The Effect of the Hall Term on the Nonlinear Evolution of the Magnetorotational Instability: I. Local Axisymmetric Simulations

The effect of the Hall term on the evolution of the magnetorotational instability (MRI) in weakly ionized accretion disks is investigated using local axisymmetric simulations. First, we show that the Hall term has important effects on the MRI when the temperature and density in the disk is below a few thousand K and between 10^13 and 10^18 cm^{-3} respectively. Such conditions can occur in the quiescent phase of dwarf nova disks, or in the inner part (inside 10 - 100 AU) of protoplanetary disks. When the Hall term is important, the properties of the MRI are dependent on the direction of the magnetic field with respect to the angular velocity vector \Omega. If the disk is threaded by a uniform vertical field oriented in the same sense as \Omega, the axisymmetric evolution of the MRI is an exponentially growing two-channel flow without saturation. When the field is oppositely directed to \Omega, however, small scale fluctuations prevent the nonlinear growth of the channel flow and the MRI evolves into MHD turbulence. These results are anticipated from the characteristics of the linear dispersion relation. In axisymmetry on a field with zero-net flux, the evolution of the MRI is independent of the size of the Hall term relative to the inductive term. The evolution in this case is determined mostly by the effect of ohmic dissipation.Comment: 31 pages, 3 tables, 12 figures, accepted for publication in ApJ, postscript version also available from http://www.astro.umd.edu/~sano/publications

Global change and the uncertain future of biodiversity in Mediterranean-type ecosystems : insights from a strategic foresight process /

La conservación requiere una previsión estratégica que permita abordar con eficacia los retos actuales que plantea el cambio global. La cuenca Mediterránea ha sido identificada como área prioritaria para la conservación, particularmente vulnerable al efecto combinado del cambio climático, el cambio de los usos del suelo y el régimen de perturbaciones por incendios forestales. Los efectos de la interacción de estos factores de cambio y las grandes incertidumbres asociadas a su predicción, también pueden ser vistas como una oportunidad para intervenir a través de mejores políticas de conservación. Los ejercicios de previsión estratégica pueden ofrecer a los responsables de la toma de decisiones herramientas para pensar de forma creativa y proactiva sobre el futuro y tomar decisiones que creen un futuro más deseable. En esta tesis ilustramos el papel de las actividades de 'horizon scanning', planificación y análisis de escenarios basados en simulación, en los que se sustenta el enfoque de previsión estratégica, y en la que usamos escenarios conceptuales como líneas argumentales y simulaciones como estimaciones numéricas de los futuros cambios ambientales. En particular, este ejercicio de previsión estratégica contribuye a la apertura de dos opciones de políticas de manejo del fuego prometedoras ('dejar quemar los incendios no planificados' y 'la extracción de biomasa forestal para bioenergía') alternativas al paradigma actual de 'apagar todos los incendios'. Ambas políticas de manejo del fuego podrían combinarse estratégicamente con el fin de alcanzar los objetivos de reducción de combustible requeridas para mitigar el creciente impacto de los grandes incendios causados por el cambio global. La planificación de la conservación puede ser mejorada considerablemente mediante la aplicación de estas estrategias de manejo del fuego. Dos principales oportunidades de conservación emergentes han sido identificados y deben ser priorizadas a fin de proteger de forma efectiva las especies de aves de interés comunitario en un futuro próximo: 1) la creación de etapas tempranas de sucesión de la vegetación para especies de hábitat abierto a través de políticas de 'dejar quemar incendios no planificados'; y 2) el aumento de la capacidad de resiliencia frente al cambio climático de los hábitats forestales claves para las especies más forestales. En esta tesis se hace hincapié en la necesidad de una perspectiva de conservación integral en donde las políticas agrícolas, forestales y de manejo de fuego deben ser consideradas explícitamente para preservar eficazmente hábitats clave para las aves más amenazadas en sistemas altamente dinámicos propensos al fuego. Nuestros resultados también arrojan luz sobre la importancia de considerar la dinámica del paisaje y las sinergias entre las diferentes fuerzas motrices a la hora de evaluar a largo plazo la eficacia de la gestión del fuego en la reducción del riesgo de incendios y la protección de la biodiversidad en los ecosistemas de tipo mediterráneoConservation needs strategic foresight leading to effectively address the ongoing challenges posed by global change. Mediterranean Basin has been identified as priority area for conservation, particularly vulnerable to the combined effects of climate change, land-use change and fire disturbance regime. The interacting effects of these drivers, and the large uncertainties associated to their forecasting, might also bring conservation opportunities to intervene through better policies. Strategic foresight exercises may offer decision-makers with tools to creatively think about the future and make decisions that create a more desirable future. In this thesis, we illustrate the role for horizon scanning, scenario planning and simulation-based scenario analysis in underpinning the strategic foresight approach - using storylines as conceptual scenarios, and simulations as numerical estimates of future environmental changes. In particular, this strategic foresight exercise contributes to opening up two promising fire management policy options ('letting unplanned fires burn' and 'forest biomass extraction for bioenergy uses') alternatives to the current fire suppression paradigm of "stopping all fires''. Both fire management policies could be strategically combined in order to achieve the fuel reduction objectives required to mitigate the increasing impact of large fires caused by global change. Conservation planning may be considerably improved through the implementation of such fire management strategies. Two main emerging conservation opportunities have been identified and should be prioritized in order to effectively protect community-interest bird species in the near future: 1) promoting early-succession stages of vegetation for open-habitat dwelling species through 'letting unplanned fires burn' policies; and 2) increasing the resilience of key forest habitats to climate change for forest-dwelling species. This thesis emphasizes the need for an integrative conservation perspective wherein agricultural, forest and fire management policies should be explicitly considered to effectively preserve key habitats for threatened birds in fire-prone, highly-dynamic systems. Our findings also shed light about the importance of considering landscape dynamics and the synergies between different driving forces when assessing the long-term effectiveness of fire management at reducing fire risk and safeguarding biodiversity in Mediterranean-type ecosystems

