A multi-wavelength and multi-messenger spectral model for ...

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

)

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 modelz

Design of the model

Lepto-hadronic jet modelz

𝜽

Design of the model


Design of the model

e e

ee

e

ee

e

e

p

p

p

p


p

Design of the model

shock

e e

ee

e

ee

e

e

p

p

p

p


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


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


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


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


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


Thermal particles


IC

p

Design of the model


Synch

ICshock

IC

e e

ee

e

ee

e

e

p

p

p

p

p Thermal particles


Design of the model


Synch

ICshock

IC

e e

ee

e

ee

e

e

p

p

p

p

p Thermal particles


Hadronic radiat ive processes inc ludes :

Design of the model


Synch

ICshock

IC

e e

ee

e

ee

e

e

p

p

p

p

p Thermal particles


Hadronic radiat ive processes inc ludes :proton-protonproton-photon

Design of the 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


Assumption of the model

Mult i -zone jet



Mult i -zone jetSteady-state treatment of the par t ic le d istr ibut ions



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



Proton-proton interact ion:



Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008



Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:



Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:Kelner&Aharonian 2008



Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:Kelner&Aharonian 2008D



Proton-proton interact ion:Kamae+2006,Kar lsson&Kamae 2008Proton-photon interat ion:Kelner&Aharonian 2008DAccelerat ion & cool ing rates from Begelman+1990






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)




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]





IRS/MIR

RXTE/X-ray

IBIS/γ-ray

Preliminary results


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]


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]





IRS/MIR

RXTE/X-ray

IBIS/γ-ray

Preliminary results


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


log(

)

log( )

log( )

log(

)

What the model offersExamples

What the model offers

Help to. . .. . . choose promis ing sources

Examples



. . . s tudy recurr ing f lar ing events of gamma-rays and neutr inos

Examples



. . . 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.


Fluctuation of jet’s bulk Lorentz factor



�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

])




�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



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


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


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

A multi-wavelength and multi-messenger spectral model for ...

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