La exhibición y el episodio de Estesilao en el prólogo de Laques y su referencialidad respecto del Agón dialéctico

Lisímaco y Melesias han invitado a los generales Nicias y Laques a presenciar una exhibición de lucha armada. Con motivo del espectáculo y ante la recomendación de esa disciplina para la educación de sus hijos, los padres deciden consultar la opinión de quienes son considerados especialistas en la materia. Esta especie de simulacro de pelea es el inicio de una conversación acerca de si es beneficioso, o no este aprendizaje. Al diálogo entre los padres y los generales se suma Sócrates. A partir de la discrepancia entre Laques y Nicias y el ingreso de Sócrates comienza a desplegarse una suerte de agón dialéctico. La presente comunicación intenta establecer una analogía entre el comportamiento de Estesilao, el luchador de la exhibición, en un determinado episodio relatado por Laques y el que sostiene Nicias frente a los embates del élenkhos socrático

La exhibición y el episodio de Estesilao en el prólogo de Laques y su referencialidad respecto del Agón dialéctico

Lisímaco y Melesias han invitado a los generales Nicias y Laques a presenciar una exhibición de lucha armada. Con motivo del espectáculo y ante la recomendación de esa disciplina para la educación de sus hijos, los padres deciden consultar la opinión de quienes son considerados especialistas en la materia. Esta especie de simulacro de pelea es el inicio de una conversación acerca de si es beneficioso, o no este aprendizaje. Al diálogo entre los padres y los generales se suma Sócrates. A partir de la discrepancia entre Laques y Nicias y el ingreso de Sócrates comienza a desplegarse una suerte de agón dialéctico. La presente comunicación intenta establecer una analogía entre el comportamiento de Estesilao, el luchador de la exhibición, en un determinado episodio relatado por Laques y el que sostiene Nicias frente a los embates del élenkhos socrático

La exhibición y el episodio de Estesilao en el prólogo de Laques y su referencialidad respecto del Agón dialéctico

Lisímaco y Melesias han invitado a los generales Nicias y Laques a presenciar una exhibición de lucha armada. Con motivo del espectáculo y ante la recomendación de esa disciplina para la educación de sus hijos, los padres deciden consultar la opinión de quienes son considerados especialistas en la materia. Esta especie de simulacro de pelea es el inicio de una conversación acerca de si es beneficioso, o no este aprendizaje. Al diálogo entre los padres y los generales se suma Sócrates. A partir de la discrepancia entre Laques y Nicias y el ingreso de Sócrates comienza a desplegarse una suerte de agón dialéctico. La presente comunicación intenta establecer una analogía entre el comportamiento de Estesilao, el luchador de la exhibición, en un determinado episodio relatado por Laques y el que sostiene Nicias frente a los embates del élenkhos socrático

El agón como el problema platónico : Una lectura deleuziana

Hay todo un entorno del problema griego según Deleuze: el agón. La ciudad ateniense es una rivalidad entre pretendientes. En la obra platónica, a la que Deleuze se refiere a menudo como la Odisea filosófica, el enfrentamiento entre rivales aparece constantemente y en todos los ámbitos, en el amor, los juegos, la política, los tribunales, incluso la filosofía tendrá también sus pretendientes. La pregunta es platónica es, según Deleuze, ¿cómo seleccionar a los pretendientes? La Idea juega el rol de paradigma de autenticidad dentro del método dialéctico cuya función debe ser entendida, según Deleuze, en términos de selección y no de clasificación. En el presente trabajo nos proponemos presentar esta lectura deleuziana a los efectos de evaluar sus alcances

El agón como el problema platónico : Una lectura deleuziana

Hay todo un entorno del problema griego según Deleuze: el agón. La ciudad ateniense es una rivalidad entre pretendientes. En la obra platónica, a la que Deleuze se refiere a menudo como la Odisea filosófica, el enfrentamiento entre rivales aparece constantemente y en todos los ámbitos, en el amor, los juegos, la política, los tribunales, incluso la filosofía tendrá también sus pretendientes. La pregunta es platónica es, según Deleuze, ¿cómo seleccionar a los pretendientes? La Idea juega el rol de paradigma de autenticidad dentro del método dialéctico cuya función debe ser entendida, según Deleuze, en términos de selección y no de clasificación. En el presente trabajo nos proponemos presentar esta lectura deleuziana a los efectos de evaluar sus alcances

El agón como el problema platónico : Una lectura deleuziana

Hay todo un entorno del problema griego según Deleuze: el agón. La ciudad ateniense es una rivalidad entre pretendientes. En la obra platónica, a la que Deleuze se refiere a menudo como la Odisea filosófica, el enfrentamiento entre rivales aparece constantemente y en todos los ámbitos, en el amor, los juegos, la política, los tribunales, incluso la filosofía tendrá también sus pretendientes. La pregunta es platónica es, según Deleuze, ¿cómo seleccionar a los pretendientes? La Idea juega el rol de paradigma de autenticidad dentro del método dialéctico cuya función debe ser entendida, según Deleuze, en términos de selección y no de clasificación. En el presente trabajo nos proponemos presentar esta lectura deleuziana a los efectos de evaluar sus alcances

