a multi-wavelength and multi-messenger spectral model for
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A multi-wavelength and multi-messenger spectral
model for astrophysical jets
FFP14, Marseille - 17 juillet 2014
S. Drappeau1, S. Markoff2, 1IRAP (CNRS/Université de Toulouse), 2University of Amsterdam
S. Corbel3, M.A. Nowak4, J. Wilms5 3AIM (CEA/CNRS/Université Paris Diderot), 4MIT, 5University of Erlangen-Nuremberg
Motivations
[eV]E1310 1410 1510 1610 1710 1810 1910 2010
]-1
sr-1 s
-2 m
1.6
[GeV
F(E)
2.6
E
1
10
210
310
410GrigorovJACEEMGUTien-ShanTibet07AkenoCASA-MIAHEGRAFly’s EyeKascadeKascade Grande 2011AGASAHiRes 1HiRes 2Telescope Array 2011Auger 2011
Knee
Ankle
Cre
dit:
Part
icle
Dat
a G
Rou
p (2
011)
Galactic cosmic rays
Extra-Galactic cosmic rays
Transition region
CERN
LHC (
14 TeV
)
Motivations
[eV]E1310 1410 1510 1610 1710 1810 1910 2010
]-1
sr-1 s
-2 m
1.6
[GeV
F(E)
2.6
E
1
10
210
310
410GrigorovJACEEMGUTien-ShanTibet07AkenoCASA-MIAHEGRAFly’s EyeKascadeKascade Grande 2011AGASAHiRes 1HiRes 2Telescope Array 2011Auger 2011
Knee
Ankle
Cre
dit:
Part
icle
Dat
a G
Rou
p (2
011)
Galactic cosmic rays
Extra-Galactic cosmic rays
Transition region
CERN
LHC (
14 TeV
)
Motivations
[eV]E1310 1410 1510 1610 1710 1810 1910 2010
]-1
sr-1 s
-2 m
1.6
[GeV
F(E)
2.6
E
1
10
210
310
410GrigorovJACEEMGUTien-ShanTibet07AkenoCASA-MIAHEGRAFly’s EyeKascadeKascade Grande 2011AGASAHiRes 1HiRes 2Telescope Array 2011Auger 2011
Knee
Ankle
Cre
dit:
Part
icle
Dat
a G
Rou
p (2
011)
Galactic cosmic rays
Extra-Galactic cosmic rays
Transition region
CERN
LHC (
14 TeV
)
MotivationsNew era of observations
Credit: L.fabre/CEA, 2006
Credit: G. Perez, SMM, IAC
Credit: IceCube/NSF
Credit: S. Saffi
all the already existing & coming telescopes & satellites!
+
Design of the model
Lepto-hadronic jet model
Design of the model
Lepto-hadronic jet model
Design of the model
Lepto-hadronic jet modelz
Design of the model
Lepto-hadronic jet modelz
𝜽
Design of the model
Lepto-hadronic jet model
Design of the model
e e
ee
e
ee
e
e
p
p
p
p
Lepto-hadronic jet model
p
Design of the model
shock
e e
ee
e
ee
e
e
p
p
p
p
Lepto-hadronic jet model
p
Design of the model
Maxwel l ian d istr ibut ion below shock
shock
e e
ee
e
ee
e
e
p
p
p
p
Lepto-hadronic jet model
Thermal particles
p
Design of the model
Maxwel l ian d istr ibut ion below shockMaxwel l ian + power- law distr ibut ion above shock
shock
e e
ee
e
ee
e
e
p
p
p
p
Lepto-hadronic jet model
Thermal particles
Non-thermal particles
p
Design of the model
Maxwel l ian d istr ibut ion below shockMaxwel l ian + power- law distr ibut ion above shockLeptonic radiat ive processes inc ludes : shock
e e
ee
e
ee
e
e
p
p
p
p
Lepto-hadronic jet model
Thermal particles
Non-thermal particles
p
Design of the model
Maxwel l ian d istr ibut ion below shockMaxwel l ian + power- law distr ibut ion above shockLeptonic radiat ive processes inc ludes :synchroton se l f -absorpted
Synch
shock
e e
ee
e
ee
e
e
p
p
p
p
Lepto-hadronic jet model
Thermal particles
Non-thermal particles
p
Design of the model
Maxwel l ian d istr ibut ion below shockMaxwel l ian + power- law distr ibut ion above shockLeptonic radiat ive processes inc ludes :synchroton se l f -absorptedsynchrotron se l f - & externa l - Compton
