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Acceleration of highest energy cosmic rays in jets of powerful AGNsPowerPoint Presentation

Acceleration of highest energy cosmic rays in jets of powerful AGNs

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### Acceleration of highest energy cosmic rays in jets of powerful AGNs

Maxim Lyutikov (UBC, U. Rochester)

in collaboration with

Rashid Ouyed (UofC)

UHECRs powerful AGNs

CR spectrum, composition, confinementsecond knee ?

toe ?

1 particle per km2

per century

knee, 4 1015 eV

ankle,3 1018 eV

heavy (Fe)

- Isotropic to highest energies
- Possible small-scale clustering
at highest energies

protons

protons

- UHECR composition: p-heavy-p

- Propagation: B-field
- rL~E21/B G pc, Galaxy ~ 10-6 G
- only E < 1019 eV are confined
- E > 1019 eV must be extragalactic

Proton fraction (green: HiRes stereo)

GZK cut-off powerful AGNsGreisen PRL; Zatsepin & Kuzmin JETP Lett (1966)

- Cosmic Microwave Background radiation (CMB) T=2.7 K
- Photo-pion production
- Attenuation length for ~ 1020 eV CR is
~ tens of Mpc. Very solid estimate;

worse for Z> 1

- UHECRs must be produced locally , < 100 Mpc

pair production energy loss

p + 2.7k + p + 0

n + +

pion production energy loss

pion production rate

Is GZK cutoff seen? powerful AGNs

- HiRes (fluorencence) and AGASA (ground array) disagree

Origin of cosmic rays powerful AGNs

Low energy CRs (<10 powerful AGNs15 eV): in SNRs through Fermi shock acceleration

observed in interplanetary space

Spectrum is “right” dn/dE ~ E-2

But: not yet confirmed by γ-ray observations of π0 decay in SNR

SNs cannot accelerate beyond ~Z 1014

Acceleration of UHECRs

not clear if can be extended to UHECR regime

maximal efficiency (τacc ~ γ/ωB) is usually either assumed or put “by hand” by using

more than allowed (super-Bohm) cross-field diffusion

Hardening above the “ankle” ~ 1018 eV may indicate new acceleration mechanism

scattering off Alfven

waves

B-field

v1 > v2

shock

Acceleration of CRWe propose new, non-stochastic acceleration mechanism

that turns on above the ankle, E> 1018 eV

Alfven wave

General constraints powerful AGNson acceleration cite:

- Constraints on UHECRs are so severe, “~“ estimates are useful
- Maximal acceleration E-field < B-field: E=β0 B, β0 ≤ 1
- Total potential Φ = E R= β0 B R
- Maximal energy E~ Z e Φ = β0 Z e B R
- Maximal Larmor radius rL ~ β0 R (Hillas condition)
- Two possibilities:
- E || B (or E>B) – DC field
- E ┴ B – inductive E-field

} Two paradigms for UHECR acceleration

E powerful AGNs

ji

ie

Φ,R

B

DC (linear) acceleration for UHECR does not workE

- Full DC accelerations schemes (with E-field || to B-field or E>B) cannot work in principle for UHECRs
- leptons will shut off E|| by making pairs (typically after ΔΦ << 1020 eV)
- Double layer is very inefficient way of accelerating UHECRs: E-field will generate current, current will create B-field, there will be large amount of energy associated with B-field. One can relate potential drop with total energy:
- Relativistic double layer:
- Maximal energy
- Total energy: E~ B2 R3~ I2 R c2

B

Lovelace 76 powerful AGNs

Blandford 99

B

E ┴ B : Inductive potentialE

E ┴ B: Poynting flux in the system: relate Φ to luminocity

Electric potential

Pictor A (FRII)

- To reach Φ=3 1020 eV, L > 1046 erg/s (for protons)
- This limits acceleration cites to high power AGNs (FRII, FSRQ,
high power BL Lac, and GRBs)

- There may be few systems with enough potential within GZK sphere
(internal jet power higher than emitted), the problem is acceleration scheme

For linear velocity profile powerful AGNs

V

V

E~x

E~-x

B

B

Potential Φ~-x2

Potential Φ~x2

Potential energy of a charge in a sheared flowE=-v x B

Depending on sign of (scalar) quantity (B *curl v) one sign of charge is at

potential maximum

Protons are at maximum for negative shear (B *curl v) < 0

This derivation is outside of applicability of non-relativisitc MHD

V powerful AGNs

B

v

E

x

Bφ

Er

Er

Astrophysical location: AGN jets- There are large scale B-fields in AGN jets
- Jet launching and collimation (Blandford-Znajek, Lovelace)
- Observational evidence of helical fields (Lyutikov et al 2004; Zavala)
- Jets may collimate to cylindrical surfaces (Heyvaerts & Norman)
- Jets are sheared (fast spine, slow edge)

Protons are at maximum for negative shear (B *curl v) < 0.

