Fisiología bucal infantil: función y crecimiento de la cavidad oral del lactante

Todas las funciones que se realizan en la cavidad oral (respiración, succión, deglución, masticación y fonación), estimulan el crecimiento y desarrollo del tercio inferior de la cara. Por ello, el tipo de lactancia, así como los hábitos orales disfuncionales, pueden influir sobre la morfología definitiva de los maxilares y de la oclusión dentaria.

La caries del biberón. Qué es y cómo prevenirla

La caries del biberón es la aparición brusca de caries en los incisivos y molares temporales, relacionadas con el hábito de succionar el chupete o el biberón, impregnados de sustancias cariogénicas. Afecta a los niños en las primeras etapas de la vida. Los dientes de leche son fundamentales para diferentes funciones como la masticación y el habla. Este trabajo revisa cuáles son sus causas más comunes y las medidas preventivas más indicadas.

MAGIC TeV Gamma-Ray Observations of Markarian 421 during Multiwavelength Campaigns in 2006

Wide-range spectral coverage of blazar-type active galactic nuclei is of paramount importance for understanding the particle acceleration mechanisms assumed to take place in their jets. The Major Atmospheric Gamma Imaging Cerenkov (MAGIC) telescope participated in three multiwavelength (MWL) campaigns, observing the blazar Markarian (Mkn) 421 during the nights of April 28 and 29, 2006, and June 14, 2006. Aims. We analyzed the corresponding MAGIC very-high energy observations during 9 nights from April 22 to 30, 2006 and on June 14, 2006. We inferred light curves with sub-day resolution and night-by-night energy spectra. Methods. MAGIC detects γ-rays by observing extended air showers in the atmosphere. The obtained air-shower images were analyzed using the standard MAGIC analysis chain. Results. A strong γ-ray signal was detected from Mkn 421 on all observation nights. The flux (E > 250 GeV) varied on night-by-night basis between (0.92±0.11) × 10-10 cm-2 s-1 (0.57 Crab units) and (3.21±0.15) × 10-10 cm-2 s-1 (2.0 Crab units) in April 2006. There is a clear indication for intra-night variability with a doubling time of 36± min on the night of April 29, 2006, establishing once more rapid flux variability for this object. For all individual nights γ-ray spectra could be inferred, with power-law indices ranging from 1.66 to 2.47. We did not find statistically significant correlations between the spectral index and the flux state for individual nights. During the June 2006 campaign, a flux substantially lower than the one measured by the Whipple 10-m telescope four days later was found. Using a log-parabolic power law fit we deduced for some data sets the location of the spectral peak in the very-high energy regime. Our results confirm the indications of rising peak energy with increasing flux, as expected in leptonic acceleration models.

On the multiwavelength spectrum of the microquasar 1E1740.7-2942

The microquasar 1E 1740.7-2942 is a source located in the direction of the Galactic Center. It has been detected at X-rays, soft gamma-rays, and in the radio band, showing an extended radio component in the form of a double-sided jet. Although no optical counterpart has been found so far for 1E 1740.7-2942, its X-ray activity strongly points to a galactic nature. Aims.We aim to improve our understanding of the hard X-ray and gamma-ray production in the system, exploring whether the jet can emit significantly at high energies under the light of the present knowledge. Methods.We have modeled the source emission, from radio to gamma-rays, with a cold-matter dominated jet model. INTEGRAL data combined with radio and RXTE data, as well as EGRET and HESS upper-limits, are used to compare the computed and the observed spectra. Results.From our modeling, we find out that jet emission cannot explain the high fluxes observed at hard X-rays without violating at the same time the constraints from the radio data, favoring the corona origin of the hard X-rays. Also, 1E 1740.7-2942 might be detected by GLAST or AGILE at GeV energies, and by HESS and HESS-II beyond 100 GeV, with the spectral shape likely affected by photon-photon absorption in the disk and corona photon fields.

