Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>We give a possible splitting method to a Hamiltonian for the description of charged particles moving around the Reissner–Nordström-(anti)-de Sitter black hole with an external magnetic field. This Hamiltonian can be separated into six analytical solvable pieces, whose solutions are explicit functions of proper time. In this case, second- and fourth-order explicit symplectic integrators are easily available. They exhibit excellent long-term behavior in maintaining the boundness of Hamiltonian errors regardless of ordered or chaotic orbits if appropriate step sizes are chosen. Under some circumstances, an increase of the positive cosmological constant gives rise to strengthening the extent of chaos from the global phase space; namely, chaos of charged particles occurs easily for the accelerated expansion of the universe. However, an increase of the magnitude of the negative cosmological constant does not. The different contributions to chaos are because the cosmological constant acts as a repulsive force in the Reissner–Nordström-de Sitter black hole, but an attractive force in the Reissner–Nordström-anti-de Sitter black hole.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The solar radio flux at F10.7 and F30 cm is required by most models characterizing the state of the Earth’s upper atmosphere, such as the thermosphere and ionosphere, to specify satellite orbits, re-entry services, collision avoidance maneuvers, and modeling of the evolution of space debris. We develop a method called RESONANCE (Radio Emissions from the Sun: ONline ANalytical Computer-aided Estimator) for the prediction of the 13-month smoothed monthly mean F10.7 and F30 indices 1–24 months ahead. The prediction algorithm has three steps. First, we apply a 13-month optimized running mean technique to effectively reduce the noise in the radio flux data. Second, we provide initial predictions of the F10.7 and F30 indices using the McNish–Lincoln method. Finally, we improve these initial predictions by developing an adaptive Kalman filter with identification of the error statistics. The rms error of predictions with lead times from 1 to 24 months is 5–27 solar flux units (sfu) for the F10.7 index and 3–16 sfu for F30, which statistically outperforms current algorithms in use. The proposed approach based on the Kalman filter is universal and can be applied to improve the initial predictions of a process under study provided by any other forecasting method. Furthermore, we present a systematic evaluation of re-entry forecast as an application to test the performance of F10.7 predictions on past ESA re-entry campaigns for payloads, rocket bodies, and space debris that re-entered from 2006 to 2019 June. The test results demonstrate that the predictions obtained by RESONANCE in general also lead to improvements in the forecasts of re-entry epochs.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present a statistical study of the largest bibliographic compilation of stellar and orbital parameters of W UMa stars derived by light-curve synthesis with Roche models. The compilation includes nearly 700 individually investigated objects from over 450 distinct publications. Almost 70% of this sample is comprised of stars observed in the past decade that have not been considered in previous statistical studies. We estimate the ages of the cataloged stars, model the distributions of their periods, mass ratios, temperatures, and other quantities, and compare them with the data from the Catalina Real-Time Transient Survey, LAMOST, and Gaia archives. As only a small fraction of the sample has radial-velocity curves, we examine the reliability of the photometric mass ratios in totally and partially eclipsing systems and find that totally eclipsing W UMa stars with photometric mass ratios have the same parameter distributions as those with spectroscopic mass ratios. Most of the stars with reliable parameters have mass ratios below 0.5 and orbital periods shorter than 0.5 days. Stars with longer periods and temperatures above 7000 K stand out as outliers and should not be labeled W UMa binaries. The collected data are available as an online database at <jats:ext-link xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="uri" xlink:href="https://wumacat.aob.rs" xlink:type="simple">https://wumacat.aob.rs</jats:ext-link>.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The ∼200,000 targets monitored for photometric variability during the Kepler prime mission include the best-studied group of stars in the sky, due both to the extensive time history provided by Kepler and to the substantial amount of ancillary data provided by other investigators or compiled by the Kepler team. To complement this wealth of data, we surveyed the entire Kepler field using the 3.6 and 4.5 <jats:italic>μ</jats:italic>m bands of the Warm Spitzer Space Telescope, obtaining photometry in both bands for almost 170,000 objects. We demonstrate relative photometric precision ranging from better than ∼1.5% for the brighter stars down to slightly greater than ∼2% for the faintest stars monitored by Kepler. We describe the data collection and analysis phases of this work and identify several stars with large infrared excess, although none that is also known to be the host of an exoplanetary system. The final catalog resulting from this work will be available at the NASA Exoplanet Archive.