cosmic rays fermi acceleration and its observational implications · 2011-11-01 · summary...
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COSMIC RAYSFermi Acceleration and itsObservational Implications
Pasquale BlasiINAF/Arcetri Astrophysical Observatory
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WHAT DOES IT MEAN TO SEARCH FORTHE SOURCES OF COSMIC RAYS?
1. SOURCES OF HADRONS
2. …THAT CAN BE PROVEN TO REACH ENERGIES CLOSE TO KNEE
3. WITH A SPECTRUM COMPATIBLE WITH GALACTIC PROPAGATION
4. NO CONFLICT WITH ANISOTROPY
5. SPECTRA OF PROPAGATED NUCLEI COMPATIBLE WITH DATA
6. …THAT SATISFY MULTIFREQUENCY CONSTRAINTS
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Pillars of the SNR paradigm
H
2hRd
disc
HaloParticle escape
CRs IN SNR DIFFUSIVE SHOCK ACCELERATION,Q(E)~E-γ
PROPAGATION OF CRs IN THE GALAXY with D(E)~Eδ n(E)~E−γ−δ
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CR spectra and SNRsBlasi & Amato 2011
Deficit compensatedby extragalactic CRs
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Chemicals and the KNEE
δ=1/3
ONLY FOR δ=1/3 SPECTRUM OF He HARDER THAN SPECTRUM OF PROTONSAS A RESULT OF SPALLATION
Blasi & Amato 2011
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CR Anisotropy
δ=1/3
δ=0.6
Naïve expectation:
proportional to Eδ
Blasi & Amato 2011
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THEORY OF CR ACCELERATIONIN SNRs
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DYNAMICAL REACTION OF ACCELERATEDPARTICLES (all nuclei)
CR INDUCEDB-FIELD AMPLIFICATION
DYNAMICAL REACTIONOF AMPLIFIED B-FIELDS
Cosmic ray accelerationup to The knee
NON LINEARTHEORY of
DSA
Analytical: Malkov(1997,1999),Blasi(2002,2004),Amato&Blasi
(2005,2006)Numerical: Berezhko & Voelk
(1997),Zirakashvili&Aharonian(2010);Kang et al.
MonteCarlo: Ellison and Collaboratorssince 90s
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PRECURSOR
Und
istu
rbed
Med
ium
Shoc
k Fr
ont v
subshock Precursor
SUB
SHO
CK Velocity Profile
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SMALL PERTURBATIONS IN THE LOCAL B-FIELD CAN BEAMPLIFIED BY THE SUPER-ALFVENIC STREAMING OF THE
ACCELERATED PARTICLES
Particles are accelerated because there isHigh magnetic field in the acceleration region
High magnetic field is present because particlesare accelerated efficiently
Without this non-linear process, no acceleration of CRto High energies (and especially not to the knee!)
BUT…
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…MAGNETIC FIELD CAN BE AMPLIFIED BY
1.RESONANT STREAMING (Bell 78, Achterberg 83, Zweibel 78)
Fast generation, fast scattering … saturation?
2. NON RESONANT STREAMING (Bell 04, Amato & PB 09)
Probably more efficient generation rate but inefficient scattering
3. SHOCK CORRUGATION (DOWNSTREAM) Giacalone & Jokipii 07Not CR induced!It happens downstream only, it does not help with particle accelerationunless perpendicular shock
4. VORTICITY IN THE PRECURSOR (PB, Matthaeus, et al. 11)
Potentially very interesting, power on large scales
5. FIREHOSE INSTABILITY (Shapiro et al. 98)
Potentially very interesting, power on large scales
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Amato & PB 2009, Bell 2004
1000 years
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Extremely uncertain. It depends on:
a) Damping (type of waves?)
b) Backreaction of fields on the CR current
a) coupling between large and small spatial scales
A naïve extrapolation of QLT would lead to:in the resonant case, upstream(or possibly δB/B~1 becauseresonance gets lost)
!
!
"B2
8#=1MA
$Vs2%CR
!
"B2
4#=12$Vs
2%CRVs
c
Estimated analytically fromSaturation condition of non resonantModes (Bell 2004)
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TYPICAL THICKNESS OF FILAMENTS: ~ 10-2 pc
The synchrotron limited thickness is:
!