Discovery of a High-Energy Gamma-Ray-Emitting Persistent Microquasar

Microquasars are stellar x-ray binaries that behave as a scaled down version of extragalactic quasars. The star LS 5039 is a new microquasar system with apparent persistent ejection of relativistic plasma at a 3 kiloparsec distance from the sun. It may also be associated with a gamma-ray source discovered by the Energetic Gamma Ray Experiment Telescope (EGRET) on board the COMPTON-Gamma Ray Observatory satellite. Before the discovery of LS 5039, merely a handful of microquasars had been identified in the Galaxy, and none of them was detected in high-energy gamma-rays.

Studying the non-thermal lobes of IRAS 16547-4247 through a multi-wavelength approach

In recent years, massive protostars have turned out to be a possible population of high-energy emitters. Among the best candidates is IRAS 16547-4247, a protostar that presents a powerful outflow with clear signatures of interaction with its environment. This source has been revealed to be a potential high-energy source because it displays non-thermal radio emission of synchrotron origin, which is evidence of relativistic particles. To improve our understanding of IRAS 16547-4247 as a high-energy source, we analyzed XMM-Newton archival data and found that IRAS 16547-4247 is a hard X-ray source. We discuss these results in the context of a refined one-zone model and previous radio observations. From our study we find that it may be difficult to explain the X-ray emission as non-thermal radiation coming from the interaction region, but it might be produced by thermal Bremsstrahlung (plus photo-electric absorption) by a fast shock at the jet end. In the high-energy range, the source might be detectable by the present generation of Cherenkov telescopes, and may eventually be detected by Fermi in the GeV range.

Deep GMRT radio observations and a multi-wavelength study of the region around HESS J1858+020

Context. There are a number of very high energy sources in the Galaxy that remain unidentified. Multi-wavelength and variability studies, and catalogue searches, are powerful tools to identify the physical counterpart, given the uncertainty in the source location and extension. Aims. This work carries out a thorough multi-wavelength study of the unidentified, very high energy source HESS J1858+020 and its environs. Methods. We have performed Giant Metrewave Radio Telescope observations at 610 MHz and 1.4 GHz to obtain a deep, low-frequency radio image of the region surrounding HESS J1858+020. We analysed archival radio, infrared, and X-ray data as well. This observational information, combined with molecular data, catalogue sources, and a nearby Fermi gamma-ray detection of unidentified origin, are combined to explore possible counterparts to the very high energy source. Results. We provide with a deep radio image of a supernova remnant that might be related to the GeV and TeV emission in the region. We confirm the presence of an H ii region next to the supernova remnant and coincident with molecular emission. A potential region of star formation is also identified. We identify several radio and X-ray sources in the surroundings. Some of these sources are known planetary nebulae, whereas others may be non-thermal extended emitters and embedded young stellar objects. Three old, background Galactic pulsars also neighbour HESS J1858+020 along the line of sight. Conclusions. The region surrounding HESS J1858+020 is rich in molecular structures and non-thermal objects that may potentially be linked to this unidentified very high energy source. In particular, a supernova remnant interacting with nearby molecular clouds may be a good candidate, but a star forming region, or a non-thermal radio source of yet unclear nature, may also be behind the gamma-ray source. The neighbouring pulsars, despite being old and distant, cannot be discarded as candidates. Further observational studies are needed, however, to narrow the search for a counterpart to the HESS source.

Gamma-ray emission from massive young stellar objects

Context.Massive stars form in dense and massive molecular cores. The exact formation mechanism is unclear, but it is possible that some massive stars are formed by processes similar to those that produce the low-mass stars, with accretion/ejection phenomena occurring at some point of the evolution of the protostar. This picture seems to be supported by the detection of a collimated stellar wind emanating from the massive protostar IRAS 16547-4247. A triple radio source is associated with the protostar: a compact core and two radio lobes. The emission of the southern lobe is clearly non-thermal. Such emission is interpreted as synchrotron radiation produced by relativistic electrons locally accelerated at the termination point of a thermal jet. Since the ambient medium is determined by the properties of the molecular cloud in which the whole system is embedded, we can expect high densities of particles and infrared photons. Because of the confirmed presence of relativistic electrons, inverse Compton and relativistic Bremsstrahlung interactions are unavoidable. Aims.We aim to make quantitative predictions of the spectral energy distribution of the non-thermal spots generated by massive young stellar objects, with emphasis on the particular case of IRAS 16547-4247. Methods.We study the high-energy emission generated by the relativistic electrons which produce the non-thermal radio source in IRAS 16547-4247. We also study the result of proton acceleration at the terminal shock of the thermal jet and make estimates of the secondary gamma rays and electron-positron pairs produced by pion decay. Results.We present spectral energy distributions for the southern lobe of IRAS 16547-4247, for a variety of conditions. We show that high-energy emission might be detectable from this object in the gamma-ray domain. The source may also be detectable in X-rays through long exposures with current X-ray instruments. Conclusions.Gamma-ray telescopes such as GLAST, and even ground-based Cherenkov arrays of new generation can be used to study non-thermal processes occurring during the formation of massive stars.

