A propósito de "Sangre y arena" de Vicente Blasco Ibáñez: miradas a un opúsculo que costaba 10 céntimos

Relaciones estilísticas entre la novela Sangre y arena, la adaptación cinematográfica que dé ella hizo el mismo Blasco Ibáñez en 1916 y un opúsculo que se publicó relacionado con ésta

Chanson D´Automne de Verlaine. Evaluation d´une traduction en castillan

En el marco de una investigación sobre la posibilidad de traducir poesía, y sobre cuales podrían ser las condiciones en las que esta clase de traducción fuese realizable, se intenta aquí el ana lisis de un caso límite: Chanson d'Automne de Verlaine; y se examina la traducción española en verso hecha por Emilio Carrere (1921).Dans le cadre d'une recherche plus vaste sur la possibilité de traduire la poésie et les conditions de réalisation de ce type de traduction, nous analysons un cas limite: Chanson d'automne de Verlaine. Après une analyse fouillée du texte-source et des relations entre forme (signifiant; recours métriques; sons; points d'articulation, etc.) et signification / signifiance, nous tentons l'évaluation d'une traduction espagnole en vers de ce texte: celle d'Emilio Carrere (1921).I intent to make an evaluation of the posibility of translating the poetry of Verlaine and the specific dificulties due to his poetics, analysing the Spanish translation of Chanson d'Automne by Emilio Carrere (1921)

Probing the Inner Disk Emission of the Herbig Ae Stars HD 163296 and HD 190073

The physical processes occurring within the inner few astronomical units of proto-planetary disks surrounding Herbig Ae stars are crucial to setting the environment in which the outer planet-forming disk evolves and put critical constraints on the processes of accretion and planet migration. We present the most complete published sample of high angular resolution H- and K-band observations of the stars HD 163296 and HD 190073, including 30 previously unpublished nights of observations of the former and 45 nights of the latter with the CHARA long-baseline interferometer, in addition to archival VLTI data. We confirm previous observations suggesting significant near-infrared emission originates within the putative dust evaporation front of HD 163296 and show this is the case for HD 190073 as well. The H- and K-band sizes are the same within $(3 \pm 3)\%$ for HD 163296 and within $(6 \pm 10)\%$ for HD 190073. The radial surface brightness profiles for both disks are remarkably Gaussian-like with little or no sign of the sharp edge expected for a dust evaporation front. Coupled with spectral energy distribution analysis, our direct measurements of the stellar flux component at H and K bands suggest that HD 190073 is much younger (<400 kyr) and more massive (~5.6 M$_\odot$) than previously thought, mainly as a consequence of the new Gaia distance (891 pc).Comment: 19 pages, 6 figure

The Small Separation A-Star Companion Population: First Results with CHARA/MIRC-X

We present preliminary results from our long-baseline interferometry (LBI) survey to constrain the multiplicity properties of intermediate-mass A-type stars within 80pc. Previous multiplicity studies of nearby stars exhibit orbital separation distributions well-fitted with a log-normal with peaks > 15au, increasing with primary mass. The A-star multiplicity survey of De Rosa et al. (2014), sensitive beyond 30au but incomplete below 100 au, found a log-normal peak around 390au. Radial velocity surveys of slowly-rotating, chemically peculiar Am stars identified a significant number of very close companions with periods $\leq$ 5 days, ~ 0.1au, a result similar to surveys of O- and B-type primaries. With the improved performance of LBI techniques, we can probe these close separations for normal A-type stars where other surveys are incomplete. Our initial sample consists of 27 A-type primaries with estimated masses between 1.44-2.49M$_{\odot}$ and ages 10-790Myr, which we observed with the MIRC-X instrument at the CHARA Array. We use the open source software CANDID to detect five companions, three of which are new, and derive a companion frequency of 0.19$^{+0.11}_{-0.06}$ over mass ratios 0.25-1.0 and projected separations 0.288-5.481 au. We find a probability of 10$^{-6}$ that our results are consistent with extrapolations based on previous models of the A-star companion population, over mass ratios and separations sampled. Our results show the need to explore these very close separations to inform our understanding of stellar formation and evolution processes.Comment: 14 pages, 3 figures, Accepted to the Astrophysical Journal on Nov. 2, 202

Dusty disk winds at the sublimation rim of the highly inclined, low mass YSO SU Aurigae

