bluuebunny/crossref_metadata_2025_split huggingface dataset:
PROBLEMI E SCELTE NELLA COMPARAZIONE. INTRODUZIONE
Authors: Morlino Leonardo 
Published: May 2019

IntroduzionePrimo esempio: negli ultimi quindici anni la democrazia sembra essersi affermata in diverse aree del mondo, dal Sud Europa all'America Latina, all'Est Europa; ma quali democrazie si sono realmente affermate e come spiegare complessivamente questo fenomeno?Secondo esempio: durante il 1989 e gran parte dell'anno successivo vi sono state le trasformazioni dei regimi non democratici in Europa Orientale; quali profondi cambiamenti politici vi sono effettivamente stati in quei paesi, oltretutto a un ritmo così rapido?Terzo esempio: in Italia, durante gli ultimi quaranta anni il partito comunista è stato piò forte di quello socialista; come spiegarlo?Quarto esempio: di fronte ai problemi di rappresentatività e democrazia che l'Italia ha, molti politici e intellettuali propongono certe riforme istituzionali; ma quali riforme sono le piò adatte rispetto a determinati obiettivi, quali accrescere la responsabilità dei governanti e la capacità di punizione dei governati oppure raggiungere maggiore efficacia decisionale o ancora riuscire ad innescare l'alternanza al governo tra partiti o coalizioni partitiche?
COMPARAZIONE E WELFARE STATE: UN CASO DI SUCCESSO?
Authors: Ferrera Maurizio 
Published: May 2019

IntroduzioneRiguardando l'abbondante letteratura dell'ultimo trentennio in tema di welfare state, non si può fare a meno di riconoscere che questo settore d'indagine ha dato luogo ad un progresso conoscitivo davvero notevole, soprattutto per quanto riguarda la sequenza causale che ha originato le politiche sociali verso la fine del secolo scorso e ne ha successivamente promosso una continua e sostenuta espansione. Per avere una conferma immediata di tale progresso è sufficiente un rapido confronto fra lo «stato dell'arte» all'inizio degli anni ‘60 e la situazione attuale. Trent'anni or sono, la stessa etichetta di «welfare state» era fresca di conio nel linguaggio politico, mentre in quello accademico era impiegata dai soli studiosi anglosassoni in riferimento pressoché esclusivo all'esperienza britannica. Pochi gli studi di vasto respiro e tutti di taglio storico, mentre l'incipiente ricerca sociologica era soprattutto assorbita dall'indagine micro-applicativa. Anche se già ben cospicua in tutti i paesi sviluppati, la «cosa» welfare state restava praticamente sconosciuta al di fuori della cerchia ristretta dellaLondon Schoole di pochi altri istituti universitari.
IL PARLAMENTO IN ITALIA. VECCHIE E NUOVE IPOTESI DI RICERCA
Authors: Morisi Massimo 
Published: May 2019

IntroduzioneIl parlamento è tra le istituzioni più studiate, anche in Italia, tuttavia, la ricerca empirica sul suofunzionamentoall'interno del sistema politico, pare languire da anni. Riempiremmo pagine se dovessimo elencare la miriade di lavori di «riflessione» sull'azione dellegislativo, sulle sue modalità e sui suoi stessi significati sistemici, nel breve come nel medio e lungo termine. Altre pagine ci vorrebbero per dar conto delle molteplici esperienze di ricerca empirica, maturate in un denso e continuo confronto fra ipotesi metodologiche diverse, mono e interdisciplinari, sia in concorrenza che in collaborazione tra diritto costituzionale, storia parlamentare, scienza politica, sociologia politica. E agli studi sulla collocazione e sul ruolo delle assemblee parlamentari all'interno del sistema politico, si potrebbero aggiungere i diversi filoni di ricerca sulla classe politica e sulla rappresentanza.
LA DIFESA EUROPEA: PROBLEMI E PROSPETTIVE
Authors: Gori Umberto 
Published: May 2019