A microquasar model applied to unidentified gamma-ray sources

Among unidentified gamma-ray sources in the galactic plane, there are some that present significant variability and have been proposed to be high-mass microquasars. To deepen the study of the possible association between variable low galactic latitude gamma-ray sources and microquasars, we have applied a leptonic jet model based on the microquasar scenario that reproduces the gamma-ray spectrum of three unidentified gamma-ray sources, 3EG J1735-1500, 3EG J1828+0142 and GRO J1411-64, and is consistent with the observational constraints at lower energies. We conclude that if these sources were generated by microquasars, the particle acceleration processes could not be as efficient as in other objects of this type that present harder gamma-ray spectra. Moreover, the dominant mechanism of high-energy emission should be synchrotron self-Compton (SSC) scattering, and the radio jets may only be observed at low frequencies. For each particular case, further predictions of jet physical conditions and variability generation mechanisms have been made in the context of the model. Although there might be other candidates able to explain the emission coming from these sources, microquasars cannot be excluded as counterparts. Observations performed by the next generation of gamma-ray instruments, like GLAST, are required to test the proposed model.

Optical spectroscopy of microquasar candidates at low Galactic latitudes

We report optical spectroscopic observations of a sample of 6 low-galactic latitude microquasar candidates selected by cross-identification of X-ray and radio point source catalogs for |b|<5 degrees. Two objects resulted to be of clear extragalactic origin, as an obvious cosmologic redshift has been measured from their emission lines. For the rest, none exhibits a clear stellar-like spectrum as would be expected for genuine Galactic microquasars. Their featureless spectra are consistent with being extragalactic in origin although two of them could be also highly reddened stars. The apparent non-confirmation of our candidates suggests that the population of persistent microquasar systems in the Galaxy is more rare than previously believed. If none of them is galactic, the upper limit to the space density of new Cygnus X-3-like microquasars within 15 kpc would be 1.1\times10^{-12} per cubic pc. A similar upper limit for new LS 5039-like systems within 4 kpc is estimated to be 5.6\times10^{-11} per cubic pc.

LS 5039: A runaway microquasar ejected from the galactic plane

We have compiled optical and radio astrometric data of the microquasar LS 5039 and derived its proper motion. This, together with the distance and radial velocity of the system, allows us to state that this source is escaping from its own regional standard of rest, with a total systemic velocity of about 150 km/s and a component perpendicular to the galactic plane larger than 100 km/s. This is probably the result of an acceleration obtained during the supernova event that created the compact object in this binary system. We have computed the trajectory of LS 5039 in the past, and searched for OB associations and supernova remnants in its path. In particular, we have studied the possible association between LS 5039 and the supernova remnant G016.8-01.1, which, despite our efforts, remains dubious. We have also discovered and studied an HI cavity in the ISM, which could have been created by the stellar wind of LS 5039 or by the progenitor of the compact object in the system. Finally, in the symmetric supernova explosion scenario, we estimate that at least 17 solar masses were lost in order to produce the high eccentricity observed. Such a mass loss could also explain the observed runaway velocity of the microquasar.

On the Hall effect in polycrystalline semiconductors

Some problems involved in the interpretation of Hall‐effect measurements in polycrystalline semiconductors have not been resolved, especially when the contribution of the boundaries is appreciable. Using the Herring theory of transport properties in inhomogeneous semiconductors, we present an alternative interpretation to that previously proposed. This model permits the calculation of the Hall coefficient under general conditions.

