Magnetic activity and differential rotation in the young Sun-like stars KIC 7985370 and KIC 7765135

Aims. We present a detailed study of the two Sun-like stars KIC 7985370 and KIC 7765135, to determine their activity level, spot distribution, and differential rotation. Both stars were previously discovered by us to be young stars and were observed by the NASA Kepler mission. Methods. The fundamental stellar parameters (vsini, spectral type, T_eff, log g, and [Fe/H]) were derived from optical spectroscopy by comparison with both standard-star and synthetic spectra. The spectra of the targets allowed us to study the chromospheric activity based on the emission in the core of hydrogen Hα and Ca ii infrared triplet (IRT) lines, which was revealed by the subtraction of inactive templates. The high-precision Kepler photometric data spanning over 229 days were then fitted with a robust spot model. Model selection and parameter estimation were performed in a Bayesian manner, using a Markov chain Monte Carlo method. Results. We find that both stars are Sun-like (of G1.5 V spectral type) and have an age of about 100–200 Myr, based on their lithium content and kinematics. Their youth is confirmed by their high level of chromospheric activity, which is comparable to that displayed by the early G-type stars in the Pleiades cluster. The Balmer decrement and flux ratio of their Ca ii-IRT lines suggest that the formation of the core of these lines occurs mainly in optically thick regions that are analogous to solar plages. The spot model applied to the Kepler photometry requires at least seven persistent spots in the case of KIC 7985370 and nine spots in the case of KIC 7765135 to provide a satisfactory fit to the data. The assumption of the longevity of the star spots, whose area is allowed to evolve with time, is at the heart of our spot-modelling approach. On both stars, the surface differential rotation is Sun-like, with the high-latitude spots rotating slower than the low-latitude ones. We found, for both stars, a rather high value of the equator-to-pole differential rotation (dΩ ≈ 0.18 rad d^-1), which disagrees with the predictions of some mean-field models of differential rotation for rapidly rotating stars. Our results agree instead with previous works on solar-type stars and other models that predict a higher latitudinal shear, increasing with equatorial angular velocity, that can vary during the magnetic cycle.

Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter

Context. Chromospheric activity produces both photometric and spectroscopic variations that can be mistaken as planets. Large spots crossing the stellar disc can produce planet-like periodic variations in the light curve of a star. These spots clearly affect the spectral line profiles, and their perturbations alter the line centroids creating a radial velocity jitter that might “contaminate” the variations induced by a planet. Precise chromospheric activity measurements are needed to estimate the activity-induced noise that should be expected for a given star. Aims. We obtain precise chromospheric activity measurements and projected rotational velocities for nearby (d ≤ 25 pc) cool (spectral types F to K) stars, to estimate their expected activity-related jitter. As a complementary objective, we attempt to obtain relationships between fluxes in different activity indicator lines, that permit a transformation of traditional activity indicators, i.e., Ca II H & K lines, to others that hold noteworthy advantages. Methods. We used high resolution (~50 000) echelle optical spectra. Standard data reduction was performed using the IRAF ECHELLE package. To determine the chromospheric emission of the stars in the sample, we used the spectral subtraction technique. We measured the equivalent widths of the chromospheric emission lines in the subtracted spectrum and transformed them into fluxes by applying empirical equivalent width and flux relationships. Rotational velocities were determined using the cross-correlation technique. To infer activity-related radial velocity (RV) jitter, we used empirical relationships between this jitter and the R’_HK index. Results. We measured chromospheric activity, as given by different indicators throughout the optical spectra, and projected rotational velocities for 371 nearby cool stars. We have built empirical relationships among the most important chromospheric emission lines. Finally, we used the measured chromospheric activity to estimate the expected RV jitter for the active stars in the sample.

