1,721,191 research outputs found
¿La teoría económica puede sobrevivir sin una relación con la historia?
Full text linkLa historia económica es una disciplina de frontera: sus herramientas de análisis se basan tanto en las ciencias históricas como en las económicas y, precisamente por ello, el hecho de que una parte importante de la historia económica contemporánea se limite únicamente a tomar como referencia las aportaciones de la economía y, en particular, del análisis económico más estrictamente cuantitativo constituye una grave limitación de su capacidad de interpretación. Por el contrario, parece imprescindible que la historia económica esté abierta a recibir todas las aportaciones metodológicas que puedan provenir de las ciencias históricas y, en general, de las ciencias sociales que se sirven también del análisis cualitativo de los fenómenos históricos
La Cassa di Risparmio della Provincia dell'Aquila 1859-2009: risparmio, ceti dirigenti, sviluppo economico
No full textClassi dirigenti, amministrazione pubblica e risparmio in un'economia regionale
Las fuerzas no profesionales en los reinos de Sicilia y de Nápoles en los siglos XVI-XVII: la “nuova milizia” y la “milizia del battaglione"
No full textFrontières externes, frontières internes. Implications politiques et sociales de l’institution des milices territoriales dans le royaumes de Naples et de Sicile, XVIe- XVIIe siècle
No full textL'articolo ha quale oggetto l'analisi della definizione delle frontiere in area mediterranea, con particolare riferimento ai regni di Napoli e Sicilia, e lo studio delle relative implicazioni sociali ed economiche nel corso del XVI secolo
First ALMA Maps of Cosmic-Ray Ionization Rate in High-mass Star-forming Regions
Full text linkLow-energy cosmic rays (<1 TeV) are a pivotal source of ionization of the interstellar medium, where they play a central role in determining the gas chemical composition and drastically influence the formation of stars and planets. Over the past few decades, H3 + absorption line observations in diffuse clouds have provided reliable estimates of the cosmic-ray ionization rate relative to H2 ( ζionH2
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). However, in denser clouds, where stars and planets form, this method is often inefficient due to the lack of H3 + rotational transitions. The ζionH2
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estimates are, therefore, still provisional in this context and represent one of the least understood components when it comes to defining general models of star and planet formation. In this Letter, we present the first high-resolution maps of the ζionH2
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in two high-mass clumps obtained with a new analytical approach recently proposed to estimate the ζionH2
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in the densest regions of molecular clouds. We obtain ⟨ζionH2⟩
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that span from 3 × 10-17 to 10-16 s-1, depending on the different distribution of the main ion carriers, in excellent agreement with the most recent cosmic-ray propagation models. The cores belonging to the same parental clump show comparable ζionH2
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, suggesting that the ionization properties of prestellar regions are determined by global rather than local effects. These results provide important information for the chemical and physical modeling of star-forming regions
Hydrothermal alteration and fluid evolution in the Mo-Deposit of Perda Lada (SW Sardinia, Italy)
No full textSkarn formation and alteration-mineralization phenomena at Funtana Raminosa (Central Sardinia, Italy). Reconstruction of the thermal history from fluid inclusions
No full textThe study of fluid inclusions trapped in minerals of the Funtana Raminosa ore district permit reconstruction of the quite complex history of thermal metamorphic and hydrothermal events that preceded and accompanied ore deposition. On this basis, we have recognized a first thermal metamorphic, isochemical event, which produced garnet-pyroxene skarns in the Silurian rocks, followed by a long-lasting hydrothermal circulation. The latter caused the retrocession of anhydrous skarn parageneses, the ore deposition and the intricate relationships existing among the different alteration assemblages that affected magmatites and surrounding rocks in the area
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