emission and high-energy particles in jets, outflows and bubbles in galaxies and beyond galaxies...

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?