La Cova des Pas de Ferreries: notícia de la seva troballa

Durant la primavera del 2005, tres espeleòlegs es varen endinsar al barranc de Trebalúger, a prop de Ferreries, al sud-est de l"illa de Menorca. El seu objectiu era el barranc; l"havien vist feia unes quantes setmanes i no podien deixar passar aquell forat, de difícil accés. No sabien que estaven a punt de fer una de les troballes més extraordinàries de la prehistòria menorquina. Varen assegurar les cordes al cim de la paret i, tot fent un ràpel de trenta-cinc metres, accediren a un petit forat, veí de la cova a la qual volien arribar. Des d"allà varen haver de reptar, penjats de l"espadat, per una mena de graó estret o postada, un pas obligat per arribar-hi, que acabaria donant nom a la petita cova. Quan varen accedir al graó d"entrada ja havien decidit que allò seria la cova des Pas.

Els prats de l'alianÇa Xerobromion als Pirineus Catalans

En este trabajo se intenta dar una visión sintética de las comunidades de la alianza Xerobromion conocidas hasta el momento de los Pirineos catalanes. Se distinguen en dicho territorio nueve asociaciones distintas, cinco de ellas ya descritas con anterioridad (Koelerio-Avenuletum mirandanae, Achilleo-Dichanthietum ischaemi,. Teucrio (pyrenaici )-Brometum, Lino (viscosi)-Brometum, Koelerio-Globularietum punctatae) y las cuatro restantes propuestas como nuevas (Cleistogeno-Dichanthietum ischaemi , Teucrio (montani )-Avenuletum mirandanae, Adonido-Brometum e Irido (germanici)-Brometum). De todas ellas, y más especialmente de estas últimas, se hacen comentarios relativos a su estructura, composición florística, ecología y distribución. Además de las tablas de inventarios correspondientes a cada una de las nuevas asociaciones, se ha elaborado una tabla sintética que agrupa el total de las comunidades consideradas.

Valoración experiencial del aprendizaje tras formación virtual.

[eng] An observable study on the behaviour in the laboratory of Pharmaceutical Technology II (pharmaceutical pilot plant), with two groups of students of 3rd course (proactive aptitude and valuation of the"knowledge to do acquired") is carried out. The variable between groups is that one has realised a training (by means of self-study of an interactive application multimedia, especially designed), without tutorship on behalf the teacher in front of the other group that carried out the same training with the same material but with the guide of the teacher in the computer lab. On the one hand it is valued if there is some effect differentiator between both types of training, by means of the accounting of the correct results obtained in a previous test to the entrance in the pilot plant and by another one the valuation that the professors made responsible for the groups of practices in situ. The results demonstrate the previous hypothesis that there must not be significant differences between the groups, beyond the inherent ones to personality of the students itself (interest and personal implication by the subject). On the other hand the test for the observation in the laboratory did not facilitate the distinction of objective differences. [spa] Se lleva a cabo un estudio observacional sobre el comportamiento de los estudiantes (aptitud pro-activa y valoración del “saber hacer adquirido”) en el laboratorio de Tecnología Farmacéutica II (planta piloto farmacéutica) de dos grupos de estudiantes de 3er curso. La variable entre los dos grupos es que uno ha realizado una formación no presencial (mediante el autoestudio de una aplicación interactiva multimedia, especialmente diseñada), sin tutoría por parte del profesor, frente al otro grupo que llevó a cabo la misma formación con el mismo material pero con la guía del profesor en el aula de informática. Por una parte se valora si hay algún efecto diferenciador entre ambos tipos de formación, mediante la contabilización de los resultados correctos obtenidos en un test previo a la entrada en la planta piloto y por otro la valoración que hicieron los profesores responsables de los grupos de prácticas in situ. Los resultados demuestran la hipótesis previa de que no debían existir diferencias significativas entre los grupos, más allá de las inherentes a la propia personalidad de los estudiantes (interés e implicación personal por el tema). Por otra parte el test para la observación en el laboratorio no facilitó la distinción de diferencias objetivas.