Casimir effect: running Newton constant or cosmological term

We argue that the instability of Euclidean Einstein gravity is an indication that the vacuum is non perturbative and contains a condensate of the metric tensor in a manner reminiscent of Yang-Mills theories. As a simple step toward the characterization of such a vacuum the value of the one-loop effective action is computed for Euclidean de Sitter spaces as a function of the curvature when the unstable conformal modes are held fixed. Two phases are found, one where the curvature is large and gravitons should be confined and another one which appears to be weakly coupled and tends to be flat. The induced cosmological constant is positive or negative in the strongly or weakly curved phase, respectively. The relevance of the Casimir effect in understanding the UV sensitivity of gravity is pointed out.Comment: Final, slightly extended version, to appear in Classical and Quantum Gravit

CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z=0.44 galaxy cluster MACS 1206.2-0847

We use an unprecedented data-set of about 600 redshifts for cluster members, obtained as part of a VLT/VIMOS large programme, to constrain the mass profile of the z=0.44 cluster MACS J1206.2-0847 over the radial range 0-5 Mpc (0-2.5 virial radii) using the MAMPOSSt and Caustic methods. We then add external constraints from our previous gravitational lensing analysis. We invert the Jeans equation to obtain the velocity-anisotropy profiles of cluster members. With the mass-density and velocity-anisotropy profiles we then obtain the first determination of a cluster pseudo-phase-space density profile. The kinematics and lensing determinations of the cluster mass profile are in excellent agreement. This is very well fitted by a NFW model with mass M200=(1.4 +- 0.2) 10^15 Msun and concentration c200=6 +- 1, only slightly higher than theoretical expectations. Other mass profile models also provide acceptable fits to our data, of (slightly) lower (Burkert, Hernquist, and Softened Isothermal Sphere) or comparable (Einasto) quality than NFW. The velocity anisotropy profiles of the passive and star-forming cluster members are similar, close to isotropic near the center and increasingly radial outside. Passive cluster members follow extremely well the theoretical expectations for the pseudo-phase-space density profile and the relation between the slope of the mass-density profile and the velocity anisotropy. Star-forming cluster members show marginal deviations from theoretical expectations. This is the most accurate determination of a cluster mass profile out to a radius of 5 Mpc, and the only determination of the velocity-anisotropy and pseudo-phase-space density profiles of both passive and star-forming galaxies for an individual cluster [abridged]Comment: A&A in press; 22 pages, 19 figure

CLASH-VLT: The stellar mass function and stellar mass density profile of the z = 0.44 cluster of galaxies MACS J1206.2-0847