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>An error in the gravitational force that the source of gravity induces on itself (a self-force error) violates both the conservation of linear momentum and the conservation of energy. If such errors are present in a self-gravitating system and are not sufficiently random to average out, the obtained numerical solution will become progressively more unphysical with time: the system will acquire or lose momentum and energy due to numerical effects. In this paper, we demonstrate how self-force errors can arise in the case where self-gravity is solved on an adaptively refined mesh when the refinement is nonuniform. We provide the analytical expression for the self-force error and numerical examples that demonstrate such self-force errors in idealized settings. We also show how these errors can be corrected to an arbitrary order by straightforward addition of correction terms at the refinement boundaries.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present <jats:monospace>allesfitter</jats:monospace>, a public and open-source <jats:monospace>Python</jats:monospace> software for flexible and robust inference of stars and exoplanets given photometric and radial velocity data. <jats:monospace>Allesfitter</jats:monospace> offers a rich selection of orbital and transit/eclipse models, accommodating multiple exoplanets, multistar systems, transit-timing variations, phase curves, stellar variability, starspots, stellar flares, and various systematic noise models, including Gaussian processes. It features both parameter estimation and Bayesian model selection, allowing either a Markov Chain Monte Carlo or Nested Sampling fit to be easily run. For novice users, a graphical user interface allows all input and perform analyses to be specified; for <jats:monospace>Python</jats:monospace> users, all modules can be readily imported into any existing script. <jats:monospace>Allesfitter</jats:monospace> also produces publication-ready tables, LaTeX commands, and figures. The software is publicly available (<jats:ext-link xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="uri" xlink:href="https://github.com/MNGuenther/allesfitter" xlink:type="simple">https://github.com/MNGuenther/allesfitter</jats:ext-link>), <jats:monospace>pip</jats:monospace>-installable (<jats:monospace>pip install allesfitter</jats:monospace>), and well documented (<jats:ext-link xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="uri" xlink:href="http://www.allesfitter.com" xlink:type="simple">www.allesfitter.com</jats:ext-link>). Finally, we demonstrate the software’s capabilities in several examples and provide updates to the literature where possible for Pi Mensae, TOI-216, WASP-18, KOI-1003, and GJ 1243.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Massive stars have a strong impact on their local environments. However, how stellar feedback regulates star formation is still under debate. In this context, we studied the chemical properties of 80 dense cores in the Orion molecular cloud complex composed of the Orion A (39 cores), B (26 cores), and <jats:italic>λ</jats:italic> Orionis (15 cores) clouds using multiple molecular line data taken with the Korean Very Long Baseline Interferometry Network 21 m telescopes. The <jats:italic>λ</jats:italic> Orionis cloud has an H <jats:sc>ii</jats:sc> bubble surrounding the O-type star <jats:italic>λ</jats:italic> Ori, and hence it is exposed to the ultraviolet (UV) radiation field of the massive star. The abundances of C<jats:sub>2</jats:sub>H and HCN, which are sensitive to UV radiation, appear to be higher in the cores in the <jats:italic>λ</jats:italic> Orionis cloud than in those in the Orion A and B clouds, while the HDCO to H<jats:sub>2</jats:sub>CO abundance ratios show the opposite trend, indicating warmer conditions in the <jats:italic>λ</jats:italic> Orionis cloud. The detection rates of dense gas tracers such as the N<jats:sub>2</jats:sub>H<jats:sup>+</jats:sup>, HCO<jats:sup>+</jats:sup>, and H<jats:sup>13</jats:sup>CO<jats:sup>+</jats:sup> lines are also lower in the <jats:italic>λ</jats:italic> Orionis cloud. These chemical properties imply that the cores in the <jats:italic>λ</jats:italic> Orionis cloud are heated by UV photons from <jats:italic>λ</jats:italic> Ori. Furthermore, the cores in the <jats:italic>λ</jats:italic> Orionis cloud do not show any statistically significant excess in the infall signature of HCO<jats:sup>+</jats:sup> (1–0), unlike those in the Orion A and B clouds. Our results support the idea that feedback from massive stars impacts star formation in a negative way by heating and evaporating dense materials, as in the <jats:italic>λ</jats:italic> Orionis cloud.