Related to (Ω*B) on black hole

Ω

BH and disk can act as Faradey disk

Acceleration by large scale inductive E-fields: powerful AGNsE~∫ v•E ds

V

- Potential difference is between different flux surface (pole-equator)
- In MHD plasma is moving along V=ExB/B2 – cannot cross field lines
- Particle has to cross flux surfaces
- Kinetic motion across B-fields- particle drift

E

B

∆ powerful AGNs

B

ud

F

∆

BφxBφ

Er

Drift due to sheared Alfven wave- Electric field Er ~- vz x Bφ : particle need to move radially, but cannot do it freely (Bφ).
- Kinetic drift
- Inertial Alfven wave propagating
along jet axis ω=VA kz

- Bφ(z) → Ud ~ ~er

B-field

F

Udrfit ~ F x B

Why this is all can be relevant? powerful AGNs Very fast energy gain :

- highest energy particles are accelerated most efficiently!!!
- low Z particles are accelerated most efficiently!!! (highest rigidity are accelerated most efficiently)
- Acceleration efficiency does reach absolute theoretical maximum 1/ωB
- Jet needs to be ~ cylindrically collimated; for spherical expansion adiabatic losses dominate

Energy gain:

For linear velocity profile, V=η x, E= η x B/c, x = ud t,

→

Wave surfing can help powerful AGNs

- Shear Alfven waves have δE~(VA/c) δB,
- Axial drift in δExB helps to keep particle in phase
- Particle also gains energy in δE

δE

B

∆

γmax/γ0

ud

Alfven wave

with shear

Er

Most of the energy gain is in

sheared E-field (not E-field of

the wave, c.f. wave surfing)

Alfven wave

without shear

Acceleration rate DOES reach absolute theoretical maximum ~ γ/ωB

- Final orbits (strong shear), rL ~ Rj, drift approximation is no longer valid
- New acceleration mechanism
- For η < ηcrit < 0, ηcrit = - ½ ωB/γ, particle motion is unstable
- non-relativistic:
- Acceleration DOES reach theoretical
maximum ~ γ/ωB

- Note: becoming unconfined is GOOD
for acceleration (contrary to shock acceleration)

η=V’

ankle ~

γ

Mixed

composition

protons

Spectrum- From injection dn/dγ~γ-p →dn/dγ ~ γ-2

Particles below the ankle do not

gain enough energy to get rL ~Rj

and do not leave the jet

This is what is seen

Radiative losses ~

- Equate energy gain in E =B to radiative loss ~ UBγ2
- As long as expansion is relativistic, total potential remains nearly constant, one can wait yrs – Myrs to accelerate

Astrophysical viability ~

- Need powerful AGN FR I/II (weak FR I , starbursts are excluded)
- UHECRs (if protons) are not accelerated by our Galaxy, Cen A or M87

- Several powerful AGN within 100 Mpc, far way → clear GZK cut-off should be observed
- For far-away sources hard acceleration spectrum, p~ 2 , is needed
- Only every other AGN accelerates UHECRs
- Clustering is expected but IGM B-field is not well known
- μGauss field of 1Mpc creates extra image of a source (Sigl)
- Isotropy & clustering: need ~ 10 sources (Blasi & Di Marco)

- Fluxes: LUHECR ~ 1043 erg/sec/(100 Mpc)3 – 1 AGN is enough
- Matching fluxes of GCR and EGCR….

Main properties of the mechanism: ~

- Protons are at maximum of electric potential for negative shear (B *curl v) < 0 (related to (B*ΩBH))
- Acceleration rate increases with energy and does reach absolute theoretical maximum τacc ~ γ/ωB
- At a given energy, particles with smallest Z (smallest rigidity) are accelerated most efficiently (UHECRs above the ankle are protons)
- produces flat spectrum
- Acceleration @ 1 pc < r< Mpc: no radiative losses, lots of time
- Pierre Auger: powerful AGNs?
- GZK cut-off
- few sources

- May see ν & γ fluxes toward source (HESS, IceCube)

Let’s wait and see

The Auger Observatory (Argentina): hybrid detector ~

- The Auger Observatory combines
- Surface Detector Array and Air Fluorescence Detectors
- Advanced control of position, performance, weather (e.g. T, humidity)
- Independent measurement techniques allow control of systematics
- Energy: ΔE/E ~ .5 @ 1020 eV
- Angle: 0.6 o
- Primary mass measured in complementary ways
- First result:
- no extra flux from Galactic center (contrary to AGASA and SUGER)
- < 25% of photons @ > 1019 eV
- (bad for top-down and Z-model)

- Coverage ~ AGASA

Intergalactic propagation of UHECR ~

- Structure of intergalactic B-field, not very known
- Average B-field < 10-9 G , rL ~ 100 Mpc for 1019 eV
- Layers of high B-field with voids. Levi flights???
- Structures of ~ 10Mpc, 10-7 G are seen in synchrotron emission (Kronberg), enough to deflect ~ radian

“Cosmic web”, Bond et al 1996

2dFGalaxy Redshift Survey 2003

Earth atmosphere is a telescope ~

Ground monitors of charged particles (e.g. AGASA)

Neutron Monitors and Supermonitors

Ionization Chambers

Muon Telescope

Observation of fluorencence and Cherenkov light (Fly’s eye & HiRes, Haverah Park)

electrons

- -rays

muons

Detectors: two typesWhen statistics is low, calibration problems begin

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