IntroduzioneDopo oltre un quarantennio di «politica dello struzzo», o — al massimo — di tentativi falliti, gli Stati dell'Europa occidentale cominciano dolorosamente a rendersi conto che non è più possibile continuare a rimuovere dall'agenda delle priorità il problema della sicurezza e della difesa.
L'ISTITUZIONALIZZAZIONE DEL GOVERNO
Authors: Calise Mauro 
Published: May 2019

IntroduzioneIl concetto di istituzionalizzazione continua ad avere un'accoglienza difficile negli studi politologici. Da Bentley a Easton, la scienza politica si è sviluppata contrapponendo la politica come processo alla politica come stato, e non v'è dubbio che le istituzioni rafforzino il versante strutturale di questa dicotomia. Parlare di istituzioni in scienza politica pone l'accento sul fatto che i comportamenti tendono a cristallizzarsi, le azioni si oggettivizzano. Fino a risollevare il vecchio dubbio che le istituzioni obbediscano a una propria logica autonoma, tant'è che gli analisti delle politiche pubbliche sono tornati a chiedersi «perché la forma dovrebbe seguire la funzione». In America, si è cominciato a parlare di «new institutionalism» per richiamare l'attenzione sulla perdurante importanza dei fattori organizzativi nella vita politica. In contrasto con gli assunti behavioristi, «la maggior parte degli attori principali nei moderni sistemi economici e politici sono organizzazioni formali, e le istituzioni della legge e della burocrazia occupano un ruolo dominante nella vita contemporanea». Il tentativo di Huntington, alla fine degli anni sessanta, di fondare sul concetto di istituzionalizzazione una teoria empirica dello sviluppo politico sembra dunque approdato alla riscoperta delle istituzioni come gabbia del mutamento.
LE TRASFORMAZIONI NELLA LEADERSHIP DEL PSI: LA DIREZIONE E I SUOI MEMBRI (1976-1984)
Authors: Massari Oreste 
Published: May 2019

IntroduzioneL'oggetto della presente ricerca è l'analisi del ruolo della Direzione e dei caratteri socio-politici dei suoi membri nell'arco di tempo che ha visto l'emergere, il rafforzamento e l'indubbio primato della leadership di Craxi prima all'interno del Partito Socialista Italiano (dal 1976) e, poi, all'interno del sistema politico nazionale come Presidente del Consiglio di un governo di coalizione (1983-1987).
IL REFERENDUM SULLA RESPONSABILITÀ CIVILE DEI MAGISTRATI
Authors: Cartocci Roberto 
Published: May 2019

IntroduzioneL'8 novembre 1987, per la quinta volta dal 1974, gli elettori italiani sono stati chiamati alle urne per decidere sull'abrogazione di cinque disposizioni di legge, tre relative alla costruzione delle centrali elettronucleari, una riguardante la commissione parlamentare inquirente, l'ultima sulla disciplina della responsabilità civile dei magistrati. Contrariamente ai referendum sul divorzio e sull'aborto o a quello sulla scala mobile, si trattava di temi di natura tecnica e istituzionale di grande complessità, tali da rendere incerte anche le conseguenze del successo delle tesi abrogazioniste. Gli schieramenti dei partiti che si sono pronunciati in favore dell'una o dell'altra alternativa sono risultati poi estremamente aggrovigliati: sui quesiti attinenti l'energia nucleare i liberali si sono schierati contro lo smantellamento delle centrali mentre erano stati tra i promotori del referendum sulla responsabilità civile dei magistrati. Su quest'ultimo le uniche forze a schierarsi per il «no» sono state il Pri e Dp, solitamente su posizioni antitetiche. Infatti sul nucleare si sono trovati su sponde opposte.
X-Ray Emission from Stellar Flares: Exosat Results
Authors: Pallavicini R. , Tagliaferri G. 
Published: May 2019

