Galician women translators in the 20th century: rewriting the history of translation from a gender and national approach

This article is the English version of “Traductoras gallegas del siglo XX: Reescribiendo la historia de la traducción desde el género y la nación” by Olga Castro. It was not published on the print version of MonTI for reasons of space. The online version of MonTI does not suffer from these limitations, and this is our way of promoting plurilingualism.

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.

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.