Hadronic modeling of AGN variability Recent...
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Hadronic modeling of AGN variability Recent Progress Felix Spanier 1 , Matthias Weidinger 1 , Svenja Hümmer 2 , Walter Winter 2 1 Lehrstuhl für Astronomie Universität Würzburg 2 Lehrstuhl für Theoretische Physik II Universität Würzburg HEPRO III Felix Spanier (Uni Würzburg) HEPRO III 1 / 14
Transcript of Hadronic modeling of AGN variability Recent...
Hadronic modeling of AGN variabilityRecent Progress
Felix Spanier 1, Matthias Weidinger 1, Svenja Hümmer 2, Walter Winter 21Lehrstuhl für AstronomieUniversität Würzburg
2Lehrstuhl für Theoretische Physik IIUniversität Würzburg
HEPRO III
Felix Spanier (Uni Würzburg) HEPRO III 1 / 14
Introduction
Long standing dispute between leptonic and hadronic modelsNowadays many non-HBL TeV sources have been observedThe need for hadronic models is evidentVariability allows a stricter determination of source parameters
Felix Spanier (Uni Würzburg) HEPRO III 2 / 14
Model setup
Model consists of separateacceleration and radiation zoneAcceleration of electrons andprotons includes Fermi-I andFermi-IISpectrum is derivedself-consistently from jetmicrophysics
Figure: Geometrical structure ofacceleration and radiation zone
Felix Spanier (Uni Würzburg) HEPRO III 3 / 14
Multizone models
Short detour: New model indevelopment
Spatially resolved modelShock is implemented asbackground fluid velocityForward and backward movingelectronsParticle flipping imitates smallangle scatteringEffectively Fermi-I
Please take a look at StephanRichter’s poster for details.Hadronic radiation models will beimplemented.
Figure: Geometry of the multizone model
Felix Spanier (Uni Würzburg) HEPRO III 4 / 14
General features
First proposed by Mannheim (1993)Nonthermal proton distributionp − γ photomeson productionπ0-decay into photonsπ±-decay into e± with subsequentsynchrotron radiationElectron-positron-pairproduction Figure: Hadronic fit for 3C279
(from Mannheim 1993)
Felix Spanier (Uni Würzburg) HEPRO III 5 / 14
Set of equationsElectron/Positron evolution
∂tNe− =∂γ
βs,eγ
2︸ ︷︷ ︸Synchrotron
+ PIC(γ)︸ ︷︷ ︸Inverse Compton
· Ne−
− Ne−
tesc,e︸ ︷︷ ︸Escape
+ Qpp︸︷︷︸Pairprod.
+ Qpγ−︸ ︷︷ ︸Pion decay
+ Q︸︷︷︸Injection
Proton evolution
∂tNp =∂γ
βs,pγ
2︸ ︷︷ ︸Synchrotron
· Np
− Np
trad,esc,p︸ ︷︷ ︸Escape
+ Q︸︷︷︸Injection
Q is injected from the acceleration zoneFelix Spanier (Uni Würzburg) HEPRO III 6 / 14
Set of equations
Photon evolution
∂tNγ = Rs︸︷︷︸Synchrotron
+ Rc︸︷︷︸Inverse Compton
+ Rπ0︸︷︷︸π0decay
− c
αSSA︸ ︷︷ ︸Self synchrotron
+ αpp︸︷︷︸Pairprod.
