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Electromagnetic and Radiative Processes Near Black Hole Event Horizon

Electromagnetic and Radiative Processes Near Black Hole Event Horizon. Kinwah Wu (MSSL, University College London) Steven Von Fuerst (KIPAC, Stanford University) Warrick Ball (P&A, University College London). Living with black holes - artists’ impression.

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Electromagnetic and Radiative Processes Near Black Hole Event Horizon

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  1. Electromagnetic and Radiative Processes Near Black Hole Event Horizon Kinwah Wu (MSSL, University College London) Steven Von Fuerst (KIPAC, Stanford University) Warrick Ball (P&A, University College London)

  2. Living with black holes - artists’ impression (images from http://www.musemessenger.com)

  3. Black holes are very simple objects • What do black hole have? • a singularity • an event horizon Schwarzschild radius

  4. Do black hole exist? Who knows …… but …… Astrophysical zoo of “black holes” ……… 1. Stellar mass black holes - dead corpses of very massive stars 2. Supermassive black holes - monsters at the centres of galaxies 3. Intermediate mass black holes (?) - “the new kids on the block” ultra-luminous X-ray sources (ULX) 4. Primordial black holes - fossils of the distant past a ULX in the starburst galaxy M82 (image from science@nasa)

  5. What we have seen .… what we are believing …. Artists’ production based on astrophysicists’ interpretation Observational images (image from http://chandra.harvard.edu/photo/2004/rxj1242)

  6. X-ray lines from accretion disks around black holes Time-averaged line profiles of Fe K alpha emission from the AGN MCG-6-30-15 obtained by the ASCA satellite. from Fabian et al. (2000)

  7. Relativistic energy shift in ray tracing: “Usual” line emission calculations • The standard recipe: • define the metric and calculate the geodesic • make a Keplerian thin disk (i.e. velocity profile of the emitters) • determine the energy shift relative to the observed at each disk pixel • sum the contribution of emission from each pixel But, …. how about radiative transfer effects? … Absorption? Scattering? Also, ….. what if the disk is not geometrically thin or Keplerian? …

  8. Formulating general relativistic radiative transfer Liouville’s Theorem Boltzmann Equation Radiative Transfer Equation in a Covariant Form BBGKY Hierarchy General Relativity no scattering - phase-space volume conservation - particle number conservation in the comoving frame (Fuerst & Wu 2004, 2007; Wu et al. 2006)

  9. Resonant scattreing in the relativistic frame work Juetter distribution constraints (conservation and covariant resonant conditions): Fuerst & Wu (2004)

  10. General relativistic radiative transfer- absorption and emission Profiles of absorption and emission lines from thin accretion disks around Schwarzschild and Kerr black holes with a = 0.998, viewed at inclinations of 45o and 85o (top and bottom rows respectively). (Fuerst & Wu 2004)

  11. General relativistic radiative transfer- angle dependent emission Accretion-disk images showing the pitch angles of photons (in the local emitters’ frame) that can reach a distant observer. The disk images are viewed at inclination angles of 45o (left panels) and 85o (right panels). Disks around a Schwarzschild black hole are on the top row, and disks around a Kerr black hole (a = 0.998) are on the bottom row. Wu et al. (2006)

  12. Emission from 3D objects around a black hole i = 45o Profiles of emission lines from opaque relativistic accretion tori with an aspect ratio set by a velocity law, with index n = 0.232 and rk = 8rg as indicated in MRI accretion disk simulations i = 85o Fuerst and Wu (2007) energy-shift torus image

  13. Emission optically thick accretion tori Energy-shift images of tori (n = 0.2) around Kerr black holes (a = 0.998), with a large aspect ratio such that the inner boundary of the emission surface reaches the black-hole event horizon. Viewing inclination angle i = 15o, 45o and 85o (panels in top row, from left to right). Fuerst and Wu (2007)

  14. Emission from semi-opaque accretion tori Lines with different energies can resonate in semi-transparent tori Wu et al. (2008)

  15. Time-dependent calculations Synchrotron and free-free emission from accretion inflows and outflows in the vicinity of a Kerr black hole (obtained by GRMHD simulations). Fuerst et al. (2007)

  16. General relativistic radiative transfer in the presence of scattering General relativistic transfer in the presence of scattering - a global integral equation instead of a local differential equation tensor moment function the radiative transfer equation in stationary space-time first-order tensor moment equation + higher-order moment equations … the energy “Doppler” shift factor Fuerst (2005), Wu et al. (2008)

  17. Scattering dominated accretion tori around a black hole (Fuerst 2005, PhD Thesis)

  18. Seeing is believing imaging black hole and shadowing Shadows of background sky cast by a Schwarzschild black hole with spherical (left) and gaussian (right) planar matter distributions Ball and Wu (2008)

  19. Can all black holes be imaged by shadowing? black hole incident electro-magnetic plane waves There are always some big photons which cannot be fit inside a black hole!

  20. Black holes as particle scatterer At infinity Near the event horizon Klein-Gordon plane waves

  21. Black hole scattering • Plane wave-like behaviour at infinity and near the black hole • event horizon Potential scattering: One can define the emission and absorption coefficient of black hole. (cf radiative processes of atomic matter) Black holes are not black after all … They are actually gray holes in disguise.

  22. Event horizon revisited • boundary of no return • surface of infinite red-shift • surface at which waves piled up • ……

  23. Making black hole event horizon in the laboratory an artificial event horizon (photon trapped surface) is developed at the leading edge of the first laser pulse laser optical fibre The first laser pulse to modify the property of the optical fibre The second pulse, at a different wavelength, as the probing wave Leohardt et al. (2007)

  24. Electrodynamics near black hole event horizon My own questions: How do information transfer near the event horizon? Can we have a classical treatment? What is the role of gravity? My thought experiment: Suppose that we thread the optical fibre with a magnetic field, do the magnetic field on the left side and the right side of the laser induced event horizon communicate (classically)? laser optical fibre

  25. What do we know about the black hole event horizon?What do we know about black holes? ? ? ?

  26. I want to believe ……

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