synthetic x-ray and radio observations of simulated jets: insights and opportunities
DESCRIPTION
Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities. I. L. Tregillis (LANL / U of MN) T. W. Jones (U of MN) Dongsu Ryu (Chungnam Natl. Univ.). X-ray and Radio Connections February 5, 2004. Overview. Introduction: A new approach - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/1.jpg)
Synthetic X-Ray and Radio Observations of Simulated Jets:
Insights and Opportunities
I. L. Tregillis (LANL / U of MN)
T. W. Jones (U of MN)
Dongsu Ryu (Chungnam Natl. Univ.)
X-ray and Radio ConnectionsFebruary 5, 2004
![Page 2: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/2.jpg)
Overview
Introduction: A new approach Background: The simulations Opportunities: Synthetic Observations
– What, Why, How?
Insights– Dynamics– Field properties– Energy partitioning
Conclusion: Opportunities
![Page 3: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/3.jpg)
Introduction: A New Approach
Self-consistent acceleration and transport of cosmic ray (CR) electrons within 3D MHD jet simulations
Synthetic synchrotron radio and inverse-Compton X-ray observations (IC/3K, SSC)
Standard observational analyses– Tregillis et al. ApJ, v601 n2 February 1 2004
The fun part: – Do we recover accurate source properties?
![Page 4: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/4.jpg)
Our Approach to CR Transport(Jones et al. ApJ, 512, 105)
Physical scales for acceleration << dynamical scales
Broad electron distribution f(p) enables “finite volume” approach in momentum space:
Use test-particle model for fast Fermi acceleration at shocks
Solve kinetic equation for downstream transport
p
pq
pf
i
i
q
n
i
i
iii
2/1
2/113
4
33
2/12/1
2
3
1
3 q
r
rq
2/1
2/1|3
023
14
i
i
pp
s
i fpp
p
p
qDu
dt
dn
![Page 5: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/5.jpg)
One Jet…(Tregillis et al. ApJ, 557, 475)
Light, supersonic (nonrelativistic) 3D MHD jet Mj=8, =j/a=0.01; pressure matched in
uniform background Helical magnetic field; 0 = 100 on axis Symmetry broken with 5o precession 15 zones across jet core for accurate shock
identification
![Page 6: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/6.jpg)
…Three Scenarios(Tregillis et al. ApJ, 557, 475)
Model 1: “Control”– No injection of fresh particles at shocks– Negligible radiative aging
Model 2: “Injection”– Minimal CR population carried down jet– Fraction (=10-4) of thermal electron flux “injected” at shocks
Model 3: “Cooling”– Radiative lifetime for 5 GeV electrons ~ simulation duration– Spectra experience considerable aging
![Page 7: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/7.jpg)
Particles…
![Page 8: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/8.jpg)
…and Fields
![Page 9: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/9.jpg)
Synthetic Observations
Particles
+ j
Fields
Synthetically-observable quantities include:Radio synchrotron surface brightness and spectral indexIC/3K and SSC X-ray surface brightnessRadio polarimetry (Stokes Q, U); Faraday rotation & RM
![Page 10: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/10.jpg)
Example:Radio Surface Brightness, 1.4 GHz
Injection Cooling
![Page 11: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/11.jpg)
Combined Observations (finally):Dynamical Insights(Tregillis et al. ApJ February 1, 2004)
IIC/3K ISm ; m = 1/3 – 1/2
Is neDB1+~ 0.5 - 1.0IIC/3K neD B ne
b
Compression (tangled) : B 2/3 m ~ 0.5 – 0.43Perpendicular shocks: B m ~ 0.4 – 0.33
![Page 12: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/12.jpg)
Dynamical Insights, continued(Tregillis et al. ApJ February 1, 2004)
ISSC ISm ; m = 1/3 – 1/2
ISSC ISm ; m = 1.0 – 1.5
Locally dominated radiation field: IS m ~ 1.47 ( ~ 0.65)
![Page 13: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/13.jpg)
Combined Observations:Magnetic Field Strengths
)(
)(1009.21006.11
14113
0
01
xic
rs
x
r
a
BC
ic I
Iz
j
jB
7/22/1
12/1
2
0
02/3
35
2/1
)(
sin
)1(11069.5
F
l
zkB
yxme
Radio:
Radio & X-ray:
![Page 14: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/14.jpg)
The Gritty Reality…
![Page 15: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/15.jpg)
…and Derived Values
![Page 16: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/16.jpg)
Combined Observations:Energy Partitioning
kdB
Bd
U
Ud
meE
B
1
4
3; min
2/7
min
•Bme is inferred from the radio emission•B is the true field value in the ideal case •So, if Bic is a useful estimator of B, why not…
Replace B with Bic and get a direct estimate of d?
![Page 17: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/17.jpg)
Best Case Scenario: High Degree of Uniformity
d Control Injection Cooling
Initial Conditions
1.6 x 10-1 1.6 x 103 1.6 x 10-1
Derived from Bic and Bme
1.7 x 10-1 1.2 x 103 9.2 x 10-2
We know d exactly at the base of the jet…
![Page 18: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/18.jpg)
More Gritty Reality
![Page 19: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/19.jpg)
…and More Derived Values
![Page 20: Synthetic X-Ray and Radio Observations of Simulated Jets: Insights and Opportunities](https://reader036.vdocuments.net/reader036/viewer/2022062517/5681303b550346895d95d3a1/html5/thumbnails/20.jpg)
Conclusions & Future Work
Combined synthetic X-ray and radio observations of simulated jets reveal:
•Dominant dynamical and transport effects •Good estimates for local field strengths•Direct, independent estimates for the energy partitioning
All of this information is crucial groundwork for understanding the long-term evolution and dissipation of extragalactic jets on cosmological scales.