Synch
ICshock
e e
ee
e
ee
e
e
p
p
p
p
Lepto-hadronic jet model
Thermal particles
Non-thermal particles
IC
p
Design of the model
Lepto-hadronic jet model
Synch
ICshock
IC
e e
ee
e
ee
e
e
p
p
p
p
p Thermal particles
Non-thermal particles
Design of the model
Lepto-hadronic jet model
Synch
ICshock
IC
e e
ee
e
ee
e
e
p
p
p
p
p Thermal particles
Non-thermal particles
Hadronic radiat ive processes inc ludes :
Design of the model
Lepto-hadronic jet model
Synch
ICshock
IC
e e
ee
e
ee
e
e
p
p
p
p
p Thermal particles
Non-thermal particles
Hadronic radiat ive processes inc ludes :proton-protonproton-photon
Design of the model
Lepto-hadronic jet model
Synch
ICshock
Gamma-ray
IC
Gamma-rayneutrinos
e e
ee
e
ee
e
e
p
p
p
p
p
Hadronic radiat ive processes inc ludes :proton-protonproton-photonModels emiss ion from Radio to Gamma-ray & neutr inos
X-ray
Radio
Lepto-hadronic jet model
Assumption of the model
Mult i -zone jet
Lepto-hadronic jet model
Assumption of the model
Mult i -zone jetSteady-state treatment of the par t ic le d istr ibut ions
Lepto-hadronic jet model
Assumption of the model
Mult i -zone jetSteady-state treatment of the par t ic le d istr ibut ionsLeptonic par t based on Markof f+2005 & Maitra+2009
Lepto-hadronic jet model
Assumption of the model
Lepto-hadronic jet model
Assumption of the model
Proton-proton interact ion:
Lepto-hadronic jet model
Assumption of the model
Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008
Lepto-hadronic jet model
Assumption of the model
Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:
Lepto-hadronic jet model
Assumption of the model
Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:Kelner&Aharonian 2008
Lepto-hadronic jet model
Assumption of the model
Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:Kelner&Aharonian 2008D
Lepto-hadronic jet model
Assumption of the model
Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:Kelner&Aharonian 2008DAccelerat ion & cool ing rates from Begelman+1990
Lepto-hadronic jet model
Assumption of the model
Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:Kelner&Aharonian 2008DAccelerat ion & cool ing rates from Begelman+1990
Lepto-hadronic jet model
Assumption of the model
One major modi f icat ion: steady-state d istr ibut ion of secondar ies e± to ca lcu late their synchrotron and IC scatter ing radiat ion (Ginzburg&Syrovatsk i i 1964)
Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:Kelner&Aharonian 2008DAccelerat ion & cool ing rates from Begelman+1990
Lepto-hadronic jet model
Assumption of the model
One major modi f icat ion: steady-state d istr ibut ion of secondar ies e± to ca lcu late their synchrotron and IC scatter ing radiat ion (Ginzburg&Syrovatsk i i 1964)Model of ste l lar wind (Lamers&Cass ine l l i 1999)
-6
-4
-2
0
2
4
8 10 12 14 16 18 20 22 24 26 28
Flu
x [
mJy
]
ν [Hz]
Black body [star+disc]Synchrotron [thermal]
Synchrotron [non-thermal]Inverse-Compton
Proton-protonSynchrotron [secondary electron]
Total emissionRyle/15GHz
IRS/MIR
RXTE/X-ray
IBIS/γ-ray
Preliminary results
Drappeau et al. (in prep.)
