On the nature of the galactic early-B hypergiants

Aims. Despite their importance to a number of astrophysical fields, the lifecycles of very massive stars are still poorly defined. In order to address this shortcoming, we present a detailed quantitative study of the physical properties of four early-B hypergiants (BHGs) of spectral type B1-4 Ia+; Cyg OB2 #12, ζ1 Sco, HD 190603 and BP Cru. These are combined with an analysis of their long-term spectroscopic and photometric behaviour in order to determine their evolutionary status. Methods. Quantitative analysis of UV–radio photometric and spectroscopic datasets was undertaken with a non-LTE model atmosphere code in order to derive physical parameters for comparison with apparently closely related objects, such as B supergiants (BSGs) and luminous blue variables (LBVs), and theoretical evolutionary predictions. Results. The long-term photospheric and spectroscopic datasets compiled for the early-B HGs revealed that they are remarkably stable over long periods ( ≥ 40 yrs), with the possible exception of ζ1 Sco prior to the 20th century; in contrast to the typical excursions that characterise LBVs. Quantitative analysis of ζ1 Sco, HD 190603 and BP Cru yielded physical properties intermediate between BSGs and LBVs; we therefore suggest that BHGs are the immediate descendants and progenitors (respectively) of such stars, for initial masses in the range ~30−60 M⊙. Comparison of the properties of ζ1 Sco with the stellar population of its host cluster/association NGC 6231/Sco OB1 provides further support for such an evolutionary scenario. In contrast, while the wind properties of Cyg OB2 #12 are consistent with this hypothesis, the combination of extreme luminosity and spectroscopic mass (~110 M⊙) and comparatively low temperature means it cannot be accommodated in such a scheme. Likewise, despite its co-location with several LBVs above the Humphreys-Davidson (HD) limit, the lack of long term variability and its unevolved chemistry apparently excludes such an identification. Since such massive stars are not expected to evolve to such cool temperatures, instead traversing an O4-6Ia → O4-6Ia+ → WN7-9ha pathway, the properties of Cyg OB2 #12 are therefore difficult to understand under current evolutionary paradigms. Finally, we note that as with AG Car in its cool phase, despite exceeding the HD limit, the properties of Cyg OB2 #12 imply that it lies below the Eddington limit – thus we conclude that the HD limit does not define a region of the HR diagram inherently inimical to the presence of massive stars.

Competències mediàtiques a l’IES Dr. Balmis d’Alacant

La introducció de les TIC en l’ensenyament (les TAC) planteja molts interrogants entre els membres de la comunitat educativa, especialment entre el professorat. L’atracció del mitjà per als aprenents, la manca de reflexió en l’ús, tant per part del professorat com de l’alumnat, la necessitat d’una formació específica, l’adequació de les infraestructures al concepte i a les possibilitats que ofereix el web 2.0 i la incorporació de les aplicacions TAC en les programacions d’aula són alguns aspectes que mereixen una atenció específica i una anàlisi detinguda. La base de gran part de les respostes rau en una planificació eficaç de la formació del professorat que satisfaça les expectatives de tothom. Els projectes de centre, la utilització de plataformes educatives com Moodle i l’autoformació són sendes que ens acosten envers les solucions. En aquest treball, hi centrem l’atenció en les valoracions, les pràctiques habituals, les actituds i els coneixements relacionats amb la competència mediàtica o digital del professorat de l’IES Dr. Balmis d’Alacant. Ens basem en una enquesta realitzada en línia que aplega aquests continguts en una combinació d’ítems de resposta tancada i d’altres de resposta oberta.

Radon measurements in the cave houses of Crevillente (Spain)

This paper focuses on the cave houses of Crevillente (Spain) as a traditional housing experience which takes advantage of local environmental conditions through simple architectural proposals, paying particular attention to the presence of radon gas inside these underground constructions. Our aim is twofold: first, to analyse the architectural conditions of the different excavated typologies found in the municipality and second, to relate them to the existing radon gas levels after checking internal concentration by means of E-PERM® long-term devices placed inside the cave houses in 2011. The measurements corresponding to the main typologies in normal use conditions show that the highest values are 881.9 Bq/m3 in the cave typology, 484.1 Bq/m3 in the cave + attached constructions typology and 373.4 Bq/m3 in the cave + house typology, with geometric mean values of 572.1, 114.0 and 75.5 Bq/m3, respectively. It can be inferred from these results that cave house levels sometimes exceed those included in the 90/143/Euratom European Commission Recommendation on the protection of the public against indoor exposure to radon. The reason why cave houses are more susceptible to radon accumulation in their spaces lies in their direct and permanent contact with the ground where they are located.

VdBH 222: a starburst cluster in the inner Milky Way

Context. It has been suggested that the compact open cluster VdBH 222 is a young massive distant object. Aims. We set out to characterise VdBH 222 using a comprehensive set of multi-wavelength observations. Methods. We obtained multi-band optical (UBVR) and near-infrared (JHKS) photometry of the cluster field, as well as multi-object and long-slit optical spectroscopy for a large sample of stars in the field. We applied classical photometric analysis, as well as more sophisticated methods using the CHORIZOS code, to determine the reddening to the cluster. We then plotted dereddened HR diagrams and determined cluster parameters via isochrone fitting. Results. We have identified a large population of luminous supergiants confirmed as cluster members via radial velocity measurements. We find nine red supergiants (plus one other candidate) and two yellow supergiants. We also identify a large population of OB stars. Ten of them are bright enough to be blue supergiants. The cluster lies behind ≈7.5 mag of extinction for the preferred value of RV = 2.9. Isochrone fitting allows for a narrow range of ages between 12 and 16 Ma. The cluster radial velocity is compatible with distances of ~6 and ~10 kpc. The shorter distance is inconsistent with the age range and Galactic structure. The longer distance implies an age ≈ 12 Ma and a location not far from the position where some Galactic models place the far end of the Galactic bar. Conclusions. VdBH 222 is a young massive cluster with a likely mass >20 000 M⊙. Its population of massive evolved stars is comparable to that of large associations, such as Per OB1. Its location in the inner Galaxy, presumably close to the end of the Galactic bar, adds to the increasing evidence for vigorous star formation in the inner regions of the Milky Way.