Cause and Effect of Feedback: Multiphase Gas in Cluster Cores Heated by AGN Jets

Multiwavelength data indicate that the X-ray-emitting plasma in the cores of galaxy clusters is not cooling catastrophically. To a large extent, cooling is offset by heating due to active galactic nuclei (AGNs) via jets. The cool-core clusters, with cooler/denser plasmas, show multiphase gas and signs of some cooling in their cores. These observations suggest that the cool core is locally thermally unstable while maintaining global thermal equilibrium. Using high-resolution, three-dimensional simulations we study the formation of multiphase gas in cluster cores heated by collimated bipolar AGN jets. Our key conclusion is that spatially extended multiphase filaments form only when the instantaneous ratio of the thermal instability and free-fall timescales (t(TI)/t(ff)) falls below a critical threshold of approximate to 10. When this happens, dense cold gas decouples from the hot intracluster medium (ICM) phase and generates inhomogeneous and spatially extended Ha filaments. These cold gas clumps and filaments ``rain'' down onto the central regions of the core, forming a cold rotating torus and in part feeding the supermassive black hole. Consequently, the self-regulated feedback enhances AGN heating and the core returns to a higher entropy level with t(TI)/t(ff) > 10. Eventually, the core reaches quasi-stable global thermal equilibrium, and cold filaments condense out of the hot ICM whenever t(TI)/t(ff) less than or similar to 10. This occurs despite the fact that the energy from AGN jets is supplied to the core in a highly anisotropic fashion. The effective spatial redistribution of heat is enabled in part by the turbulent motions in the wake of freely falling cold filaments. Increased AGN activity can locally reverse the cold gas flow, launching cold filamentary gas away from the cluster center. Our criterion for the condensation of spatially extended cold gas is in agreement with observations and previous idealized simulations.

COOL CORE CYCLES: COLD GAS AND AGN JET FEEDBACK IN CLUSTER CORES

Using high-resolution 3D and 2D (axisymmetric) hydrodynamic simulations in spherical geometry, we study the evolution of cool cluster cores heated by feedback-driven bipolar active galactic nuclei (AGNs) jets. Condensation of cold gas, and the consequent enhanced accretion, is required for AGN feedback to balance radiative cooling with reasonable efficiencies, and to match the observed cool core properties. A feedback efficiency (mechanical luminosity approximate to epsilon(M) over dot(acc)c(2); where (M) over dot(acc). is the mass accretion rate at 1 kpc) as small as 6 x 10(-5) is sufficient to reduce the cooling/accretion rate by similar to 10 compared to a pure cooling flow in clusters (with M-200 less than or similar to 7 x 10(14) M-circle dot). This value is much smaller compared to the ones considered earlier, and is consistent with the jet efficiency and the fact that only a small fraction of gas at 1 kpc is accreted onto the supermassive black hole (SMBH). The feedback efficiency in earlier works was so high that the cluster core reached equilibrium in a hot state without much precipitation, unlike what is observed in cool-core clusters. We find hysteresis cycles in all our simulations with cold mode feedback: condensation of cold gas when the ratio of the cooling-time to the free-fall time (t(cool)/t(ff)) is less than or similar to 10 leads to a sudden enhancement in the accretion rate; a large accretion rate causes strong jets and overheating of the hot intracluster medium such that t(cool)/t(ff) > 10; further condensation of cold gas is suppressed and the accretion rate falls, leading to slow cooling of the core and condensation of cold gas, restarting the cycle. Therefore, there is a spread in core properties, such as the jet power, accretion rate, for the same value of core entropy t(cool)/t(ff). A smaller number of cycles is observed for higher efficiencies and for lower mass halos because the core is overheated to a longer cooling time. The 3D simulations show the formation of a few-kpc scale, rotationally supported, massive (similar to 10(11) M-circle dot) cold gas torus. Since the torus gas is not accreted onto the SMBH, it is largely decoupled from the feedback cycle. The radially dominant cold gas (T < 5 x 10(4) K; vertical bar v(r)vertical bar >vertical bar v(phi vertical bar)) consists of fast cold gas uplifted by AGN jets and freely infalling cold gas condensing out of the core. The radially dominant cold gas extends out to 25 kpc for the fiducial run (halo mass 7 x 10(14) M-circle dot and feedback efficiency 6 x 10(-5)), with the average mass inflow rate dominating the outflow rate by a factor of approximate to 2. We compare our simulation results with recent observations.

