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Emission and high-energy particles in jets, outflows and bubbles in galaxies and beyond galaxies
Kinwah Wu Mullard Space Science Laboratory University College London United Kingdom
Collabortors:
Ziri Younsi * (ITP, Frankfurt), Ignacio Ferreras (MSSL, UCL)
Idunn Jacobsen (MSSL, UCL), Aayush Saxena * (Leiden)
Sandor Kruk * (Oxford), Curtis Saxton (Technion)
Alvina On (MSSL, UCL), Steven Fuerst * (Kavli, Stanford)
Hung-Yi Pu (ASIAA), Youske Mizuno (ITP, Frankfurt)
Content
1. A phenomenological overview
2. Some simple minded physics
3. Systems that I have looked at (I) :
Emission from plasmoids ejected from black holes
Younsi & Wu (2015), MNRAS, to be submitted
4. Systems that I have looked at (II) :
UHE neutrino fluxes from various AGN populations …
Jacobsen, Wu, et al (2015), MNRAS, in press
5. Some naïve thoughts about galactic outflows:
Galactic outflows from the starburst galaxy M82
Sutton, Ferreras, Wu, et al. (2014), MNRAS, 440,
150
1. A phenomenological overview
The Hillas plot
The Lamor radius of the particle should not exceed the characteristic size of its accelerator
Source phenomenology
RCW120 nebula
(credit: Hershel Observatory)
superbubble in the LMC
(credit: C. Smith [U Michigan])
Source phenomenology
large-scale galactic winds/outflows in the starburst galaxy M82
(credit: HST/Chandra/Spitzer)
Source phenomenology
(credit: wikipedia)
Source phenomenology
cavity/bubbles in NGC741 group
(Jetha et al. 2008)
Source phenomenology
(credit: NRAO/U Northern Iowa)
M87
Source phenomenology
cavities/bubbles in galaxy clusters
(Doria et al. 2012)
Source phenomenology
(credit: Nature.com)
Revisiting the Hillas plot
Now, shall we look at the Hillas plot in a slightly different perspective?
2. Very simple-minded physics
Magnetic fields in astro-systems
magnetic field (gauss)
1 10310-3 106 109 101210-6
stars white dwarfs
neutron stars
magnetars
galaxies
clusters walls? voids?
1023
linear size (cm)
109 106 10610101025>1026
10-9 ?
1011
mass (solar mass)
1 1 1~11013
Magnetic fields in astro-systems
- magnetars
- neutron stars
- white dwarfs
- solar-like stars
- galaxies
- galaxy clusters
- superclusters, filaments, voids
1028 G cm2
1021 - 1025 G cm2
1021 - 1025 G cm2
~1041 G cm2
1021 - 1023 G cm2
~1042 G cm2
???
non-directional magnetic flux
in co-moving frame
High-energy emission
High-energy electromagnetic radiation
How about High-energy non-photonic radiation?
- Synchrotron radiation - (inverse) Compton scattering - Bremsstrahlung radiation - Electron-positron annihilation
- Cosmic rays - Neutrinos
It seems to need some high-energy particles.
But what? Where? How?
Transport of high-energy emission
About the delivery of the particles/radiation
About the path of delivery of the particles/radiation
- Particle number (non-)conservation - Particle phase space conservation
- Space-time (properties) - Electro-magnetic force (?)
Continuity equation:
Transport of high-energy emission
Continuity equation (as a Boltzmann equation):
Continuity equation (in the covariant form):
Continuity equation for free-falling particle packets:
Producing high-energy emissionAstrophysical context (macro-phenomenological physics)
- shocks in astrophysical systems
(credit: UC Berkeley)
Producing high-energy emissionAstrophysical context (macro-phenomenological physics)
- unipolar induction (?)