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present <jats:monospace>piXedfit</jats:monospace>, pixelized spectral energy distribution (SED) fitting, a Python package that provides tools for analyzing spatially resolved properties of galaxies using multiband imaging data alone or in combination with integral field spectroscopy (IFS) data. It has six modules that can handle all tasks in the spatially resolved SED fitting. The SED-fitting module uses the Bayesian inference technique with two kinds of posterior sampling methods: Markov Chain Monte Carlo (MCMC) and random dense sampling of parameter space (RDSPS). We test the performance of the SED-fitting module using mock SEDs of simulated galaxies from IllustrisTNG. The SED fitting with both posterior sampling methods can recover physical properties and star formation histories of the IllustrisTNG galaxies well. We further test the performance of <jats:monospace>piXedfit</jats:monospace> modules by analyzing 20 galaxies observed by the CALIFA and MaNGA surveys. The data are comprised of 12-band imaging data from the Galaxy Evolution Explorer, SDSS, 2MASS, and WISE and the IFS data from CALIFA or MaNGA. The <jats:monospace>piXedfit</jats:monospace> package can spatially match (in resolution and sampling) the imaging and IFS data. By fitting only the photometric SEDs, <jats:monospace>piXedfit</jats:monospace> can predict the spectral continuum, <jats:italic>D<jats:sub>n</jats:sub> </jats:italic>4000, H<jats:sub> <jats:italic>α</jats:italic> </jats:sub>, and H<jats:sub> <jats:italic>β</jats:italic> </jats:sub> well. The star formation rate derived by <jats:monospace>piXedfit</jats:monospace> is consistent with that derived from H<jats:sub> <jats:italic>α</jats:italic> </jats:sub> emission. The RDSPS method gives equally good fitting results as the MCMC and is much faster. As a versatile tool, <jats:monospace>piXedfit</jats:monospace> is equipped with a parallel computing module for efficient analysis of large data sets and will be made publicly available (<jats:ext-link xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="uri" xlink:href="https://github.com/aabdurrouf/piXedfit" xlink:type="simple">https://github.com/aabdurrouf/piXedfit</jats:ext-link>).</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The helioglow is the fluorescence of interstellar atoms inside the heliosphere, where they are excited by the solar EUV emission. So far, the helioglow of interstellar H and He has been detected. The helioglow features a characteristic distribution in the sky, which can be used to derive the properties of both interstellar neutral (ISN) gas and the solar wind. This requires a simulation model capable of catching with sufficient realism the essential coupling relations between the solar and interstellar factors. The solar factors include the solar wind flux and its variation with time and heliolatitude, as well as the heliolatitude and time variation of the solar EUV output. The ISN gas inside the heliosphere features a complex distribution function, which varies with time and location. The paper presents the first version of a WawHelioGlow simulation model for the helioglow flux using an optically thin, single-scattering approximation. The helioglow computations are based on a sophisticated kinetic treatment of the distribution functions of interstellar H and He provided by the (n)WTPM model. The model takes into account the heliolatitudinal and spectral variations of the solar EUV output from observations. We present a formulation of the model and the treatment of the solar spectral flux. The accompanying Paper II illustrates details of the line-of-sight evolution of the elements of the model and a brief comparison of results of the WawHelioGlow code with selected sky maps of the hydrogen helioglow, obtained by the SWAN instrument on board the Solar and Heliospheric Observatory mission.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The helioglow is the fluorescence of interstellar atoms inside the heliosphere, where they are excited by the solar EUV. Because the mean free path between collisions for interstellar gas is comparable to the size of the heliosphere, the distribution function of this gas inside the heliosphere strongly varies in space and with time and is non-Maxwellian. Coupling between realistically modeled solar factors and the distribution function of interstellar neutral gas is accounted for in a helioglow model that we have developed. WawHelioGlow is presented in the accompanying Paper I. Here, we present the evolution of the gas density, solar illumination, helioglow source function, and other relevant parameters building up the helioglow signal for selected lines of sight observed at 1 au. We compare these elements for various phases of the solar cycle, and we present the sensitivity of the results to the heliolatitudinal anisotropy of the solar EUV output. We assume a realistic latitudinal anisotropy of the solar wind flux using results from the analysis of interplanetary scintillations. We compare the simulated helioglow with selected maps observed by the SOHO/SWAN instrument. We demonstrate that WawHelioGlow is able to reproduce fundamental features of the sky distribution of the helioglow. For some phases of the solar cycle, the model with solar EUV output anisotropy better reproduces the observations, while for other phases, no EUV anisotropy is needed. In all simulated cases, the solar wind anisotropy following insight from interplanetary scintillation measurements is present.</jats:p>