Hot Settling Accretion Flow onto a Spinning Black Hole

We study the structure and properties of hot MHD accretion onto a Kerr black hole. In such a system, the hole is magnetically coupled to the inflowing gas and exerts a torque onto the accretion flow. A hot settling flow can form around the hole and transport the angular momentum outward, to the outer edge of the flow. Unlike other hot flows, such as advection- and convection-dominated flows and inflow-outflow solutions (ADAFs, CDAFs, and ADIOS), the properties of the hot settling flow are determined by the spin of the central black hole, but are insensitive to the mass accretion rate. Therefore, it may be possible to identify rapidly spinning BHs simply from their broad-band spectra. Observationally, the hot settling flow around a Kerr hole is somewhat similar to other hot flows in that they all have hard, power-law spectra and relatively low luminosities. Thus, most black hole candidates in the low/hard and, perhaps, intermediate X-ray state may potentially accrete via the hot settling flow. However, a settling flow will be somewhat more luminous than ADAFs/CDAFs/ADIOS, will exhibit high variability in X-rays, and may have relativistic jets. This suggests that galactic microquasars and active galactic nuclei may be powered by hot settling flows. We identify several galactic X-ray sources as the best candidates.Comment: 7 pages, 1 figure. Submitted to Ap

De l'interactivité du récit au récit interactif

À ses origines, la théorie du récit, notamment la narratologie d'inspiration formaliste et structuraliste, s'est développée dans le creuset des études littéraires. De ce fait, le point focal de cette discipline a longtemps été constitué par le récit verbal, généralement sous la forme d'un texte écrit et planifié par un auteur, laissant de côté les formes narratives émergentes, participatives ou interactives. On observe cependant, depuis une vingtaine d'année, une accélération dans le processus d'élargissement des objets d'étude de la narratologie, accompagnée par une mutation épistémologique. Retraçant cette évolution, Jan Christoph Meister observe ainsi un changement d'orientation faisant passer la théorie du récit de l'étude de phénomènes textuels à l'analyse « des fonctions cognitives de récits oraux et non littéraires, ouvrant ainsi un nouveau chapitre dans le projet narratologique » (2009 : 340). Si l'intrigue peut être décrite - en adoptant un point de vue fonctionnaliste et cognitiviste - comme une matrice de possibilités ontologiquement instable, comme un dispositif dont la fonction première est d'ouvrir des virtualités narratives et d'engendrer de la curiosité ou du suspense (Baroni 2007 ; 2009), alors il n'y a pas de raison de la considérer comme un obstacle à l'analyse de récits émergents et participatifs, voire de simulations ou de pratiques ludiques hautement interactives

Relativistic Hydrodynamic Flows Using Spatial and Temporal Adaptive Structured Mesh Refinement

Astrophysical relativistic flow problems require high resolution three-dimensional numerical simulations. In this paper, we describe a new parallel three-dimensional code for simulations of special relativistic hydrodynamics (SRHD) using both spatially and temporally structured adaptive mesh refinement (AMR). We used the method of lines to discretize the SRHD equations spatially and a total variation diminishing (TVD) Runge-Kutta scheme for time integration. For spatial reconstruction, we have implemented piecewise linear method (PLM), piecewise parabolic method (PPM), third order convex essentially non-oscillatory (CENO) and third and fifth order weighted essentially non-oscillatory (WENO) schemes. Flux is computed using either direct flux reconstruction or approximate Riemann solvers including HLL, modified Marquina flux, local Lax-Friedrichs flux formulas and HLLC. The AMR part of the code is built on top of the cosmological Eulerian AMR code {\sl enzo}. We discuss the coupling of the AMR framework with the relativistic solvers. Via various test problems, we emphasize the importance of resolution studies in relativistic flow simulations because extremely high resolution is required especially when shear flows are present in the problem. We also present the results of two 3d simulations of astrophysical jets: AGN jets and GRB jets. Resolution study of those two cases further highlights the need of high resolutions to calculate accurately relativistic flow problems.Comment: 14 pages, 23 figures. A section on 3D GRB jet simulation added. Accepted by ApJ