(credit: NRAO/AUI, MPIfR, ASC-Lebedev, Y. Y. Kovalev)
Producing high-energy emissionAstrophysical context (macro-phenomenological physics)
- alternation of magnetic field topology
(credit:NASA-GSFC)
3. Systems that I look at (I): Emission from plasmoids ejected from black holes
GRMHD jet
(Pu … Wu et al 2015)
Episodic outflow from a black hole
(Meyer et al. 2015)
CME-like plasmoid ejection from accreting black holes
(Yuan, Lin, Wu, Ho 2009)
Covariant radiative transfer
• Relativistic beaming • Doppler shift • Transverse Doppler shift • Gravitational redshift • Gravitational lensing • Reference frame dragging
spin/polarisation in strong gravity-de-Sitter precession -Lense-Thirring precession -spin-curvature coupling
[moment expansion: Thorne (1980), Fuerst (2005), Wu et al. (2006, 2008) Shibata et al. (2011)]
Younsi & Wu (2014)
Ray-tracing in black hole environments
( Ziri Younsi, 2013, PhD thesis, UCL)
Schwarzschild black holeKerr black hole
Black hole shadowing and tori around a rotating black hole
Movies:
1.Shadow of a Kerr black hole 2.Frequency shifts on a surface of a torus around a Kerr black hole 3.Intensity of emission from an opaque tours around a Kerr black hole4.Emission image of a semi-opaque torus around a Kerr black hole 5.Emission image of an translucent torus around a Kerr black hole
Plasmoid launched from a black hole
(Younsi & Wu 2015)
Gravitational lensing on the plasmoid emission
Movies: 1.Plasmoid orbiting a Schwarzschild black hole viewed at an inclination of 45 deg 2.Plasmoid orbiting a Schwarzschild black hole viewed at an inclination of 90 deg 3.Plasmoid orbiting a Kerr black hole viewed at an inclination of 45 deg 4.Plasmoid robiting a Kerr black hole viewed at an inclination of 90 deg
Lightcurves of opaque plasmoids
Younsi & Wu (2015)
Lightcurves of opaque plasmoids
( Ziri Younsi, 2013, PhD thesis, UCL)
Time corrected lightcurves of an opaque plasmoid orbiting a Schwarzschild black hole
Younsi & Wu (2015)
Time corrected lightcurves of an opaque plasmoid orbiting a Schwarzschild black hole
Younsi & Wu (2015)
Time corrected lightcurves of a transparent plasmoid orbiting a Kerr black hole
Younsi & Wu (2015)
Lightcurves of plasmoid ejection
Younsi & Wu (2015)
Lightcurves of plasmoid ejection
Younsi & Wu (2015)
3. Systems that I look at (II): UHE neutrino fluxes from various AGN populations derived from X-ray surveys
AGN as UHE neutrino sources
(credit: ESO, MPIfR, APEX, NASA, CXC)
Testing AGN as UHE neutrino sources
UHE neutrinos
Gamma-ray
X-raysaccretion disk
jet/outflow
hadronic interaction
jet astrophysics
photo-hadronic interaction
accretion
Note that (Pakvasa 2008)
Photo-hadronic jet models
Left: Koers & Tinyakov (2008) model; Right: Becker & Biermann (2009) model
X-ray luminosity function of AGN
AGN populations
The AGN populations and their evolution are derived from the X-ray luminosity functions constructed from the Chandra (Silverman et al. 2008) and Swift/BAT (Ajello et al. 2009) X-ray survey data.
(Jacobsen, Wu et al. 2015)
Neutrino fluxes from various AGN
(Jacobsen, Wu et al. 2015)
IC59: IceCube 1-year limit (Aartsen et al.2015)
Dashed line: Best-fit IceCube diffuse neutrino spectrum(Aartsen et al. 2015)
Neutrino fluxes from various AGN
(Jacobsen, Wu et al. 2015)
What we have found:
1. Cen A is not a typical neutrino source or not even a source
2. X-ray and neutrino fluxes of AGN are not universally scaled across the sub-classes
3. The jet models by Koers & Tinyakov (2008) and Becker & Biermann (2009) overestimated the neutrino production rate
4. Some AGN are by nature not neutrino sources
5. Neutrino generation and X-ray generation may gave different duty cycle
6. It is a combination of the above
3. Some comments/thoughts about galactic outflow: Galactic outflows from the starburst galaxy M82
The starburst galaxy M82
(credit: R. Zmaritsch and A. Gross)
Swift/UVOT observation of M82
Hutton, Ferreras, Wu et al. (2014)
Luminosity density across M82
Hutton, Ferreras, Wu et al. (2014)
Colour difference between the galactic disk and the wind
Hutton, Ferreras, Wu et al. (2014)
Colour difference between the galactic disk and the wind
x = 0 Mie scattering
x = - 4Rayleigh scattering
Hutton, Ferreras, Wu et al. (2014)
Size distribution of dust grain in the galaxy wind of M82
Hutton, Ferreras, Wu et al. (2014)
Some very naïve thoughts about galactic outflows
1. How the dust co-exist with the high-energy radiations in the disk wind?
2. Can we use the spatial distribution of the dust properties to infer the cosmic ray and high-energy particle content throughout the wind cone?