Context. The study of the galaxy stellar mass function (SMF) in relation to the galaxy environment and the stellar mass density profile, (r), is a powerful tool to constrain models of galaxy evolution. Aims. We determine the SMF of the z = 0.44 cluster of galaxies MACS J1206.2-0847 separately for passive and star-forming (SF) galaxies, in different regions of the cluster, from the center out to approximately 2 virial radii. We also determine (r) to compare it to the number density and total mass density profiles. Methods. We use the dataset from the CLASH-VLT survey. Stellar masses are obtained by spectral energy distribution fitting with the MAGPHYS technique on 5-band photometric data obtained at the Subaru telescope. We identify 1363 cluster members down to a stellar mass of 109.5 M, selected on the basis of their spectroscopic (~1/3 of the total) and photometric redshifts. We correct our sample for incompleteness and contamination by non members. Cluster member environments are defined using either the clustercentric radius or the local galaxy number density. Results. The whole cluster SMF is well fitted by a double Schechter function, which is the sum of the two Schechter functions that provide good fits to the SMFs of, separately, the passive and SF cluster populations. The SMF of SF galaxies is significantly steeper than the SMF of passive galaxies at the faint end. The SMF of the SF cluster galaxies does not depend on the environment. The SMF of the passive cluster galaxies has a significantly smaller slope (in absolute value) in the innermost (= 0.50 Mpc, i.e., ~0.25 virial radii), and in the highest density cluster region than in more external, lower density regions. The number ratio of giant/subgiant galaxies is maximum in this innermost region and minimum in the adjacent region, but then gently increases again toward the clusteroutskirts. This is also reflected in a decreasing radial trend of the average stellar mass per cluster galaxy. On the other hand, the stellar mass fraction, i.e., the ratio of stellar to total cluster mass, does not show any significant radial trend. Conclusions. Our results appear consistent with a scenario in which SF galaxies evolve into passive galaxies due to density-dependent environmental processes and eventually get destroyed very near the cluster center to become part of a diffuse intracluster medium. Dynamical friction, on the other hand, does not seem to play an important role. Future investigations of other clusters of the CLASH-VLT sample will allow us to confirm our interpretation

CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847

Aims. We constrain the mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 CLASH cluster MACS J1206.2-0847, using the projected phase-space distribution of cluster galaxies in combination with gravitational lensing. Methods. We use an unprecedented data-set of â‰600 redshifts for cluster members, obtained as part of a VLT/VIMOS large program, to constrain the cluster mass profile over the radial range ~0-5 Mpc (0-2.5 virial radii) using the MAMPOSSt and Caustic methods. We then add external constraints from our previous gravitational lensing analysis. We invert the Jeans equation to obtain the velocity-anisotropy profiles of cluster members. With the mass-density and velocity-anisotropy profiles we then obtain the first determination of a cluster pseudo-phase-space density profile. Results. The kinematics and lensing determinations of the cluster mass profile are in excellent agreement. This is very well fitted by a NFW model with mass M200 = (1.4 ± 0.2) × 1015 M ⊙ and concentration c200 = 6 ± 1, only slightly higher than theoretical expectations. Other mass profile models also provide acceptable fits to our data, of (slightly) lower (Burkert, Hernquist, and Softened Isothermal Sphere) or comparable (Einasto) quality than NFW. The velocity anisotropy profiles of the passive and star-forming cluster members are similar, close to isotropic near the center and increasingly radial outside. Passive cluster members follow extremely well the theoretical expectations for the pseudo-phase-space density profile and the relation between the slope of the mass-density profile and the velocity anisotropy. Star-forming cluster members show marginal deviations from theoretical expectations. Conclusions. This is the most accurate determination of a cluster mass profile out to a radius of 5 Mpc, and the only determination of the velocity-anisotropy and pseudo-phase-space density profiles of both passive and star-forming galaxies for an individual cluster. These profiles provide constraints on the dynamical history of the cluster and its galaxies. Prospects for extending this analysis to a larger cluster sample are discussed. © ESO, 2013

Intracluster light properties in the CLASH-VLT cluster MACS J1206.2-0847

Aims. We aim constrain the assembly history of clusters by studying the intracluster light (ICL) properties, estimating its contribution to the fraction of baryons in stars, f, and understanding possible systematics or bias using different ICL detection techniques. Methods. We developed an automated method, GALtoICL, based on the software GALAPAGOS, to obtain a refined version of typical BCG+ICL maps. We applied this method to our test case MACS J1206.2-0847, a massive cluster located at z ∼ 0:44, which is part of the CLASH sample. Using deep multiband Subaru images, we extracted the surface brightness (SB) profile of the BCG+ICL and studied the ICL morphology, color, and contribution to fout to R500. We repeated the same analysis using a different definition of the ICL, SBlimit method, i.e., a SB cut-off level, to compare the results. Results. The most peculiar feature of the ICL in MACS1206 is its asymmetric radial distribution, with an excess in the SE direction and extending toward the second brightest cluster galaxy, which is a post starburst galaxy. This suggests an interaction between the BCG and this galaxy that dates back to τ 1.5 Gyr. The BCG+ICL stellar content is ∼8% of M 500, and the (de-) projected baryon fraction in stars is f= 0:0177(0:0116), in excellent agreement with recent results. The SBlimit method provides systematically higher ICL fractions and this effect is stronger at lower SB limits. This is due to the light from the outer envelopes of member galaxies that contaminate the ICL. Though more time consuming, the GALtoICL method provides safer ICL detections that are almost free of this contamination. This is one of the few ICL study at redshift z 0:3. At completion, the CLASH/VLT program will allow us to extend this analysis to a statistically significant cluster sample spanning a wide redshift range: 0:2 ≲ z ≲ 0:6. © 2014 ESO