simulations of astrophysical jets
DESCRIPTION
SIMULATIONS OF ASTROPHYSICAL JETS. Gianluigi Bodo, Claudio Zanni, Attilio Ferrari, Silvano Massaglia, A. Mignone, P. Rossi INAF - Osservatorio Astronomico di Torino Università di Torino. Collimated, supersonic outflows (jets) are generated in many astrophysical environments. AGN. pulsars. - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/1.jpg)
SIMULATIONS OF SIMULATIONS OF
ASTROPHYSICAL JETSASTROPHYSICAL JETS
Gianluigi Bodo, Claudio Zanni, Attilio Ferrari, Gianluigi Bodo, Claudio Zanni, Attilio Ferrari, Silvano Massaglia, A. Mignone, P. RossiSilvano Massaglia, A. Mignone, P. Rossi
INAF - Osservatorio Astronomico di TorinoINAF - Osservatorio Astronomico di Torino
Università di Torino Università di Torino
![Page 2: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/2.jpg)
Collimated, supersonic outflows (jets)are generated in many astrophysicalenvironments
AGN
YSOX-ray transients
pulsars
![Page 3: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/3.jpg)
Wide range of scales and velocities
Scales from below the pc up to Mpc
Highly relativistic velocities (AGN, GRB)
Mildly relativistic velocities (X-ray transients – galactic superluminals, SS433)
Few hundreds km/s (YSO)
![Page 4: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/4.jpg)
YSO jets HST images HH 30
1"10''
![Page 5: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/5.jpg)
AGN Jets
Scales up to MpcNon-thermal synchrotron radiationCollimation angle can be few degrees
Observed at differentenergies
time scales 10 yrs7
![Page 6: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/6.jpg)
• Launching Launching phase: acceleration fromdisk and collimation• Propagation Propagation phase: confinement,stability, entrainment• Termination Termination: interaction with external medium
BASIC PROBLEMS
![Page 7: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/7.jpg)
THE TOOL: PLUTO OUTLINE• Explicit, compressible code (FV):
– Shock capturing– High-mach number flows
• Works in 1, 2, 3-D• Modular structure:
– Physics– Time stepping– Interpolations– Riemann Solvers
• HD, MHD, RHD (Mignone, Plewa, Bodo 2005, HLLC Mignone & Bodo 2005) , RMHD (HLLC Mignone & Bodo 2005)
• Geometry support (Cart, Cyl, Spher)• Radiative losses
![Page 8: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/8.jpg)
Algorithms
Time Stepping
Fwd Euler (Split/Unsplit) RK 2nd (Split/Unsplit) RK 3rd (Split/Unsplit) Hancock (Split/CTU) Characteristic Tracing
(Split/CTU)
Interpolation Prim. TVD-limited (II order) Characteristic TVD-limited Piecewise-Parabolic Multi-D Linear Interpolation 2nd and 3rd order WENO
Riemann Solvers Riemann (non-linear)
TVD/ROE HLL HLLC TVDLF
(split) (split)
HD RHD MHD RMHD
![Page 9: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/9.jpg)
Stability of jets
Kelvin-Helmholtz instability
Transfer of momentum, entrainment
Effects on the jet evolution
Consider first a simple case, simple planar shearlayer
Velocity profileVx = tanh y
AGN: relativistic case
![Page 10: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/10.jpg)
Linear stability: different regimes depending on the Mach number, monotonic instability at low Mach, overstability at high Mach
Nonlinear evolution dominated by vortices or by waves
![Page 11: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/11.jpg)
Layer width velocity Layer width tracer
Relativistic cases: correspondence at equal Mr = v/s cs
we showed in linear analysis (Bodo, Mignone & Rosner 2004)that the stability limits (vortex sheet) are the same if expressed in Mr
We introduced a tracer passively advected to distinguish the material on the two sides
![Page 12: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/12.jpg)
![Page 13: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/13.jpg)
JET STABILITYJET STABILITY
Linear phase
Acousticphase
Mixingphase
Bodo et al. 1998
![Page 14: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/14.jpg)
Fanaroff-Riley classificationFanaroff-Riley classification
FR II or lobe dominated “classical doubles”
FR I or jet dominated
Cygnus AVLA
3C 449VLA
![Page 15: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/15.jpg)
Jet velocitiesNo direct velocity measures Evidences for relativistic motions on pc scale come from:
Superluminal motions
Jet one-sidedness
Rapid variabilities
High brightness temperatures
![Page 16: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/16.jpg)