AbstractWe present an overview of recent observations of stellar X-ray flares obtained with the EXOSAT Observatory. We discuss a few examples of flares from M dwarf flare stars, from RS CVn and Algol-type binaries, from single late-type stars (including a G0 dwarf and an A-type visual binary), and from pre-main-sequence objects. We also draw some general conclusions from the pieliminary analysis of the EXOSAT data sample.
A correlation between Balmer and soft X-ray emission from stellar and solar flares
Authors: Butler C.J. , Rodono M. , Foing B.H. 
Published: May 2019

SummarySimultaneous optical spectroscopy and X-ray monitoring of stellar and solar flares shows that a well-defined linear correlation exists between the integrated Hγ and soft X-ray flux that extends over four orders of magnitude. The existence of this relationship implies a direct proportionality between the emission from the cooler and denser regions (T ≈ 104K) responsible for Balmer lines and the emission from the hot plasma (T ≈ 107K) responsible for soft X-rays. The consequences are considered for (a) several models which have been proposed for solar flares, and (b) the suggestion that the Balmer emission results from irradiation by soft X-rays.
Optical Chromospheric Spectral Lines in K and M Dwarf Stars
Authors: Robinson R.D. , Cram L.E. 
Published: May 2019

AbstractObservations are reported of the Ca II resonance lines and II α in dK and dM stars, made with high S/N ratio and high spectral resolution. Ca II emission is found in all stars observed, and those having weak Ca II exhibit marked Hα absorption. It is found that the strengths of the two kinds of chromospheric, lines are not tightly correlated, an effect which can be shown to be independent of the effective temperature of the stars. The result implies that a one-parameter description (e.g. heating rate) of the chromospheres is not viable. While lateral inhomogeneities are likely to be an important second parameter, we also suggest that the Hα line may be formed in a region considerable higher that in which the Ca II lines are formed.
High Time Resolution Photometry of Red Dwarf Flare Stars I. A Search For Fine Structures on the Optical Light Curves of Flares
Authors: Beskin G.M. , Mitronova S.N. , Neizvestnyj S.I. , Plakhotnichenko V.L. , Pustil'nik L.A. , Shvartsman V.F. , Gershberg R.E. 
Published: May 2019

AbstractA detailed analysis of 73 flares on UV Cet type stars observed at the 6 m telescope of the Special Astrophysical Observatory with 3x10–7 s time resolution shows no fine structures on flare light curves with time scales from 10–6 to 10–1 s.
High Time Resolution Photometry of Red Dwarf Flare Stars II. The Shortest Flare Rise Time
Authors: Beskin G.M. , Plakhotnichenko V.L. , Pustil'nik L.A. , Shvartsman V.F. , Gershberg R.E. 
Published: May 2019

AbstractWe have studied the initial phases of 65 optical flares on UV Cet type stars with a time resolution of 3x10–7 s. Ninety per cent of these flares have rapid brightenings shorter than 10 s and several are shorter than 1 s. We detected on UV Cet the shortest flare observed to date with a total duration of 1.7 s and a rise time of 0.3 s. The shortest flare rise times on the observed stars fit the predictions of the gas-dynamic flare model by Katsova et al. (1981) and Katsova and Livshits 1986).
General Properties of Ultraviolet Flares in RS CVn Systems
Authors: Neff J. E. , Brown A. , Linsky J. L. 
Published: May 2019

AbstractApproximately 10 very bright flares in RS CVn systems have been observed with the IUE. In several cases, high-resolution spectra of the Mg II k line profiles were obtained before, during, and after the flare. Such data permit us to measure the position and size of the flaring region, the amount of line broadening, and any systematic flow velocity. In two cases, several spectra were obtained during the flare decay, permitting us to study the change in these quantities during the flare decay.
The Sun as a Flare Star: X-Ray Spatial and Plasma Properties Derived from a Solar Eclipse Observed by Goes
Authors: P. L. Bornmann  
Published: May 2019

