Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S....
-
date post
21-Dec-2015 -
Category
Documents
-
view
214 -
download
1
Transcript of Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S....
![Page 1: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/1.jpg)
Cosmological MHDHui Li
Collaborators:
S. Li, M. Nakamura, S. Diehl, B. Oshea,
P. Kronberg, S. Colgate (LANL)
H. Xu, M. Norman (UCSD), R. Cen (Princeton)
Observational overview of large scale magnetic fields Several examples of numerical modeling of cosmological MHD
![Page 2: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/2.jpg)
Part I:
Observations
![Page 3: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/3.jpg)
Hydra A
Galaxy Clusters
MS0735.6+7421
![Page 4: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/4.jpg)
Cluster RadioHalo
A754Kassim et al. ‘01
![Page 5: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/5.jpg)
Bachigi et al. 2006, Science
Cluster Accretion Shocks (?)
![Page 6: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/6.jpg)
Beyond Clusters…. (???)
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Kronberg et al. 2007, ApJ
![Page 7: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/7.jpg)
Part II:
Origin of Extra-Galactic Magnetic Fields
![Page 8: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/8.jpg)
Numerical simulations- cold dark matter cosmology = 0.73, DM = 0.27, gas = 0.043, h=0.7, n = 1, 8 = 0.8 without/with gas cooling- computational box: (100h-1 Mpc)3
10243 cells for gas and gravity, 5123 DM particles, x = 97.7 h-1kpc
Ryu et al. 2005
= 1 – 104 <> and higher
Baryon DensityVorticity Generation
![Page 9: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/9.jpg)
Cosmic Energy Flow
Gravity
Stars, galaxies, galaxy clusters,
large scale shocks, etc.
IGM
“Feedback”MechanicalChemicalThermal
Non-ThermalMagnetic
collapse
Black Holes
RadiationKinetic WindsMagnetic fields
108 Msun 1062 ergs
![Page 10: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/10.jpg)
Part III:
Astrophysical Jet Modeling and Interaction with ICM
![Page 11: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/11.jpg)
“flux core: & Iz”(“helix/jet”)
toroidal Bfrom Iz(“lobes”)
confinement(B2
/8 ~ pgas)
Jz @ t = 10global current flow
(Li et al. 2006, Nakamura, Li, Li 2006, 2007)
![Page 12: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/12.jpg)
Hydra A
Diehl, Li, et al. 2007
![Page 13: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/13.jpg)
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Zavala & Taylor 20053C273
Differential FRM
Is there current in jets?
![Page 14: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/14.jpg)
Part IV:
Magnetic Fields Injected from SMBHs
![Page 15: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/15.jpg)
Growing “cherries” on cosmic trees …
Mpc/(1+z)Johnson et al. in preparation
z=2
![Page 16: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/16.jpg)
Mpc/(1+z)
B=0.1 G
Li et al. 2007
![Page 17: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/17.jpg)
Part V:
Cosmological MHD Simulation of Cluster
formation with Magnetic Fields
![Page 18: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/18.jpg)
AMR MHD Cluster Formation Simulations
Same simulation with radiactive cooling, star formation and star formation feedback, uniform initial magnetic fields of 1e-9 G in y direction.
Projected logarithmic baryon density, refined to level 2,4,6 and 8. Each plot has a resolution of 512x512 zones. Best spatial resolution is 7.8125kpc/h
256Mpc/
h4M
pc/h
ΛCMD model, Ω=1, ΩΛ=0.7, Ωb =0.04, h=0.7,and box size = 256 Mpc. Root grid is 1283,refined by 2 to level 8, simulation is from z=30 to z=0.
![Page 19: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/19.jpg)
Magnetic Energy Density Evolution
256Mpc/
h
4Mpc/h
![Page 20: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/20.jpg)
SZ Effect: y-parameter
256Mpc/
h
4Mpc/h
![Page 21: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/21.jpg)
AMR MHD Cluster Formation SimulationsImagines of cluster center(1Mpc/h)
Gas density SZ_y
Magnetic energy density Rotation measurement
![Page 22: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/22.jpg)
AMR MHD Cluster Formation SimulationsΛCMD model, Ω=1, ΩΛ=0.7, Ωb =0.04, h=0.7,and box size = 256 Mpc/h. Root grid is 1283,refined by 2 to level 8, simulation is from z=30 to z=0. No initial magnetic fields
Imagines of projected baryon density of inner 4 Mpc/h at z=0, left is from MHD solver and right is from ppm solver
![Page 23: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/23.jpg)
AMR MHD Cluster Formation SimulationsΛCMD model, Ω=1, ΩΛ=0.7, Ωb =0.04, h=0.7,and box size = 256 Mpc/h. Root grid is 1283,refined by 2 to level 8, simulation is from z=30 to z=0. No initial magnetic fields
Y parameter of SZ Effect of slice of inner 4 Mpc/h at z=0, left is from MHD solver and right is from ppm solver
![Page 24: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/24.jpg)
AMR MHD Cluster Formation SimulationsΛCMD model, Ω=1, ΩΛ=0.7, Ωb =0.04, h=0.7,and box size = 256 Mpc/h. Root grid is 1283,refined by 2 to level 8, simulation is from z=30 to z=0. No initial magnetic fields
X-ray luminosity of of inner 4 Mpc/h at z=0, left is from MHD solver and right is from ppm solver
![Page 25: Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)](https://reader030.fdocuments.in/reader030/viewer/2022032704/56649d6b5503460f94a4b11d/html5/thumbnails/25.jpg)
Some Key Problems1. Diffused Radio Emission: Distribution and strength of
cosmic magnetic fields, seeding from first stars, dwarf galaxies, AGN feedbacks, or (turbulent) dynamo.
2. Differential FRM of jet pc-kpc scale: is there current?3. Clusters as magnetic field laboratories: Structure
formation, AGNs, heating, mixing, etc.4. Physical state of IGM: impact on galaxy formation? 5. UHECR transport?6. Does magnetic energy flow destroy the statistics of Lyman-alpha forests?