Nγ −Nγ
tph,esc︸ ︷︷ ︸Escape
Felix Spanier (Uni Würzburg) HEPRO III 6 / 14
Hadronic implementationPrevious models rely on Monte Carlo codes to simulate photomesonproductionThe leading model here is the SOPHIA code (Mücke et al.) based onQGSJETMonte Carlo is not at any rate fast enough to produce time-dependentmodelsOne way out: Parametrization of results by Kelner& Aharonian
Figure: Parametric fit from Kelner&Aharonian
Felix Spanier (Uni Würzburg) HEPRO III 7 / 14
Hadronic fit - 3C279
Details: see Matthias Weidinger’s poster
Felix Spanier (Uni Würzburg) HEPRO III 8 / 14
Hadronic fit - 3C279
Details: see Matthias Weidinger’s poster
Felix Spanier (Uni Würzburg) HEPRO III 8 / 14
Hadronic fit - 3C454.3
Det
ails
:se
eM
atth
ias
Wei
ding
er’s
post
er
Felix Spanier (Uni Würzburg) HEPRO III 9 / 14
Hadronic fit - 3C454.3
Det
ails
:se
eM
atth
ias
Wei
ding
er’s
post
er
Felix Spanier (Uni Würzburg) HEPRO III 9 / 14
Drawbacks of Kelner&Aharonian
Unstable secondary particles are integrated outImplementation of new (accelerator) observations requires new MonteCarlo generator and new parametrization
Felix Spanier (Uni Würzburg) HEPRO III 10 / 14
Simplified Model
New model design: Morecomplete than deltaFactorized response functionOnly single integration over thedistribution function necessaryModels some of the physicalprocesses
Felix Spanier (Uni Würzburg) HEPRO III 11 / 14
Simplified Model
New model design: Morecomplete than deltaFactorized response functionOnly single integration over thedistribution function necessaryModels some of the physicalprocesses
Felix Spanier (Uni Würzburg) HEPRO III 11 / 14
Simplified Model
QITb = Np
(Eb
χIT
)mp
Eb
∞∫εth/2
dy nγ
(mp y χIT
Eb
)M IT
b f IT(y)
Rb(x , y) ≡∑
IT
RIT(x , y) ≡∑
IT
12y2
2y∫εth
dεr εr σIT(εr ) M ITb (εr ) δ
(x − χIT(εr )
).
factorizes inRIT(x , y) = δ(x − χIT) M IT
b f IT(y)
with
f IT(y) ≡ 12y2
2y∫εth
dεr εr σIT(εr ) .
Felix Spanier (Uni Würzburg) HEPRO III 11 / 14
Simplified Model
New model design: Morecomplete than deltaFactorized response functionOnly single integration over thedistribution function necessaryModels some of the physicalprocesses
Qb(Eb) =
∞∫Eb
dEp
EpNp(Ep)
∞∫εthmp2Ep
dεnγ(ε) Rb(x , y)0.10 1.000.500.20 2.000.30 3.000.15 1.500.70
1
5
10
50
100
500
1000
Εr �GeV�
Σ�Μ
barn�
LR
HR
KP
Felix Spanier (Uni Würzburg) HEPRO III 11 / 14
Simplified Model
0.0 0.5 1.0 1.5 2.00
50
100
150
200
250
y��Ep ��mp �GeV�
FΠ�Μ
barn�
Proton � Π� or neutron � Π�
0.0 0.5 1.0 1.5 2.00
50
100
150
200
250
y��Ep ��mp �GeV�
FΠ�Μ
barn�
Proton � Π� or neutron � Π�
0.0 0.5 1.0 1.5 2.00
50
100
150
200
250
y��Ep ��mp �GeV�
FΠ�Μ
barn�
Proton or neutron � Π0
0.0 0.5 1.0 1.5 2.00
50
100
150
y��Ep ��mp �GeV�
FΠ�Μ
barn�
Proton � Π� or neutron � Π�
Direct
LR HRMulti�Π
0.0 0.5 1.0 1.5 2.00
50
100
150
y��Ep ��mp �GeV�
FΠ�Μ
barn�
Proton � Π� or neutron � Π�
Direct
HRMulti�Π
0.0 0.5 1.0 1.5 2.00
50
100
150
y��Ep Ε��mp �GeV�FΠ�Μ
barn�
Proton or neutron � Π0
DirectLR
HRMulti�Π
Felix Spanier (Uni Würzburg) HEPRO III 12 / 14
Simplified Model
103 104 105 106 107 108 109 101010�16
10�15
10�14
10�13
10�12
E�GeV
EΠ2
Q��
NΓ
NpG
eVcm�3s�
1 �
Π�
Sim�CSim�BSim�ABWSOPHIA
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103 104 105 106 107 108 109 101010�16