AbstractThe size, location, and flux of four solar soft X-ray sources, including a flare, were derived from the disk-integrating GOES X-Ray Sensors during a solar eclipse. The fluxes were used to derive the temperatures and emission measures of these sources. If an incorrect amount of flux is attributed to the flare source, then the evolution of these derived plasma properties seems unphysical.
Plasma Parameters and Structures of the X4 Flare of 19 May 1984 as Observed by SMM-XRP
Authors: Schmelz J.T. , Saba J.L.R. , Strong K.T. 
Published: May 2019

AbstractThe eruption of a large flare on the east limb of the Sun was observed by the X-Ray Polychromator (XRP) on board the Solar Maximum Mission (SMM) on 19 May 1984. The XRP Flat Crystal Spectrometer (FCS) made polychromatic soft X-ray images during the preflare, flare and postflare phases. The XRP Bent Crystal Spectrometer (BCS) provided information on the temperature and dynamics of the hot (Te > 8 x 106K) coronal plasma from spectra integrated spatially over the whole region.
Solar Neutron Observations During the Coming Solar Maximum: A Plan on the Japan-China Collaborative Project
Authors: Sakurai Kunitomo 
Published: May 2019

AbstractNeutrons are sometimes released from solar flares accompanied by generation of high energy protons and other nuclei and some of them occasionally reach the earth before they decay radioactively. Together with the satellite observations on gamma ray and neutron emissions associated with such flares, the ground-based observations of these neutrons give us a clue to understand the possible nuclear interactions of those protons and nuclei with gases ambient in the solar atmosphere. A review is given on the Japan-China collaborative program on the ground-based observations of these neutrons for the coming solar maximum, though there still remain obstacles to be resolved.
Model of Slowly Evolving Flare
Authors: Chiuderi Drago F. , Landini M. , Monsignori Fossi B.C. 
Published: May 2019

AbstractA gradual rise and fall flare, with a duration of about one hour was observed on June 10, 1980 in the radio (Toyokawa and VLA), optical (Bing Bear) and XUV (SMM satellite) ranges of wavelengths. The flare developed as a large loop connecting two regions of opposite polarity in a pre-exisisting active region. A model of the differential emission measure of the loop observed at three different stage of the flare is deduced from the analysis of the XUV images in C IV (1549 A), O VIII (18.97 A), Ne IX (13.45 A), Mg XI (9.17 A) and Si XIII (6.65 A) emission lines. The differential emission measure as a function of temperature is controlled by the conductive flux via the temperature gradient; the evaluation of the divergence of the conductive flux is used in the energy balance to have information on the power deposition function.
September 7 1973 Two-Ribbon Flare
Authors: Doyle J.G. , Widing K.G. 
Published: May 2019

AbstractThe flare images show a compact, nearly cylindrical arcade centered along the filament channel and composed of 4 prominent loops. The loop systems of Fe XII (Te = 1.7 106K) and Fe XIV (Te = 2.3 106K) are smaller than, and lie nested within, the arcades of Fe XVI (Te = 3 106K) and Ca XVII (Te = 5 106K). The loop arcades at different temperatures, as well as different loops within a given arcade, show different expansion rates. These vary from 6 – 8 km s–1 for Fe XIV shortly after flare maximum to 0.5 – 1 km s–1 late in the decay phase. For hotter ions, such as Ca XVII, the velocities are approximately constant at 2 – 3 km s–1 daring the whole of the observations.
Chromospheric Downflows as a Diagnostic of Solar Flare Heating
Authors: Zarro Dominic M. , Canfield Richard C. 
Published: May 2019