Estudio y aplicación de metaheurísticas y comparación con métodos exhaustivos

Cuando nos enfrentamos a problemas reales haciendo uso de recursos computacionales, hemos de tener en cuenta que el número de posibles soluciones candidatas a tener en cuenta puede llegar a ser tan inmenso que abordarlas mediante técnicas algorítmicas clásicas, en la mayoría de los casos, pueden llegar a convertirse en un problema en sí mismo debido al gran coste en recursos que pueden llegar a generar. En este contexto, aspectos como el tiempo utilizado en la búsqueda de una solución mediante algoritmos de búsqueda exhaustiva tales como fuerza bruta, vuelta atrás, ramificación y poda, etc., puede llegar a ser prohibitivo en la práctica. Ante este problema que se nos plantea, podemos hacer un estudio sobre otros métodos, tales como los metaheurísticos, que, aunque no siempre aseguran la optimalidad de las soluciones producidas; tienen un tiempo de ejecución mucho menor que los métodos exhaustivos. En el presente trabajo hemos seleccionado dos problemas NP-completos de entre los más famosos de la literatura y hemos realizado un estudio de ambos. Concretamente, los problemas seleccionados han sido el TSP (Traveling Salesman Problem) y el problema de la Mochila 0-1. Por otro lado, hemos llevado a cabo un estudio sobre distintas metaheurísticas para poder resolver los problemas mencionados. Entre estas metaheurísticas, hemos seleccionado cuatro: metaheurísticas evolutivas, metaheurísticas inspiradas en colonias de hormigas, metaheurísticas simulated annealing (enfriamiento simulado) y metaheurísticas GRASP (Greedy Randomized Adaptive Search Procedure). Después de esto, cada problema ha sido resuelto aplicando tanto algoritmos de búsqueda exhaustiva como metaheurísticas. Una vez adaptados los algoritmos a la resolución de los problemas concretos, hemos realizado un estudio experimental, donde se realizaron comparativas de rendimiento. Finalmente, todo este trabajo ha sido plasmado en el desarrollo de una aplicación software, la cual consta de dos partes: una que contiene la implementación los algoritmos adaptados para la resolución de los problemas y que son ofrecidos a modo de servicios web y otra parte donde se ha implementado un cliente web que puede consumir estos servicios y realizar una presentación más vistosa de la ejecución de los algoritmos y los resultados obtenidos. Esta arquitectura podrá servir como base para futuras ampliaciones de este estudio.

Space density distribution of galaxies in the absolute magnitude - rotation velocity plane: a volume-complete Tully-Fisher relation from CALIFA stellar kinematics

We measured the distribution in absolute magnitude - circular velocity space for a well-defined sample of 199 rotating galaxies of the Calar Alto Legacy Integral Field Area Survey (CALIFA) using their stellar kinematics. Our aim in this analysis is to avoid subjective selection criteria and to take volume and large-scale structure factors into account. Using stellar velocity fields instead of gas emission line kinematics allows including rapidly rotating early-type galaxies. Our initial sample contains 277 galaxies with available stellar velocity fields and growth curve r-band photometry. After rejecting 51 velocity fields that could not be modelled because of the low number of bins, foreground contamination, or significant interaction, we performed Markov chain Monte Carlo modelling of the velocity fields, from which we obtained the rotation curve and kinematic parameters and their realistic uncertainties. We performed an extinction correction and calculated the circular velocity v_circ accounting for the pressure support of a given galaxy. The resulting galaxy distribution on the M-r - v(circ) plane was then modelled as a mixture of two distinct populations, allowing robust and reproducible rejection of outliers, a significant fraction of which are slow rotators. The selection effects are understood well enough that we were able to correct for the incompleteness of the sample. The 199 galaxies were weighted by volume and large-scale structure factors, which enabled us to fit a volume-corrected Tully-Fisher relation (TFR). More importantly, we also provide the volume-corrected distribution of galaxies in the M_r - v_circ plane, which can be compared with cosmological simulations. The joint distribution of the luminosity and circular velocity space densities, representative over the range of -20 > M_r > -22 mag, can place more stringent constraints on the galaxy formation and evolution scenarios than linear TFR fit parameters or the luminosity function alone.