner JetSMBH

Evolution of Luminous and Active Galaxies

Evolution of Blazars

will be tested by Neutrino Telescopes(Neutrinos from FSRQs rather than BL Lacs)

and Gamma Ray Telescopes (-ray halos around FR II galaxies, but not around FR I

galaxies;

Statistics of BL Lacs and FSRQs)

Radio Jet Formation Scenario

Galaxy EvolutionGalaxy 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 -ray test

Sensitivity of High Energy TelescopesSensitivity of High Energy Telescopes

Chandra

ASCAHESS