B "100 µGauss
In some cases the strong fields are confirmedby time variability of X-raysUchiyama & Aharonian, 2007
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PB, Amato & Caprioli, 2007
Magnetic fieldamplification leadsto higher values of theMaximum energy Knee Region
Data from Bertaina et al. 2008
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PRECURSORREGION RIM
Morlino, Amato, PB & Caprioli 2010
Ambiguity with perpendicular field
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EFFICIENT CR ACCELERATION ≠ HADRONIC GAMMAS
IN SN II EXPLOSION IN BUBBLE SMALL TARGET DENSITY (~10-3cm-3)
EFFICIENCY IS TIME DEPENDENT
MAX ENERGY IS TIME DEPENDENT HARD TO CATCH A PEVATRON
YOU COULD SEE GAMMAS FROM MC NEAR SNR, BUT PROBLEMATIC INTERPRETATION (SEE BELOW)
(PROBABLY MC MORE USEFUL TO INVESTIGATE THE PROBLEM OF ESCAPE)
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EFFICIENT
RXJ1713
RXJ1
713
Morlino, Amato & PB 2009
INEFFICIENT
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Fermi Coll. 2011
SOME OPEN QUESTIONS:
1.Photon background?
2.Thickness of filaments?
3.KN regime
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Caprioli 2011 (see also poster 131)
VERY SURPRISING TO SEE THAT THEREQUIRED ACCELERATION EFFIC AREHIGH BUT THE SPECTRA ARE STEEP
POSSIBLE SIGNATURE OF FINITE POSSIBLE SIGNATURE OF FINITE SPEED OF THE SCATTERING SPEED OF THE SCATTERING CENTERS !!!???CENTERS !!!???
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Morlino&Caprioli 2011(see also poster 145)
STEEP SPECTRUM BASICALLY IMPOSSIBLE TOEXPLAIN WITH LEPTONS
SEE ALSO POSTER 135, 146 FOR FERMI DATA ON TYCHO
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TWO SCENARIOS:
SNR SHOCK ENTERS THE MCCollisionless shock only involves the small fraction ofIons (low density)
Ion-neutral density kills waveslow Emax
MC IS ILLUMINATED BY CR FROM SNRThe mc only acts as a target for ppGamma ray flux depends on -Age of SNR-Diffusion coefficient around the SNR-Escape physics
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SNRShock Free Escape
Boundary
AdvectedCRs
The escape flux can be calculated using the transport equation IFone assumes a free escape boundary surface (DURING ST PHASE)
!
"esc(E, x) = D(E) #f (E, x)#x
$
% &
'
( ) x=x fe
Caprioli et al. 2010Caprioli et al. 2009
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COLLISIONLESS SNR SHOCKS INPARTIALLY IONIZED MEDIA:
Anomalous width of Balmer lines
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SHOCK VELOCITYNEUTRALSAND IONS
+ +Hotion
Cold neutral
hot neutral
Coldion
CHARGE EXCHANGE BROAD BALMER LINE (NEUTRALS THAT MADECHARGE EXCHANGE)REFLECTING THE TEMPERATURE OF IONS…
BUT THE LATTER AFFECTED BY EFFICIENT CR ACCELERATION
!
"v
PB+, 2011
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Helder et al. 2009
INFERRED EFFICIENCY of CR ACCELERATION 50-60% !!! (BUT modeldependent)
!
Wbroad = 8 ln 2 kT2
m" 1.02 vsh
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Sollerman et al. 2003
!
Wbroad = 8 ln 2 kT0
m" 21 km/s T0
104K#
$ %
&
' (
1/2
NEUTRALS
IONS
!
"v
CHARGE EXCHANGE OCCURSNOW IN THE CR INDUCEDPRECURSOR
NARROW BALMER LINE IS EXPECTED TO BE BROADERTHAN FOR AN UNMODIFIED SHOCK
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SUMMARY
REQUIRED POWER NON LINEAR THEORY OF ACCELERATION
MAGNETIC FIELD AMPLIFICATION MOST LIKELY CR INDUCED
EFFICIENT ACCELERATION SEEN IN SIZE OF X-RAY FILAMENTS,ABSENCE OF X-RAYS FROM PRECURSOR, EMAX @ KNEE, ANOMALOUS BALMER LINE WIDTHS
ANISOTROPY SUGGESTS δ∼1/3 INJECTION SLOPE 2.3-2.4
GAMMA RAYS ALSO SUGGEST STEEP INJECTION PROBABLYACTION OF SCATTERING CENTERS SPEED, BUT ALSO NEUTRALS
TYCHO PROBABLY THE FIRST UNAMBIGUOUS HADRONIC SOURCE
IN GENERAL EFFICIENT ACCELERATION DOES NOT IMPLY GAMMA
AS A BY-PRODUCT OF SNR PARADIGM TRANSITION TO EXTRAGALACTIC CR AT 1018 eV, NOT @ ANKLE