T Tauri stars are low-mass young stars whose disks provide the setting for planet formation. Despite this, their structure is poorly understood. We present new infrared interferometric observations of the SU Aurigae circumstellar environment that offer 3 x higher resolution and better baseline position angle coverage over previous observations. We investigate the characteristics of circumstellar material around SU Aur, constrain the disk geometry, composition and inner dust rim structure. The CHARA array offers opportunities for long baseline observations, with baselines up to 331 m. Using the CLIMB 3-telescope combiner in the K-band allows us to measure visibilities as well as closure phase. We undertook image reconstruction for model-independent analysis, and geometric modeling. Additionally, the fitting of radiative transfer models constrains the physical parameters of the disk. For the first time, a dusty disk wind is introduced to the radiative transfer code TORUS to model protoplanetary disks. Our implementation is motivated by theoretical dusty disk winds, where magnetic field lines drive dust above the disk plane close to the sublimation zone. Image reconstruction reveals an inclined disk with slight asymmetry along its minor-axis, likely due to inclination effects obscuring the inner disk rim through absorption of incident star light on the near-side and thermal re-emission/scattering of the far-side. Geometric modelling of a skewed ring finds the inner rim at 0.17+/-0.02 au with an inclination of 50.9+/-1.0 degrees and minor axis position angle 60.8+/-1.2 degrees. Radiative transfer modelling shows a flared disk with an inner radius at 0.18 au which implies a grain size of 0.4 um and a scale height of 15.0 au at 100 au. Among the tested radiative transfer models, only the dusty disk wind successfully accounts for the K-band excess by introducing dust above the mid-plane.Comment: Accepted for publication in Astronomy \& Astrophysic

Micro-contextual identification of archaeological lipid biomarkers using resin-impregnated sediment slabs

Characterizing organic matter preserved in archaeological sediment is crucial to behavioral and paleoenvironmental investigations. This task becomes particularly challenging when considering microstratigraphic complexity. Most of the current analytical methods rely on loose sediment samples lacking spatial and temporal resolution at a microstratigraphic scale, adding uncertainty to the results. Here, we explore the potential of targeted molecular and isotopic biomarker analysis on polyester resin-impregnated sediment slabs from archaeological micromorphology, a technique that provides microstratigraphic control. We performed gas chromatography-mass spectrometry (GC-MS) and gas chromatography-isotope ratio mass spectromety (GC-IRMS) analyses on a set of samples including drill dust from resin-impregnated experimental and archaeological samples, loose samples from the same locations and resin control samples to assess the degree of interference of polyester resin in the GC-MS and Carbon-IRMS signals of different lipid fractions (n-alkanes, aromatics, n-ketones, alcohols, fatty acids and other high polarity lipids). The results show that biomarkers within the n-alkane, aromatic, n-ketone, and alcohol fractions can be identified. Further work is needed to expand the range of identifiable lipid biomarkers. This study represents the first micro-contextual approach to archaeological lipid biomarkers and contributes to the advance of archaeological science by adding a new method to obtain behavioral or paleoenvironmental proxies.This study has been funded by an ERC-Paleochar Consolidator Grant Project (ERC-2014-CoG-648871-PALEOCHAR). Archaeological research at El Salt is currently funded by the Spanish Ministry of Science and Innovation (Project PID2019-107113RB-I00) and was funded by the Spanish Ministry of Economy, Industry and Competitiveness (Project HAR2015-68321-P) when sampling for this study took place. Additional financial support for El Salt fieldwork is from the Cultural Heritage Department of the Valencia Government and the Archaeological Museum Camil Visedo Moltó of Alcoy. Research at the Axlor site is funded by the Spanish Ministry of Science and Innovation (Project PID2019-107260GB-I00, PID2019-107113RB-I00). Research at Crvena Stijena is funded by the Montenegrin Ministry of Culture, the Montenegrin Academy of Sciences, the United States National Science Foundation (NSF-BCS 1758285), and the University of Minnesota’s Office of the Vice President of Research Grant-in-Aid program. Research at Cape Esperberg is funded by a collaborative grant from the US National Science Foundation (ARC-1523160, ARC-1523205, ARC-1523059, ARC-1523079) and from the Archeology Commission of the French Ministry of Foreign Affairs