An algorithm for computing the 2D structure of fast rotating stars

Stars may be understood as self-gravitating masses of a compressible fluid whose radiative cooling is compensated by nuclear reactions or gravitational contraction. The understanding of their time evolution requires the use of detailed models that account for a complex microphysics including that of opacities, equation of state and nuclear reactions. The present stellar models are essentially one-dimensional, namely spherically symmetric. However, the interpretation of recent data like the surface abundances of elements or the distribution of internal rotation have reached the limits of validity of one-dimensional models because of their very simplified representation of large-scale fluid flows. In this article, we describe the ESTER code, which is the first code able to compute in a consistent way a two-dimensional model of a fast rotating star including its large-scale flows. Compared to classical 1D stellar evolution codes, many numerical innovations have been introduced to deal with this complex problem. First, the spectral discretization based on spherical harmonics and Chebyshev polynomials is used to represent the 2D axisymmetric fields. A nonlinear mapping maps the spheroidal star and allows a smooth spectral representation of the fields. The properties of Picard and Newton iterations for solving the nonlinear partial differential equations of the problem are discussed. It turns out that the Picard scheme is efficient on the computation of the simple polytropic stars, but Newton algorithm is unsurpassed when stellar models include complex microphysics. Finally, we discuss the numerical efficiency of our solver of Newton iterations. This linear solver combines the iterative Conjugate Gradient Squared algorithm together with an LU-factorization serving as a preconditionner of the Jacobian matrix.Comment: 40 pages, 12 figures, accepted in J. Comput. Physic

Physical processes leading to surface inhomogeneities: the case of rotation

In this lecture I discuss the bulk surface heterogeneity of rotating stars, namely gravity darkening. I especially detail the derivation of the omega-model of Espinosa Lara & Rieutord (2011), which gives the gravity darkening in early-type stars. I also discuss the problem of deriving gravity darkening in stars owning a convective envelope and in those that are members of a binary system.Comment: 23 pages, 11 figure, Lecture given to the school on the cartography of the Sun and the stars (May 2014 in Besan\c{c}on), to appear in LNP, Neiner and Rozelot edts V2: typos correcte

Neutrino Masses in the Lee-Wick Standard Model

Recently, an extension of the standard model based on ideas of Lee and Wick has been discussed. This theory is free of quadratic divergences and hence has a Higgs mass that is stable against radiative corrections. Here, we address the question of whether or not it is possible to couple very heavy particles, with masses much greater than the weak scale, to the Lee-Wick standard model degrees of freedom and still preserve the stability of the weak scale. We show that in the LW-standard model the familiar see-saw mechanism for generating neutrino masses preserves the solution to the hierarchy puzzle provided by the higher derivative terms. The very heavy right handed neutrinos do not destabilize the Higgs mass. We give an example of new heavy degrees of freedom that would destabilize the hierarchy, and discuss a general mechanism for coupling other heavy degrees of freedom to the Higgs doublet while preserving the hierarchy.Comment: 7 pages, 1 figur

Black holes and Higgs stability

We study the effect of primordial black holes on the classical rate of nucleation of AdS regions within the standard electroweak vacuum. We find that the energy barrier for transitions to the new vacuum, which characterizes the exponential suppression of the nucleation rate, can be reduced significantly in the black-hole background. A precise analysis is required in order to determine whether the the existence of primordial black holes is compatible with the form of the Higgs potential at high temperature or density in the Standard Model or its extensions.Comment: 27 pages, 10 figures, conclusions expanded, to appear in JCA

Economic analysis of potato, corn and wheat response to nitrogen and phosphorus application in the highlands of Ecuador

Cover title.Includes bibliographical references (page 39)

Condensation in an Economic Model with Brand Competition

We present a linear agent based model on brand competition. Each agent belongs to one of the two brands and interacts with its nearest neighbors. In the process the agent can decide to change to the other brand if the move is beneficial. The numerical simulations show that the systems always condenses into a state when all agents belong to a single brand. We study the condensation times for different parameters of the model and the influence of different mechanisms to avoid condensation, like anti monopoly rules and brand fidelity.Comment: Accepted in: International Journal of Modern Physics

Comprehensive study of Leon-Queretaro area

There are no author-identified significant results in this report

Ineficiencia en la Distribución de Energía Eléctrica: Una Aplicación de las Funciones de Distancia Estocástica

Este documento evalúa el desempeño de las empresas distribuidoras de energía durante el periodo 1999-2003, utilizando la metodología de funciones de distancia estocástica, la cual a través de la estimación de las desviaciones de una función ideal de producción, permite medir los niveles de eficiencia técnica de las diferentes empresas. Los resultados indican que existen diferencias significativas en el desempeño de las empresas, sugiriendo que se podrían obtener importantes ganancias en términos de eficiencia técnica si las empresas operaran o se acercaran a los niveles de operación de las más eficientes. Estas ganancias se podrían expresar en el ahorro de recursos, la calidad del servicio y/o en menores niveles de tarifas a los usuarios finales. También se encontró que el desempeño de las empresas distribuidoras de energía puede verse afectado por factores fuera del control de las firmas, tales como las condiciones geográficas, el número de usuarios atendidos y la densidad poblacional. En particular, se encuentra que empresas con un entorno más favorable en términos de densidad poblacional y/o de los niveles de consumo de los usuarios se ven favorecidas cuando dichas variables afectan directamente la tecnología de producción. Por otra parte, se observa que las empresas públicas registran un mejor desempeño cuando las variables ambientales afectan directamente la eficiencia y no la función de producción. Estos resultados sugieren que las empresas privadas se podrían estar beneficiando de condiciones de entorno más favorables, teniendo en cuenta que estas, en promedio atienden áreas de más alta densidad poblacional y usuarios de consumos más altos.