Cyg X-1
6 8 10 12 14
E� [eV]
16
17
18
19
20
21
22
Flu
x[e
rg/c
m2/
s]
Work in progress! neutrinophoton
log(
)
log( )
log( )
log(
)
-6
-4
-2
0
2
4
8 10 12 14 16 18 20 22 24 26 28
Flu
x [
mJy
]
ν [Hz]
Black body [star+disc]Synchrotron [thermal]
Synchrotron [non-thermal]Inverse-Compton
Proton-protonSynchrotron [secondary electron]
Total emissionRyle/15GHz
IRS/MIR
RXTE/X-ray
IBIS/γ-ray
Preliminary results
Drappeau et al. (in prep.)
Cyg X-1
6 8 10 12 14
E� [eV]
16
17
18
19
20
21
22
Flu
x[e
rg/c
m2/
s]
Work in progress! neutrinophoton
log(
)
log( )
log( )
log(
)
-6
-4
-2
0
2
4
8 10 12 14 16 18 20 22 24 26 28
Flu
x [
mJy
]
ν [Hz]
Black body [star+disc]Synchrotron [thermal]
Synchrotron [non-thermal]Inverse-Compton
Proton-protonSynchrotron [secondary electron]
Total emissionRyle/15GHz
IRS/MIR
RXTE/X-ray
IBIS/γ-ray
Preliminary results
Drappeau et al. (in prep.)
Cyg X-1
6 8 10 12 14
E� [eV]
16
17
18
19
20
21
22
Flu
x[e
rg/c
m2/
s]
Work in progress! neutrinophoton
log(
)
log( )
log( )
log(
)
-6
-4
-2
0
2
4
8 10 12 14 16 18 20 22 24 26 28
Flu
x [
mJy
]
ν [Hz]
Black body [star+disc]Synchrotron [thermal]
Synchrotron [non-thermal]Inverse-Compton
Proton-protonSynchrotron [secondary electron]
Total emissionRyle/15GHz
IRS/MIR
RXTE/X-ray
IBIS/γ-ray
Preliminary results
Drappeau et al. (in prep.)
Cyg X-1
6 8 10 12 14
E� [eV]
16
17
18
19
20
21
22
Flu
x[e
rg/c
m2/
s]
Work in progress! neutrinophoton
log(
)
log( )
log( )
log(
)
-6
-4
-2
0
2
4
8 10 12 14 16 18 20 22 24 26 28
Flu
x [
mJy
]
ν [Hz]
Black body [star+disc]Synchrotron [thermal]
Synchrotron [non-thermal]Inverse-Compton
Proton-protonSynchrotron [secondary electron]
Total emissionRyle/15GHz
IRS/MIR
RXTE/X-ray
IBIS/γ-ray
Preliminary results
Drappeau et al. (in prep.)
Cyg X-1
6 8 10 12 14
E� [eV]
16
17
18
19
20
21
22
Flu
x[e
rg/c
m2/
s]
Work in progress! neutrinophoton
log(
)
log( )
log( )
log(
)
-6
-4
-2
0
2
4
8 10 12 14 16 18 20 22 24 26 28
Flu
x [
mJy
]
ν [Hz]
Black body [star+disc]Synchrotron [thermal]
Synchrotron [non-thermal]Inverse-Compton
Proton-protonSynchrotron [secondary electron]
Total emissionRyle/15GHz
IRS/MIR
RXTE/X-ray
IBIS/γ-ray
Preliminary results
Drappeau et al. (in prep.)
