Relativistic jets in the

computer lab: long-term

evolution and dynamics

Manel Perucho-Pla Departament d'Astronomia i Astrofísica

extragalactic jets

NGC4261

Jets are relativistic, as indicated by superluminal motion at pc scales and one-

sidedness of pc scale jets (due to Doppler boosting of the emitted radiation).

The production of jets is connected with the process of

accretion on supermassive black holes at the core of

Active Galactic Nuclei.

Emission: synchrotron (from radio to X-rays) and inverse Compton (-ray

emission) from a relativistic (e+/e-, ep) jet.

Carilli

A. Bridle’s gallery

FRII FRI

jet power

AGN

extragalactic jets

~20 sources with detected jets in the Galaxy.

SS 433

Migliari et al.

Cygnus X-1 Gallo et al. 2005

S6 in NGC 7793 Pakull et al., Soria et al. 2010 MICROQUASARS

relativistic jets in our Galaxy

22/10/11 5

Relativistic hydrodynamics: SRHD equations

Rorb ~ 2.e12 cm

6.e10 cm ~ 0.004 AU

2.e12 cm ~ 0.13 AU

wind from the star

6.e11 cm ~ 0.04 AU

y

x z

Image: NASA/ESA

wind-jet interaction in HMXB

Perucho, Bosch-Ramon & Khangulyan 2010

t = 977 s

t = 192 s

Pj = 3.e36erg/s

Pj = 1.e37erg/s

wind-jet interaction in HMXB

Pj = 3.e36 erg/s Pj = 1.e37 erg/s

clumpy stellar winds in HMXB

Perucho & Bosch-Ramon, A&A submitted 650 khr. 200 processors/simulation with Ratpenat

wind-jet interaction in HMXB

HIGHLIGHTS The interaction produces candidate sites for the production of very-high energy radiation that has already been detected by several instruments: INTEGRAL, Suzaku and AGILE (Moldón et al. 2008, Malzac et al. 2008, Hoffmann et al. 2009, Takahashi et al. 2009, Zdziarski et al. 2009, Sabatini et al. 2010, Koljonen 2010, Zabalza et al. 2011). The statistics of high-mass microquasars predict 10 (unobserved) objects in our Galaxy with jet power in the range of 1.e35 to 1.e38 erg/s, i.e., jets that could be possibly disrupted by the interaction with the strong wind from the companion star.

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MS0735+7421 (McNamara et al. 2005).

200 kpc diameter cavities.

Shock-wave (M=1.4).

PV=1.e61 erg.

T=1.e8 yr.

Ps=1.7e47 erg/s.

long-term evolution of extragalactic jets

• 2D axisymmetric hydro simulations with Ratpenat using

up to 140 processors (added as the jet grows) during

months... ≈1.e6 computational hours for the whole project. • Resolution: 50x50 pc or 100x100 pc per cell in the central region

(Total 16000x2000 cells, 800 /900 kpc x 500 kpc).

1.e46 erg/s

200 Myr

long-term evolution of extragalactic jets

time

1.e46 erg/s

200 Myr

Perucho, Quilis, Martí 2011, ApJ, accepted

long-term evolution of extragalactic jets

X-ray morphology

MS0735+7421 (McNamara et al.).

>1.e11 MΘ of shocked ambient

gas.

Red: ambient.

Blue: jet.

M≈30

Our parameters

(consistent)

Vbs= 0.044 – 0.1 c

Mbs= 10 – 30

Usual parameters in

newtonian simulations Vbs= 0.009 – 0.015 c

Mbs= 3 – 5

Martí et al. (1997)

Perucho, Quilis, Martí 2011, ApJ, accepted

long-term evolution of extragalactic jets

HIGHLIGHTS Consistent numerical simulations show that heating by powerful AGN jets may occur mainly through shock heating. Heating by AGN jets is extremely efficient and fast: Up to 95 % or even more goes into the ambient medium via shock and mixing (≈ 1%). Heating by mixing, and buoyant cavities can be important when the shocks disappear:

extremeley old sources. low-power AGN jets.

The distance up to which the energy is deposited depends on the jet power and ambient properties.

long-term evolution of extragalactic jets

Schlieren plot: enhanced density gradients.

1.e46 erg/s

long-term evolution of extragalactic jets

1.e44 erg/s

long-term evolution of extragalactic jets