Spin-coherent dynamics and carrier lifetime in strained Ge1−xSnx semiconductors on silicon

We demonstrate an effective epitaxial route for the manipulation and further enrichment of the intriguing spin-dependent phenomena boasted by germanium. We show optical initialization and readout of spins in Ge-rich germanium-tin alloys and report on spin quantum beats between Zeeman-split levels under an external magnetic field. While heavy Sn atoms can be readily utilized to strengthen the spin-orbit coupling, our experiments reveal robust spin orientation in a wide temperature range and a persistent spin lifetime that noticeably approaches the nanosecond regime at room temperature. In addition, time decay photoluminescence experiments evidence a temperature-induced monotonic decrease of the carrier lifetime, eventually providing crucial insights also into nonradiative recombination mechanisms

Carbon-enhanced metal-poor stars in the SDSS-APOGEE data base

We identify six new carbon-enhanced metal-poor (CEMP) stars ([C/Fe]>+ 0.7 and [Fe/H] < -1.8) and another seven likely candidates within the APOGEE data base following Data Release 12. These stars have chemical compositions typical of metal-poor halo stars, e.g. mean [a/Fe]=+0.24 +/- 0.24, based on the APOGEE Stellar Parameters and Chemical Abundances Pipeline results. A lack of heavy-element spectral lines impedes further sub-classification of these CEMP stars, however, based on radial velocity (RV) scatter, we predict most are not CEMP-s stars which are typically found in binary systems. Only one object, 2M15312547+4220551, may be in a binary since it exhibits a scatter in its RV of 1.7 +/- 0.6 km s(-1) based on three visits over a 25.98 d baseline. Optical observations are now necessary to confirm the stellar parameters and low metallicities of these stars, to determine the heavy-element abundance ratios and improve the precision in the derived abundances, and to examine their CEMP sub-classifications

Reevaluating the evidence for a Hadean-Eoarchean dynamo.

The time of origin of the geodynamo has important implications for the thermal evolution of the planetary interior and the habitability of early Earth. It has been proposed that detrital zircon grains from Jack Hills, Western Australia, provide evidence for an active geodynamo as early as 4.2 billion years (Ga) ago. However, our combined paleomagnetic, geochemical, and mineralogical studies on Jack Hills zircons indicate that most have poor magnetic recording properties and secondary magnetization carriers that postdate the formation of the zircons. Therefore, the existence of the geodynamo before 3.5 Ga ago remains unknown

Reevaluating the evidence for a Hadean-Eoarchean dynamo

The time of origin of the geodynamo has important implications for the thermal evolution of the planetary interior and the habitability of early Earth. It has been proposed that detrital zircon grains from Jack Hills, Western Australia, provide evidence for an active geodynamo as early as 4.2 billion years (Ga) ago. However, our combined paleomagnetic, geochemical, and mineralogical studies on Jack Hills zircons indicate that most have poor magnetic recording properties and secondary magnetization carriers that postdate the formation of the zircons. Therefore, the existence of the geodynamo before 3.5 Ga ago remains unknown

The Pristine Survey – VI. The first three years of medium-resolution follow-up spectroscopy of Pristine EMP star candidates★

We present the results of a 3-year long, medium-resolution spectroscopic campaign aimed at identifying very metal-poor stars from candidates selected with the CaHK, metallicity-sensitive Pristine survey. The catalogue consists of a total of 1007 stars, and includes 146 rediscoveries of metal-poor stars already presented in previous surveys, 707 new very metal-poor stars with [Fe/H]<−2.0⁠, and 95 new extremely metal-poor stars with [Fe/H]<−3.0⁠. We provide a spectroscopic [Fe/H] for every star in the catalogue, and [C/Fe] measurements for a subset of the stars (10% with [Fe/H]<−3 and 24% with −3<[Fe/H]<−2⁠) for which a carbon determination is possible, contingent mainly on the carbon abundance, effective temperature and S/N of the stellar spectra. We find an average carbon enhancement fraction ([C/Fe] ≥ +0.7) of 41 ± 4% for stars with −3<[Fe/H]<−2 and 58 ± 14% for stars with [Fe/H]<−3⁠, and report updated success rates for the Pristine survey of 56 % and 23 % to recover stars with [Fe/H]<−2.5 and [Fe/H]<−3⁠, respectively. Finally, we discuss the current status of the survey and its preparation for providing targets to upcoming multi-object spectroscopic surveys such as WEAVE