AbstractUsing coordinated X-ray and Hα observations of five solar flares, we investigate the dynamics of chromospheric condensations formed during chromospheric evaporation. We show that the peak downflow velocity of condensations predicted by simple hydrodynamic compression of the chromosphere is in good agreement with empirical downflow velocities implied by impulsive phase Hα redwing Doppler shifts. This agreement indicates that the Hα wing redshift provides a useful diagnostic of the pressure excess in the evaporating region and, hence, the energy flux driving chromospheric evaporation.
Heat Flux in a Non-Maxwellian Solar Coronal Plasma
Authors: Ljepojevic N.N. , MacNeice P. 
Published: May 2019

AbstractWe determine the electron distribution function within a hot coronal loop using a hybrid numerical scheme which couples the Spitzer-Härm method at low velocities with the solution to the high velocity form of the Landau-Fokker-Planck equation. From this we calculate the heat flux throughout the loop and compare it with the classical fourier law of Spitzer and Härm(1953).
Particle Acceleration and Plasma Heating at Collisionless Shocks in Solar Flares
Authors: Cargill Peter J. , Vlahos Loukas 
Published: May 2019

AbstractRecent observations suggest that the energy release in solar flares may occur in many small bursts. If these bursts give rise to plasma heating, a large number of collisionless shocks will be generated. These shocks can individually heat plasma and accelerate particles, but the interaction of particles with many shocks as well, as of shocks with each other can give rise to further heating and acceleration.
Linear and non linear study of a possible mechanism for the generation of stellar radio bursts: The Synchrotron Maser Instability
Authors: Louarn P. , Le Queau D. , Roux A. 
Published: May 2019

AbstractThe emission mechanism studied here, the synchrotron maser instability is based on a gyroresonance of highly energetic electrons. Compared to the cyclotron maser, this mechanism has the great advantage to be a direct amplification process even if the ratio ωp/ωc is not very small; a situation relevant to stellar flares.The high efficiency of the process can be confirm by the non linear study of its saturation.
Propagation and Absorption of Electron Cyclotron Maser Emission during Solar Flares
Authors: McKean M. E. , Winglee R. M. , Dulk G. A. 
Published: May 2019

AbstractThe propagation and absorption of the maser radiation emitted during solar flares are examined through linear theory and electromagnetic particle simulations. While linear theory predicts complete absorption of the maser radiation at the second harmonic layer (where the local cyclotron frequency is roughly one-half the frequency of the maser radiation), particle simulations indicate that some radiation escapes clue to reemission of absorbed energy by the ambient plasma. Strong perpendicular heating of the ambient electrons occurs as well.
Computer Simulation of a Solar Microwave Burst
Authors: Bruggmann G. , Schanda E. , Magun A. 
Published: May 2019

A simple impulsive event observed at microwave frequencies between 3.2 and 50 GHz is simulated with a homogeneous source model. Intensity and polarization of the 1984 April 26 event are shown in fig. 1a and 1b, respectively. The spectral maximum is close to the observing frequency of 11.8 GHz.The time profiles of the intensity I and the circular polarization ρc at this frequency as well as the spectrum at different characteristic phases (rise, maximum and decay) are calculated and compared with the observation in order to deduce parameters of the microwave source.
A New Explanation for Flares on dMe Stars
Authors: Simnett G.M. 
Published: May 2019

AbstractIt has been proposed that non-thermal ions dominate the energy transfer at the onset of solar flares. Here we examine this hypothesis in the context of flares on dMe stars. If the magnetic field in the stellar corona is significantly larger than that in the solar corona, and if strong fields in the photosphere, analagous to active regions, are absent, then a self-consistent explanation of stellar flares may be formulated.
Chromospheric NLTE-Radiative-Transfer Modeling of dMe Stars
Authors: P.M.Panagi  , Houdebine E. , Butler C.J. , Rodonò M. 
Published: May 2019

AbstractThe formation of the Lyman and Balmer lines of Hydrogen at densities typical in dMe stars is shown to be very dependent on the atomic model used viz. the number of levels and line transitions. The effect of increasing the number of levels and line transitions on the line fluxes and ionization fraction is also discussed.
Dislocations in Deformed Aluminum Alloy
Authors: Zhang Z. , Wang Y. 
Published: May 2019