Geodynamic events reconstructed in the Betic, Maghrebian, and Apennine chains (central-western Tethys)

A synthetic study has been made to identify main tectono-sedimentary and geodynamic events in central-western Tethys. For this, an interdisciplinary analysis has been performed on successions belonging to tectonic units derived from Betic-Maghrebian-southern Apennine “Flysch basin” domain. The stratigraphic records of the internal, external, and mixed successions deposited in lateral basins of different chains show very similar characters, especially regarding: (a) lithostratigraphy and ages; (b) kind and provenance of supplies (immature and supermature petrofacies from internal and external margins, respectively); (c) presence of “mixed successions” (composed of alternating internal and external petrofacies) attesting to clear palaeogeographic relationships between opposite depositional systems; and (d) timing of the deformation. In addition, specific lithofacies reveal correspondence with similar sedimentary events, such as: (1) very thick silicoclastic supply concentrated in restricted time ranges indicating the main deformational phases in the margin/basin systems; (2) levels rich in black-shales, glauconian, siliceous-producers, and volcaniclastic intercalations, widespread in the studied successions and linked to particular events at the Tethyan scale (anoxic periods, starvation-upwelling, acid-intermediate penecontemporaneous volcanic activity, respectively). Tectonic influence has also been recorded by means of unconformities and tectofacies (such as turbidites, slumps, or olisthostromes, etc.), being correlated with the main deformational phases. Similar stratigraphic and tectonic events have also been found in the Calvana unit of Val Marecchia nappe (Ligurides, northern Apennine). Correlations of stratigraphic and tectonic events support the proposal of an evolutionary geodynamic model involving the presence of a “Mesomediterranean microplate” in intermediate position during Africa-Europe convergence. The closure of central-western Tethys occasioned the Betic-Maghrebian-southern Apennine oceanic branch deformation and the birth of perimediterranean chains during middle-late Miocene.

On the forbidden gap of finite graphene nanoribbons

The electronic structure of isolated finite graphene nanoribbons is investigated by solving, at the Hartree-Fock (HF) level, the Pariser, Parr and Pople (PPP) many-body Hamiltonian. The study is mainly focused on 7-AGNR and 13-AGNR (Armchair Graphene Nano-Ribbons), whose electronic structures have been recently experimentally investigated. Only paramagnetic solutions are considered. The characteristics of the forbidden gap are studied as a function of the ribbon length. For a 7-AGNR, the gap monotonically decreases from a maximum value of ~6.5 eV for short nanoribbons to a very small value of ~0.12 eV for the longer calculated systems. Gap edges are defined by molecular orbitals that are spatially localized near the nanoribbon extremes, that is, near both zig-zag edges. On the other hand, two delocalized orbitals define a much larger gap of about 5 eV. Conductance measurements report a somewhat smaller gap of ~3 eV. The small real gap lies in the middle of the one given by extended states and has been observed by STM and reproduced by DFT calculations. On the other hand, the length dependence of the gap is not monotonous for a 13-AGNR. It decreases initially but sharply increases for lengths beyond 30 Å remaining almost constant thereafter at a value of ~2.1 eV. Two additional states localized at the nanoribbon extremes show up at energies 0.31 eV below the HOMO (Highest Occupied Molecular Orbital) and above the LUMO (Lowest Unoccupied Molecular Orbital). These numbers compare favorably with those recently obtained by means of STS for a 13-AGNR sustained by a gold surface, namely 1.4 eV for the energy gap and 0.4 eV for the position of localized band edges. We show that the important differences between 7- and 13-AGNR should be ascribed to the charge rearrangement near the zig-zag edges obtained in our calculations for ribbons longer than 30 Å, a feature that does not show up for a 7-AGNR no matter its length.

Summary of the evolution of the fortifications of Santa Barbara Castle in Alicante from its origins to the beginning of the eighteenth century

Since ancient times, Alicante has been considered a strategic location on the east coast of Spain. Situated close to the sea, it is protected to the southeast by the Cape of Huerta and to the southwest by the Cape of Santa Pola. The city lies at the foot of Mount Benacantil, a high outcrop which has been the site of defensive buildings since time immemorial due to its naturally strong position: it was undoubtedly one of the strongest natural sites in the Levant. Its summit, lying 160 metres above the sea, is topped by a series of fortified enclosures now known as Santa Barbara Castle. This paper briefly describes the alterations made to the castle fortifications from its origins through the Renaissance, including the Muslim and Christian periods until the late fifteenth century and subsequent alterations to adapt new bastioned fortification techniques, and depicts the status of the fortress in each period. This paper is the result of doctoral research carried out at different national and international archives and leading to a thesis presented in 2011.