El sacramento de la penitencia: signo vital de reconciliación de cara al nuevo milenio

Una mirada actual al sacramento de la penitencia nos lleva a reconocerle comopresencia y acción reconciliadora de dimensión integral-globalizante. Partimosdel acontecimiento Jesucristo, profecía de perdón, desde la realidad de aquel Jeslísde Nazaret que se constituye en paradigma de justicia a partir de la transparenciade la misericordia de Dios Padre. La comunidad eclesial es expresión real en el hoyde la historia donde esta profecía se actualiza en la responsabilidad propia de laevangelización: ser signo eficaz de justicia en la lucha collfra el pecado personaly social. La acción reconciliadora no sólo desenmascara el pecado, sino al superarsu fuerza idolátrica, proyecta la vida hacia la verdadera liberación. Tal es lavitalidad sacramental de la penitencia de cara al nuevo milenio

Refining the Mediterranean "Messinian gap" with high-precision U-Pb zircon geochronology, central and northern Italy

""During the Messinian Salinity Crisis (MSC), the Mediterranean Basin recorded a well developed precessionally modulated cyclicity. The astronomical tuning of the Messinian deposits with the insolation curve reveals a ~90 kyr “Messinian gap”, corresponding to the evaporative draw down of the Mediterranean, with consequent erosion of the basin margins. and formation of the Messinian Erosional Surface (MES). In the Messinian deposits above. the MES, a distinctive volcanic ash bed with a biotite 40Ar\\\/39 Ar plateau corrected date of 5.50 ±0.04 Ma has been used to constrain the post-evaporitic phase of the MSC and to tune the sedimentary cycles to the insolation curve. Using high-precision CA-TIMS U-Pb dates on single zircon grains derived from two post-MES ash layers sampled in northern and central Italy, we obtained dates of 5.5351 ± 0.0051 Ma and 5.5392 ± 0.0088 Ma, respectively. Combining the new high-precision geochronology with the age model for the precessionally modulated cycles of the Messinian Lower Evaporites, we refine the duration of the “Messinian gap” to 50 kyr or less, which correlates with either the TG12 glacial interval alone, or both the TG12 and TG14 glacial intervals. This gap should encompass the draw down of the Mediterranean, its near-complete desiccation, and deposition of the thick Messinian halite layer."

Reevaluating the evidence for a Hadean-Eoarchean dynamo.

The time of origin of the geodynamo has important implications for the thermal evolution of the planetary interior and the habitability of early Earth. It has been proposed that detrital zircon grains from Jack Hills, Western Australia, provide evidence for an active geodynamo as early as 4.2 billion years (Ga) ago. However, our combined paleomagnetic, geochemical, and mineralogical studies on Jack Hills zircons indicate that most have poor magnetic recording properties and secondary magnetization carriers that postdate the formation of the zircons. Therefore, the existence of the geodynamo before 3.5 Ga ago remains unknown.NERC and ER

Estimating fundamental parameters of nearby M dwarfs from SPIRou spectra

International audienceWe present the results of a study aiming at retrieving the fundamental parameters of M dwarfs from spectra secured with SPIRou, the near-infrared high-resolution spectropolarimeter installed at the Canada-France-Hawaii Telescope (CFHT), in the framework of the SPIRou Legacy Survey (SLS). Our study relies on comparing observed spectra with two grids of synthetic spectra, respectively, computed from PHOENIX and MARCS model atmospheres, with the ultimate goal of optimizing the precision at which fundamental parameters can be determined. In this first step, we applied our technique to 12 inactive M dwarfs with effective temperatures (Teff) ranging from 3000 to 4000 K. We implemented a benchmark to carry out a comparison of the two models used in this study. We report that the choice of model has a significant impact on the results and may lead to discrepancies in the derived parameters of 30 K in Teff and 0.05 dex to 0.10 dex in surface gravity (log g) and metallicity ($\rm {[M/H]}$), as well as systematic shifts of up to 50 K in Teff and 0.4 dex log g and $\rm {[M/H]}$. The analysis is performed on high signal-to-noise ratio template SPIRou spectra, averaged over multiple observations corrected from telluric absorption features and sky lines, using both a synthetic telluric transmission model and principal component analysis. With both models, we retrieve Teff, log g, and $\rm {[M/H]}$ estimates in good agreement with reference literature studies, with internal error bars of about 30 K, 0.05 dex, and 0.1 dex, respectively