Since 2002 Perimeter Institute has been recording seminars, conference talks, public outreach events such as talks from top scientists using video cameras installed in our lecture theatres. Perimeter now has 7 formal presentation spaces for its many scientific conferences, seminars, workshops and educational outreach activities, all with advanced audio-visual technical capabilities.
Recordings of events in these areas are all available and On-Demand from this Video Library and on Perimeter Institute Recorded Seminar Archive (PIRSA). PIRSA is a permanent, free, searchable, and citable archive of recorded seminars from relevant bodies in physics. This resource has been partially modelled after Cornell University's arXiv.org.
Accessibly by anyone with internet, Perimeter aims to share the power and wonder of science with this free library.
It is known that the entanglement entropy of quantum
fields on the black hole
background contributes to the Bekenstein-Hawking entropy,and that its
divergences can be absorbed into the renormalization of gravitational
couplings. By introducing a Wilsonian cutoff scale and the concepts of
the renormalization group, we can expand this observation
into a broader framework for understanding black hole entropy. At a
given RG scale, two contributions to the black hole entropy can be
I will discuss recent work in simulating asymptotically
anti-de Sitter spacetimes, and its relation to heavy ion collider physics. For
this purpose, I intend to focus on a class of oblately deformed black hole
spacetime solutions. For each of these solutions, I will map the gravitational
metric in the spacetime bulk to a stress tensor one-point function of the
conformal field theory defined on the spacetime boundary. During the ring-down
process, wherein the deformed black hole settles down to the AdS analog of the
Astronomical hydrodynamics is usually almost ideal in the sense that the Reynolds number (Re) is enormous and any effective viscosity must be due to shocks or turbulence. Astronomical magnetohydrodynamics (MHD) is often also nearly ideal, so that magnetic fields and plasma are well coupled. In particular, dissipation of orbital energy in accretion disks around black holes is readily explained by MHD turbulence. On the other hand, the planet-bearing disks around protostars are magnetically far from ideal because of very low fractional ionization. MHD turbulence is at best marginal
Check back for details on the next lecture in Perimeter's Public Lectures Series