Cyg X-1
p
6 8 10 12 14
E� [eV]
16
17
18
19
20
21
22
Flu
x[e
rg/c
m2/
s]
Work in progress! neutrinophoton
log(
)
log( )
log( )
log(
)
-6
-4
-2
0
2
4
8 10 12 14 16 18 20 22 24 26 28
Flu
x [
mJy
]
ν [Hz]
Black body [star+disc]Synchrotron [thermal]
Synchrotron [non-thermal]Inverse-Compton
Proton-protonSynchrotron [secondary electron]
Total emissionRyle/15GHz
IRS/MIR
RXTE/X-ray
IBIS/γ-ray
Preliminary results
Drappeau et al. (in prep.)
Cyg X-1
p
6 8 10 12 14
E� [eV]
16
17
18
19
20
21
22
Flu
x[e
rg/c
m2/
s]
Correlated
Work in progress! neutrinophoton
log(
)
log( )
log( )
log(
)
What the model offersExamples
What the model offers
Help to. . .. . . choose promis ing sources
Examples
What the model offers
Help to. . .. . . choose promis ing sources
. . . s tudy recurr ing f lar ing events of gamma-rays and neutr inos
Examples
What the model offers
Help to. . .. . . choose promis ing sources
. . . s tudy recurr ing f lar ing events of gamma-rays and neutr inos
. . .better constra in gamma-ray and neutr ino background s igna l from astrophys ica l sources in the Dark Matter annih i lat ion
Examples
Next stepsBetter treatment of the neutrino signal
open to collaboration with the neutrino community!
Complete the radiative processes modelling
pair production/annihilation, synchrotron from proton and secondaries,…
Quid of nuclei acceleration in jet? (AUGER results)
Development of a time-dependant version
variability-triggered internal shocks
Internal shocks driven by accretion flow variability
Ref: • Malzac 2013, 2014 • Drappeau et al. subm.
Internal shocks driven by accretion flow variability
Fluctuation of jet’s bulk Lorentz factor
Ref: • Malzac 2013, 2014 • Drappeau et al. subm.
Internal shocks driven by accretion flow variability
�3.0 �2.5 �2.0 �1.5 �1.0 �0.5 0.0 0.5 1.0
log(f [Hz])
�3.0
�2.5
�2.0
�1.5
log(f
⇥Pow
er[(rm
s/m
ean)2
])
Fluctuation of jet’s bulk Lorentz factor
Ref: • Malzac 2013, 2014 • Drappeau et al. subm.
Internal shocks driven by accretion flow variability
�3.0 �2.5 �2.0 �1.5 �1.0 �0.5 0.0 0.5 1.0
log(f [Hz])
�3.0
�2.5
�2.0
�1.5
log(f
⇥Pow
er[(
rms/
mea
n)2
])
GX 339-4
X-ray PSD
Fluctuation of jet’s bulk Lorentz factor
Ref: • Malzac 2013, 2014 • Drappeau et al. subm.
8 10 12 14 16 18
log(⌫ [Hz])
�2.0
�1.5
�1.0
�0.5
0.0
0.5
1.0
1.5
2.0
2.5
log(
F⌫
[mJy
])
Drappeau et al. submitted
Radio WISE - MIR NIR- OUV X-ray
W1W2
W3W4
GX 339-4
Photon Spectra
Internal shocks driven by accretion flow variability
Fnu [mJy] Fvar
simulation WISE simulation WISE
W1 56.07 55.2 ± 3.9 0.24 0.25 ± 0.03
W2 63.87 64.3 ± 4.6 0.25 0.25 ± 0.03
W3 82.38 79.9 ±7.3 0.31 0.32 ± 0.06
W4 89.15 87.4 ± 8.3 0.38 0.32 ± 0.06
Dra
ppea
u et
al.
subm
itted
0 2 4 6 8 10
time [arbitrary units]
10�1
100
101
102
Flu
xden
sity
F⌫
[mJy]
W4/2
W3/10
W2/50
W1/200
GX 339-4Simulated light curves
Internal shocks driven by accretion flow variability
Take-away points
We propose an multi-wavelength and multi-messenger spectral jet model
Prepare the future of radio to gamma-ray + neutrinos analyses of accreting black holes at all scales
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