AbstractA deformed aluminum-copper alloy was studied by X-ray diffraction. The 111 diffraction profile was found to consist of a main peak and a subpeak. They were separated by a numerical differential method combined with a non-linear least square profile fitting procedure. The subpeak could not be ascribed to the θ phase in the alloy since the intensity ratio of the subpeak to main peak is 20-30 times more than the volume ratio of the θ phase to die matrix. On the other hand, the Transmission Electron Microscope (TEM) micrographs showed clearly that there is a highly inhomogeneous dislocation distribution just like the cell structure in pure aluminum. The main X-ray peak was thus assumed to be due to diffraction from the cell interior while the subpeak is determined by the cell wall. After applying a series of standard data processing procedures based on Wilkens' theory and the Pearson VII-Voigt function, the dislocation densities in both the cell interior and wall were evaluated.
X-Ray Powder Diffraction Study of NBS Fly Ash Standard Reference Materials
Authors: McCarthy Gregory J. , Johansen Diane M. 
Published: May 2019

AbstractThe fly ash Standard Reference Materials (SRMs) issued by the U.S. National Bureau of Standards have been studied by X-ray powder diffraction (XRD). Based on observations of large diffuse scattering maxima in their X-ray diffractograms, it was evident that all of the ashes had a high glass content. SRM 1633a and 2689, derived from the combustion of bituminous coal, contained different amounts of quartz, mullite, hematite and ferrite spinel (magnetite). SRM 2891, derived from subbituminous coal had quite a different chemical composition and a more complex crystalline phase assemblage, that included these four phases plus anhydrite, tricalcium aluminate, lime, periclase and minor phases. SRM 2690, also derived from subbituminous coal, had only quartz, mullite and ferrite spinel as detectable phases in its diffractogram. Analytical CaO is an important factor in determining the phase assemblage; SRM 2691 had 25.8 wt%, SRM-2690 had 8.0%, and the ash derived from bituminous coals had only 1.6-3.0%. The changing composition of the glass phases in the SRMs is detected in a shift in the position and shape of the diffuse scattering maximum in the diffractograms. Use of an internal intensity standard permitted quantitative comparisons of the relative amounts of crystalline phases among the four fly ash SRMs.
Limiting Factors for Diffraction in the Gandolfi X-Ray Camera
Authors: Canfield Dennis V. , Sundeen Daniel A. 
Published: May 2019

AbstractA discrepancy was discovered between an experimental X-ray diffraction pattern of sodium acetate trihydrate collected with the Gandolfi camera and a calculated pattern based on a single crystal study of the same compound. The experimental d spacings matched those of the calculated pattern with the exception of the strongest reflection d = 3.002 Å (h k l = 40 − 2) which was missing in the experimental pattern. Another experimental Gandolfi pattern obtained from a powdered sample of sodium acetate trihydrate gave excellent agreement with the calculated d spacings and intensities.The results of our investigation into this discrepancy show that the angle θ, crystal alignment, camera diameter, and the crystal system can affect diffraction in the Gandolfi camera. It is shown that all reciprocal lattice points with θ angles less then 10.08° would diffract in the film plane of the 114.6 mm Gandolfi camera and points with θ angles less then 20.49° would diffract in the film plane for the 57.3 mm camera regardless of the crystal system or alignment. However, reciprocal lattice points aligned along the spindle axis of the 114.6 mm Gandolfi camera having reciprocal lattice points with Z ≥ 0.35 reciprocal lattice units (r.l.u.) and X and Y ≤ Z-0.35 r.l.u. will not diffract into the recording plane of the Gandolfi camera. The reciprocal lattice points aligned along the spindle axis of the 57.3 mm Gandolfi camera with Z ≥ 0.70 r.l.u. and X and Y ≤ Z-0.70 r.l.u. will not diffract into the recording plane of the camera.