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103 104 105 106 107 108 109 10100
2
4
6
8
10
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E�GeV
Q��Q�
���
Sim�CSim�BSim�ABWSOPHIA
103 104 105 106 107 108 109 10100.0
0.5
1.0
1.5
2.0
2.5
E�GeV
QΠ��QΠ
0
Π��Π0
Sim�CSim�BSim�ABWSOPHIA
103 104 105 106 107 108 109 10100.0
0.2
0.4
0.6
0.8
1.0
E�GeV
QΠ��QΠ
0
Π��Π0
Sim�CSim�BSim�ABWSOPHIA
Pion production in the AGN testcase
Felix Spanier (Uni Würzburg) HEPRO III 12 / 14
Neutrino Emission
New model allows also for the prediction of neutrino flux
100 101 102 103 104 105 106 107 108 10910�23
10�22
10�21
10�20
10�19
10�18
10�17
10�16
10�15
E�GeV
EΝ2
Q��
NΓ
NpG
eVcm�3 s�1 �
GRB: Νe,Νe
Νe SOPHIAΝe from n decayΝe from Μ decayΝe SOPHIAΝe
103 104 105 106 107 108 109 101010�16
10�15
10�14
10�13
10�12
10�11
E�GeV
EΝ2
Q��
NΓ
NpG
eVcm�3 s�1 �
AGN: Νe,Νe
Νe SOPHIAΝe from n decayΝe from Μ decayΝe SOPHIAΝe
103 104 105 106 107 108 109 1010 1011 101210�15
10�14
10�13
10�12
10�11
10�10
E�GeV
EΝ2
Q��
NΓ
NpG
eVcm�3 s�1 �
BB: Νe,Νe
Νe SOPHIAΝe from n decayΝe from Μ decayΝe SOPHIAΝe
Neutrino-/Anti-Neutrino-Production rate
Felix Spanier (Uni Würzburg) HEPRO III 13 / 14
Neutrino Emission
100 101 102 103 104 105 106 107 108 1090
2
4
6
8
10
E�GeV
Flux
ratio
:Νe�Ν
e
GRB: Νe�Νe
SOPHIA
From Π�Μ�n�K decays
From Π�Μ decays
103 104 105 106 107 108 109 10100
2
4
6
8
10
E�GeV
Flux
ratio
:Νe�Ν
e
AGN: Νe�Νe
SOPHIA
From Π�Μ�n�K decays
From Π�Μ decays
103 104 105 106 107 108 109 1010 1011 10120
2
4
6
8
10
E�GeV
Flux
ratio
:Νe�Ν
e
BB: Νe�Νe
SOPHIA
From Π�Μ�n�K decays
From Π�Μ decays
100 101 102 103 104 105 106 107 108 1090.6
0.7
0.8
0.9
1.0
1.1
1.2
1.3
1.4
E�GeV
Flux
ratio
:ΝΜ�ΝΜ
GRB: ΝΜ�ΝΜ
SOPHIA
From Π�Μ�n�K decays
From Π�Μ decays
103 104 105 106 107 108 109 10100.6
0.7
0.8
0.9
1.0
1.1
1.2
1.3
1.4
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Flux
ratio
:ΝΜ�ΝΜ
AGN: ΝΜ�ΝΜ
SOPHIA
From Π�Μ�n�K decays
From Π�Μ decays
103 104 105 106 107 108 109 1010 1011 10120.6
0.7
0.8
0.9
1.0
1.1
1.2
1.3
1.4
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Flux
ratio
:ΝΜ�ΝΜ
BB: ΝΜ�ΝΜ
SOPHIA
From Π�Μ�n�K decays
From Π�Μ decays
Neutrino-/Anti-Neutrino-Production rate
Felix Spanier (Uni Würzburg) HEPRO III 13 / 14
Neutrino Emission
Better prediction of neutrino flavor
100 101 102 103 104 105 106 107 108 1090.30
0.35
0.40
0.45
0.50
0.55
0.60
0.65
0.70
E�GeV
Flux
ratio
:�Ν
e�Νe���ΝΜ�ΝΜ�
GRB: �Νe�Νe���ΝΜ�ΝΜ�
SOPHIA
From Π�Μ dec., h�0
From Π�Μ�n�K decays
From Π�Μ decays
103 104 105 106 107 108 109 10100.30
0.35
0.40
0.45
0.50
0.55
0.60
0.65
0.70
E�GeV
Flux
ratio
:�Ν
e�Νe���ΝΜ�ΝΜ�
AGN: �Νe�Νe���ΝΜ�ΝΜ�
SOPHIA
From Π�Μ dec., h�0
From Π�Μ�n�K decays
From Π�Μ decays
103 104 105 106 107 108 109 1010 1011 10120.30
0.35
0.40
0.45
0.50
0.55
0.60
0.65
0.70
E�GeV
Flux
ratio
:�Ν
e�Νe���ΝΜ�ΝΜ�
BB: �Νe�Νe���ΝΜ�ΝΜ�
SOPHIA
From Π�Μ dec., h�0
From Π�Μ�n�K decays
From Π�Μ decays
Flavor-ratio for µ-e-Neutrinos
Felix Spanier (Uni Würzburg) HEPRO III 13 / 14
Summary
Time-dependent lepto-hadronic model including particle acceleration isavailableComplicated time variation patternsNew photo-meson production model is discussed
Felix Spanier (Uni Würzburg) HEPRO III 14 / 14
