Emission & High-energy Particles in Jets, Outflows, and Bubbles

1. 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)

2. Content • A phenomenological overview • Some simple minded physics • Systems that I have looked at (I) : Emission from plasmoids ejected from black holes Younsi & Wu (2015), MNRAS, to be submitted • Systems that I have looked at (II) : UHE neutrino fluxes from various AGN populations … Jacobsen, Wu, et al (2015), MNRAS, in press • Some naïve thoughts about galactic outflows: Galactic outflows from the starburst galaxy M82 Sutton, Ferreras, Wu, et al. (2014), MNRAS, 440, 150

3. 1. A phenomenological overview

4. The Hillas plot The Lamor radius of the particle should not exceed the characteristic size of its accelerator

5. Source phenomenology RCW120 nebula superbubble in the LMC (credit: Hershel Observatory) (credit: C. Smith [U Michigan])

6. Source phenomenology large-scale galactic winds/outflows in the starburst galaxy M82 (credit: HST/Chandra/Spitzer)

7. Source phenomenology (credit: wikipedia)

8. Source phenomenology cavity/bubbles in NGC741 group (Jetha et al. 2008)

9. Source phenomenology M87 (credit: NRAO/ U Northern Iowa)

10. Source phenomenology cavities/bubbles in galaxy clusters (Doria et al. 2012)

11. Source phenomenology (credit: Nature.com)

12. Revisiting the Hillas plot Now, shall we look at the Hillas plot in a slightly different perspective?

13. 2. Very simple-minded physics

14. Magnetic fields in astro-systems magnetic field (gauss) 10-9 ? 10-6 10-3 1 103 106 109 1012 walls? voids? clusters stars white dwarfs magnetars galaxies neutron stars >1026 1025 1023 1010 109 106 106 linear size (cm) 1013 1011 ~1 1 1 1 mass (solar mass)

15. Magnetic fields in astro-systems non-directional magnetic flux 1028 G cm2 - magnetars 1021 - 1025 G cm2 - neutron stars 1021 - 1025 G cm2 - white dwarfs 1021 - 1023 G cm2 - solar-like stars ~1041 G cm2 - galaxies ~1042 G cm2 - galaxy clusters ??? - superclusters, filaments, voids in co-moving frame

16. High-energy emission High-energy electromagnetic radiation • Synchrotron radiation • (inverse) Compton scattering • Bremsstrahlung radiation • Electron-positron annihilation How about High-energy non-photonic radiation? • Cosmic rays • Neutrinos It seems to need some high-energy particles. But what? Where? How?

17. Transport of high-energy emission About the delivery of the particles/radiation • Particle number (non-)conservation • Particle phase space conservation About the path of delivery of the particles/radiation • Space-time (properties) • Electro-magnetic force (?) Continuity equation:

18. Transport of high-energy emission Continuity equation (as a Boltzmann equation): Continuity equation (in the covariant form): Continuity equation for free-falling particle packets:

19. Producing high-energy emission Astrophysical context (macro-phenomenological physics) - shocks in astrophysical systems (credit: UC Berkeley)

20. Producing high-energy emission Astrophysical context (macro-phenomenological physics) - unipolar induction (?) (credit: NRAO/AUI, MPIfR, ASC-Lebedev, Y. Y. Kovalev)

21. Producing high-energy emission Astrophysical context (macro-phenomenological physics) - alternation of magnetic field topology (credit:NASA-GSFC)

22. 3. Systems that I look at (I): Emission from plasmoids ejected from black holes

23. GRMHD jet (Pu … Wu et al 2015)

24. Episodic outflow from a black hole (Meyer et al. 2015)

25. CME-like plasmoid ejection from accreting black holes (Yuan, Lin, Wu, Ho 2009)

26. Covariant radiative transfer Younsi & Wu (2014) [moment expansion: Thorne (1980), Fuerst (2005), Wu et al. (2006, 2008) Shibata et al. (2011)] • 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

27. Ray-tracing in black hole environments Kerr black hole Schwarzschild black hole ( Ziri Younsi, 2013, PhD thesis, UCL)

28. Black hole shadowing and tori around a rotating black hole • Movies: • Shadow of a Kerr black hole • Frequency shifts on a surface of a torus around a Kerr black hole • Intensity of emission from an opaque tours around a Kerr black hole • Emission image of a semi-opaque torus around a Kerr black hole • Emission image of an translucent torus around a Kerr black hole

29. Plasmoid launched from a black hole (Younsi & Wu 2015)

30. Gravitational lensing on the plasmoid emission • Movies: • Plasmoid orbiting a Schwarzschild black hole viewed at an inclination of 45 deg • Plasmoid orbiting a Schwarzschild black hole viewed at an inclination of 90 deg • Plasmoid orbiting a Kerr black hole viewed at an inclination of 45 deg • Plasmoidrobiting a Kerr black hole viewed at an inclination of 90 deg

31. Lightcurves of opaque plasmoids Younsi & Wu (2015)

32. Lightcurves of opaque plasmoids ( Ziri Younsi, 2013, PhD thesis, UCL)

33. Time corrected lightcurves of an opaque plasmoid orbiting a Schwarzschild black hole Younsi & Wu (2015)

34. Time corrected lightcurves of an opaque plasmoid orbiting a Schwarzschild black hole Younsi & Wu (2015)

35. Time corrected lightcurves of a transparent plasmoid orbiting a Kerr black hole Younsi & Wu (2015)

36. Lightcurves of plasmoid ejection Younsi & Wu (2015)

37. Lightcurves of plasmoid ejection Younsi & Wu (2015)

38. 3. Systems that I look at (II): UHE neutrino fluxes from various AGN populations derived from X-ray surveys

39. AGN as UHE neutrino sources (credit: ESO, MPIfR, APEX, NASA, CXC)

40. Testing AGN as UHE neutrino sources UHE neutrinos jet/outflow accretion Gamma-ray hadronic interaction accretion disk X-rays jet astrophysics photo-hadronic interaction (Pakvasa 2008) Note that

41. Photo-hadronic jet models Left: Koers & Tinyakov (2008) model; Right: Becker & Biermann (2009) model

42. X-ray luminosity function of AGN

43. 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)

44. Neutrino fluxes from various AGN IC59: IceCube 1-year limit (Aartsen et al.2015) Dashed line: Best-fit IceCube diffuse neutrino spectrum (Aartsen et al. 2015) (Jacobsen, Wu et al. 2015)

45. Neutrino fluxes from various AGN (Jacobsen, Wu et al. 2015)

46. What we have found: Cen A is not a typical neutrino source or not even a source X-ray and neutrino fluxes of AGN are not universally scaled across the sub-classes The jet models by Koers & Tinyakov (2008) and Becker & Biermann (2009) overestimated the neutrino production rate Some AGN are by nature not neutrino sources Neutrino generation and X-ray generation may gave different duty cycle It is a combination of the above

47. 3. Some comments/thoughts about galactic outflow: Galactic outflows from the starburst galaxy M82

48. The starburst galaxy M82 (credit: R. Zmaritsch and A. Gross)

49. Swift/UVOT observation of M82 Hutton, Ferreras, Wu et al. (2014)

50. Luminosity density across M82 Hutton, Ferreras, Wu et al. (2014)