Enhanced thermionic-dominated photoresponse in graphene Schottky junctions

Vertical heterostructures of van der Waals materials enable new pathways to tune charge and energy transport characteristics in nanoscale systems. We propose that graphene Schottky junctions can host a special kind of photoresponse which is characterized by strongly coupled heat and charge flows that run vertically out of the graphene plane. This regime can be accessed when vertical energy transport mediated by thermionic emission of hot carriers overwhelms electron-lattice cooling as well as lateral diffusive energy transport. As such, the power pumped into the system is efficiently extracted across the entire graphene active area via thermionic emission of hot carriers into a semiconductor material. Experimental signatures of this regime include a large and tunable internal responsivity ${\cal R}$ with a non-monotonic temperature dependence. In particular, ${\cal R}$ peaks at electronic temperatures on the order of the Schottky potential $\phi$ and has a large upper limit ${\cal R} \le e/\phi$ ($e/\phi=10\,{\rm A/W}$ when $\phi = 100\,{\rm meV}$). Our proposal opens up new approaches for engineering the photoresponse in optically-active graphene heterostructures.Comment: 6 pages, 2 figure

Normal state magnetotransport properties of β\beta-FeSe superconductors

We present $\beta$-FeSe magnetotransport data, and describe them theoretically. Using a simplified microscopic model with two correlated effective orbitals, we determined the normal state electrical conductivity and Hall coefficient, using Kubo formalism. With model parameters relevant for Fe-chalcogenides, we describe the observed effect of the structural transition on the ab-plane electrical resistivity, as well as on the magnetoresistance. Temperature-dependent Hall coefficient data were measured at 16 Tesla, and their theoretical description improves upon inclusion of moderate electron correlations. We confirm the effect of the structural transition on the electronic structure, finding deformation-induced band splittings comparable to those reported in angle-resolved photoemission.Comment: 6 pages, 5 figure

Dynamical mass of the O-type supergiant in Zeta Orionis A

A close companion of Zeta Orionis A was found in 2000 with the Navy Precision Optical Interferometer (NPOI), and shown to be a physical companion. Because the primary is a supergiant of type O, for which dynamical mass measurements are very rare, the companion was observed with NPOI over the full 7-year orbit. Our aim was to determine the dynamical mass of a supergiant that, due to the physical separation of more than 10 AU between the components, cannot have undergone mass exchange with the companion. The interferometric observations allow measuring the relative positions of the binary components and their relative brightness. The data collected over the full orbital period allows all seven orbital elements to be determined. In addition to the interferometric observations, we analyzed archival spectra obtained at the Calar Alto, Haute Provence, Cerro Armazones, and La Silla observatories, as well as new spectra obtained at the VLT on Cerro Paranal. In the high-resolution spectra we identified a few lines that can be associated exclusively to one or the other component for the measurement of the radial velocities of both. The combination of astrometry and spectroscopy then yields the stellar masses and the distance to the binary star. The resulting masses for components Aa of 14.0 solar masses and Ab of 7.4 solar masses are low compared to theoretical expectations, with a distance of 294 pc which is smaller than a photometric distance estimate of 387 pc based on the spectral type B0III of the B component. If the latter (because it is also consistent with the distance to the Orion OB1 association) is adopted, the mass of the secondary component Ab of 14 solar masses would agree with classifying a star of type B0.5IV. It is fainter than the primary by about 2.2 magnitudes in the visual. The primary mass is then determined to be 33 solar masses

C II abundances in early-type stars: solution to a notorious non-LTE problem

We address a long-standing discrepancy between non-LTE analyses of the prominent C II 4267 and 6578/82 A multiplets in early-type stars. A comprehensive non-LTE model atom of C II is constructed based on critically selected atomic data. This model atom is used for an abundance study of six apparently slow-rotating main-sequence and giant early B-type stars. High-resolution and high-S/N spectra allow us to derive highly consistent abundances not only from the classical features but also from up to 18 further C II lines in the visual - including two so far unreported emission features equally well reproduced in non-LTE. These results require the stellar atmospheric parameters to be determined with care. A homogeneous (slightly) sub-solar present-day carbon abundance from young stars in the solar vicinity (in associations and in the field) of log C/H +12= 8.29+/-0.03 is indicated.Comment: 8 pages, 5 figure

An asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry

The O9V star HD 46202, which is a member of the young open cluster NGC 2244, was observed by the CoRoT satellite in October/November 2008 during a short run of 34 days. From the very high-precision light curve, we clearly detect beta Cep-like pulsation frequencies with amplitudes of ~0.1 mmag and below. A comparison with stellar models was performed using a chi^2 as a measure for the goodness-of-fit between the observed and theoretically computed frequencies. The physical parameters of our best-fitting models are compatible with the ones deduced spectroscopically. A core overshooting parameter alpha_ov = 0.10 +- 0.05 pressure scale height is required. None of the observed frequencies are theoretically excited with the input physics used in our study. More theoretical work is thus needed to overcome this shortcoming in how we understand the excitation mechanism of pulsation modes in such a massive star. A similar excitation problem has also been encountered for certain pulsation modes in beta Cep stars recently modelled asteroseismically.Comment: Accepted for publication in Astronomy and Astrophysics on 17/12/2010, 9 pages, 7 figures, 4 table

Anomalous Proximity Effect in Underdoped YBaCuO Josephson Junctions

Josephson junctions were photogenerated in underdoped thin films of the YBa$_2$Cu$_3$O$_{6+x}$ family using a near-field scanning optical microscope. The observation of the Josephson effect for separations as large as 100 nm between two wires indicates the existence of an anomalously large proximity effect and show that the underdoped insulating material in the gap of the junction is readily perturbed into the superconducting state. The critical current of the junctions was found to be consistent with the conventional Josephson relationship. This result constrains the applicability of SO(5) theory to explain the phase diagram of high critical temperature superconductors.Comment: 11 pages, 4 figure

Modelo anual de la dinámica sedimentaria en una marisma mareal mediterránea.

Se ha detectado un patrón estacional en la dinámica sedimentaria en zonas de marisma baja, relacionado con la distribución anual de las precipitaciones característica del clima mediterráneo, que induce cambios en el caudal de los ríos y en la cantidad y distribución de los aportes de partículas finas que entran en el estuario. En este escenario se pone de manifiesto cómo la presencia de vegetación (Spartina maritima) favorece la acreción y estabilización de sedimentos. En planicies desprovistas de vegetación, los mayores niveles de acreción se registran durante primavera y principios de verano. Las lluvias otoñales determinan un aumento del caudal de los ríos, con un incremento en el aporte de sedimentos y removilización de éstos en las zonas desnudas. Parte de estos sedimentos quedarán entonces retenidos en las zonas provistas de vegetación. Durante este periodo de otoño es cuando esta vegetación alcanza sus mayores valores de biomasa, maximizando así su papel como estabilizador de sedimentos.We have found a seasonal pattern operating on the lower areas of a tidal marsh, in relation to the characteristic annual distribution of the rainfall in a Mediterranean climate which induces changes in river flows and in quantity and distribution of loam sediments entering the estuary. Also, the presence of vegetation (S. maritima) favours the accretion rate and the sediment stabilization. Bare muds record the maximum values of accretion during Spring and early Summer. Autumn rainfalls increase the river flow what means a new input of sediments and the movilization of the old ones from the bare muds; the vegetation raises the maximum biomass and it traps and stabilizes these sediments.Dirección General de Investigación Científica y Técnica. Gobierno de España-PB94-145