In FRI radiosources jets on kpc scale become symmetric
Brightness ratio between jetand counterjet in 3C31
3C272.1
VLBI one-sided jet VLA
![Page 17: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/17.jpg)
AGN jets: deceleration of FRI jets
Mass entrainment
Injection from stellar winds (Komissarov 1994; Bowman, Leahy, Komissarov 1996)
Entrainment through the instability evolution
Simulations of a propagating jet perturbedat the inlet
![Page 18: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/18.jpg)
Physical parameters
j j
e
Jet Mach number
Lorentz factor
Density ratio
![Page 19: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/19.jpg)
Mach 3, 30Density ratio (lab frame) 10 1000Lorentz factor 10
Low resolution 12 points over radiusHigh resolution 25 points over radius
Stretched grid in the transverse directionIncreasing grid size
Parameters values
![Page 20: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/20.jpg)
3D Numerical Simulation 3D Numerical Simulation
Grid: 300x800x300
Jet injection+perturbation
outflow
outflow
outflow
![Page 21: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/21.jpg)
1) M=3 =1000 =10 t=760
![Page 22: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/22.jpg)
1)
The entrainment is mediated by the cocoon
![Page 23: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/23.jpg)
M=30 =10 =10 t=265
![Page 24: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/24.jpg)
1)
2)
![Page 25: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/25.jpg)
1) M=3 =1000 =10 t=760
2) M=30 =10 =10 t=265
Faster decelerationStrong pinching due to high pressure cocoonShort wavelength mode more efficient for entrainment
Helical mode
![Page 26: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/26.jpg)
Jet mass External mass
Jet mass
External mass
![Page 27: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/27.jpg)
![Page 28: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/28.jpg)
Jet-IGM interaction from the point of view of IGM
Observational consequences of the interaction: X-ray observations
From the observations can we deduce information on jet parameters?
Heating of IGM
![Page 29: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/29.jpg)
CHANDRA
HYDRA A X-RAY
HYDRA AX - RADIO
![Page 30: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/30.jpg)
CHANDRA
Perseus AX - radio
Perseus A X-ray
![Page 31: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/31.jpg)
OBSERVATIONS
X-ray cavities corresponding to radio lobes Shells surrounding the cavities Shell temperature equal or lower than the surrounding medium
Weak shocks
![Page 32: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/32.jpg)
L-T relation for cluster gas
![Page 33: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/33.jpg)
NUMERICAL SIMULATIONS
reflecting
outflow
outflow
refl
ecti
ng
0 2.6
2.6Initial density distribution
Uniform temperature
1024x1024 grid points
Jet inlet
![Page 34: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/34.jpg)
UNITS
![Page 35: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/35.jpg)
RESULTS
![Page 36: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/36.jpg)
![Page 37: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/37.jpg)
M
Subsonic jet lc = 0.5
lc = 1lc = 2
Strongly overpressured
Weakly overpressured
![Page 38: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/38.jpg)
Similar setup as before
Larger grid, Longer integration times,longer than the lifetime of the radiosource
Three cases withcluster of different scales:
T 0.5 keV 1 keV 2 keV
![Page 39: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/39.jpg)
Entropy and dissipated energyEntropy and dissipated energy
Efficiency Efficiency Borgani et al. (2002)Borgani et al. (2002)
![Page 40: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/40.jpg)
Hydrostatic equilibriumHydrostatic equilibrium
Lloyd-Davies et al. (2000)Lloyd-Davies et al. (2000)
![Page 41: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/41.jpg)
L-T relationL-T relation
Entropy per particleEntropy per particle(at )(at )
First stage, future: insert heatingat z > 0 on protoclusters and follow the evolution with a cosmological simulation
![Page 42: SIMULATIONS OF ASTROPHYSICAL JETS](https://reader036.vdocuments.mx/reader036/viewer/2022062410/568159df550346895dc72a57/html5/thumbnails/42.jpg)
Summary
Single shear KH instability
Deceleration of relativistic jets
Heating of external medium by jets