Computational studies of the transverse structure of AGN jets

Both the emission properties and the evolution of the radio jets of Active Galactic Nuclei are dependent on the magnetic (B) fields that thread them. A number of observations of AGN jets suggest that the B fields they carry have a significant helical component, at least on parsec scales. This thesis uses a model, first proposed by Laing and then developed by Papageorgiou, to explore how well the observed properties of AGN jets can be reproduced by assuming a helical B field with three parameters; pitch angle, viewing angle and degree of entanglement. This model has been applied to multifrequency Very Long Baseline Interferometry (VLBI) observations of the AGN jets of Markarian 501 and M87, making it possible to derive values for the helical pitch angle, the viewing angle and the degree of entanglement for these jets. Faraday rotation measurements are another important tool for investigating the B fields of AGN jets. A helical B field component should result in a systematic gradient in the observed Faraday rotation across the jet. Real observed radio images have finite resolution; typical beam sizes for cm-wavelength VLBI observations are often comparable to or larger than the intrinsic jet widths, raising questions about how well resolved a jet must be in the transverse direction in order to reliably detect transverse Faraday-rotation structure. This thesis presents results of Monte Carlo simulations of Faraday rotation images designed to directly investigate this question, together with a detailed investigation into the probabilities of observing spurious Faraday Rotation gradients as a result of random noise and finite resolution. These simulations clearly demonstrate the possibility of detecting transverse Faraday-rotation structures even when the intrinsic jet widths are appreciably smaller than the beam width.

Multidimensional modelling of X-ray spectra for AGN accretion disc outflows - III. Application to a hydrodynamical simulation

We perform multidimensional radiative transfer simulations to compute spectra for a hydrodynamical simulation of a line-driven accretion disc wind from an active galactic nucleus. The synthetic spectra confirm expectations from parametrized models that a disc wind can imprint a wide variety of spectroscopic signatures including narrow absorption lines, broad emission lines and a Compton hump. The formation of these features is complex with contributions originating from many of the different structures present in the hydrodynamical simulation. In particular, spectral features are shaped both by gas in a successfully launched outflow and in complex flows where material is lifted out of the disc plane but ultimately falls back. We also confirm that the strong Fe Ka line can develop a weak, red-skewed line wing as a result of Compton scattering in the outflow. In addition, we demonstrate that X-ray radiation scattered and reprocessed in the flow has a pivotal part in both the spectrum formation and determining the ionization conditions in the wind. We find that scattered radiation is rather effective in ionizing gas which is shielded from direct irradiation from the central source. This effect likely makes the successful launching of a massive disc wind somewhat more challenging and should be considered in future wind simulations. © 2010 The Authors. Journal compilation © 2010 RAS.

Multidimensional modelling of X-ray spectra for AGN accretion disc outflows

We use a multidimensional Monte Carlo code to compute X-ray spectra for a variety of active galactic nucleus (AGN) disc-wind outflow geometries. We focus on the formation of blueshifted absorption features in the Fe K band and show that line features similar to those which have been reported in observations are often produced for lines of sight through disc-wind geometries. We also discuss the formation of other spectral features in highly ionized outflows. In particular, we show that, for sufficiently high wind densities, moderately strong Fe K emission lines can form and that electron scattering in the flow may cause these lines to develop extended red wings. We illustrate the potential relevance of such models to the interpretation of real X-ray data by comparison with observations of a well-known AGN, Mrk 766. Journal compilation © 2008 RAS.

Multidimensional modelling of X-ray spectra for AGN accretion disc outflows - II

Highly ionized fast accretion disc winds have been suggested as an explanation for a variety of observed absorption and emission features in the X-ray spectra of active galactic nuclei. Simple estimates have suggested that these flows may be massive enough to carry away a significant fraction of the accretion energy and could be involved in creating the link between supermassive black holes and their host galaxies. However, testing these hypotheses, and quantifying the outflow signatures, requires high-quality theoretical spectra for comparison with observations. Here, we describe extensions of our Monte Carlo radiative transfer code that allow us to generate realistic theoretical spectra for a much wider variety of disc wind models than that was possible in our previous work. In particular, we have expanded the range of atomic physics simulated by the code so that L- and M-shell ions can now be included. We have also substantially improved our treatment of both ionization and radiative heating such that we are now able to compute spectra for outflows containing far more diverse plasma conditions. We present example calculations that illustrate the variety of spectral features predicted by parametrized outflow models and demonstrate their applicability to the interpretation of data by comparison with observations of the bright quasar PG1211+143. We find that the major features in the observed 2-10 keV spectrum of this object can be well reproduced by our spectra, confirming that it likely hosts a massive outflow. © 2010 The Authors. Journal compilation © 2010 RAS.

Expanded iron uta spectra - Probing the thermal stability limits in AGN clouds

The Fe unresolved transition arrays (UTAs) produce prominent features in the 15-17 Å wavelength range in the spectra of active galactic nuclei (AGNs). Here, we present new calculations of the energies and oscillator strengths of inner-shell lines from Fe XIV, Fe XV, and Fe XVI. These are crucial ions since they are dominant at inflection points in the gas thermal stability curve, and UTA excitation followed by autoionization is an important ionization mechanism for these species. We incorporate these, and data reported in previous papers, into the plasma simulation code Cloudy. This updated physics is subsequently employed to reconsider the thermally stable phases in absorbing media in AGNs. We show how the absorption profile of the Fe XIV UTA depends on density, due to the changing populations of levels within the ground configuration. © 2013. The American Astronomical Society. All rights reserved.