3,930 research outputs found
Tutela dei minori e nuove transizioni familiari
No full textAbstract. The Author claims that the protection of minors in our contemporary society is primarily concerned with the changes in family transitions. As a matter of fact, family transitions loose the normative regulations they had in the past. The emergent effect is an overall increase in the risks and uncertainties that minors have to face. What does it happen when the relative stability of the transitional stages that families meet wither away? What are the consequences on children? What kind of interventions (social policies, personal social services, etc.) addressed to minors can be envisaged in a society which configures family transitions as an unbound morphogenesis of its relations? The social condition of minors becomes an unceasingly transition due to many factors, but basically because the societal morphogenesis makes the reflexive abilities of the families more and more problematic. The paper suggests that, in order to protect children, we have to go beyond the conditional and muddling through models of the past. We need to adopt a new model of analysis and intervention, called ODG-system, which is relational and reflexive. It consists in developing the relational reflexivity of the family as a social system able to cope with children’s needs
Pompeius, in artem Donati
No full textLindemann, F., ed. (1820), Pompeii Commentum Artis Donati. Eiusdem in librum Donati De barbarismis et metaplasmis Commentariolum. Accessit Ars grammatica Servii, Leipzig, xvi & 576 p. Zago, A., ed. (2017), Pompeii Commentum in Artis Donati partem tertiam. 1: introduzione, testo critico e traduzione, Hildesheim, cxlix & 130 p. Adams, J. N. (1991), "Some neglected evidence for latin 'habeo' with infinitive: the order of the constituents", Transactions of the Philological Society. Oxford , 89..
[Sergius] explanationes in artes Donati
No full textEichenfeld, J. von & S. Endlicher, eds. (1837) Analecta grammatica, maximam partem anecdota, Wien, xxvii & 571 p. Lindemann, F., ed. (1820), Pompeii Commentum Artis Donati. Eiusdem in librum Donati De barbarismis et metaplasmis Commentariolum. Accessit Ars grammatica Servii, Leipzig, xvi & 576 p. Bouterwerk, R. (1866), "Das erste Buch des Lucilius nebst zwei Fragmenten aus Sergius", Rheinisches Museum, 21, p. 339-361. Bücheler, F. (1866), "Clara obscura", Jahrbücher für klassische ..
Physics-based large-signal sensitivity analysis of microwave circuits using technological parametric sensitivity from multidimensional semiconductor device models
No full textThe authors present an efficient approach to evaluate the large-signal (LS) parametric sensitivity of active semiconductor devices under quasi-periodic operation through accurate, multidimensional physics-based models. The proposed technique exploits efficient intermediate mathematical models to perform the link between physics-based analysis and circuit-oriented simulations, and only requires the evaluation of dc and ac small-signal (dc charge) sensitivities under general quasi-static conditions. To illustrate the technique, the authors discuss examples of sensitivity evaluation, statistical analysis, and doping profile optimization of an implanted MESFET to minimize intermodulation which makes use of LS parametric sensitivities under two-tone excitatio
Modelling the hidden magnetic field of low-mass stars
No full textPL acknowledges support from a Science and Technology Facilities Council studentship. JM, AAV and RF acknowledge support from fellowships of the Alexander von Humboldt foundation, the Royal Astronomical Society and Science and Technology Facilities Council, respectively.Zeeman-Doppler imaging is a spectropolarimetric technique that is used to map the large-scale surface magnetic fields of stars. These maps in turn are used to study the structure of the stars' coronae and winds. This method, however, misses any small-scale magnetic flux whose polarization signatures cancel out. Measurements of Zeeman broadening show that a large percentage of the surface magnetic flux may be neglected in this way. In this paper we assess the impact of this 'missing flux' on the predicted coronal structure and the possible rates of spin-down due to the stellar wind. To do this we create a model for the small-scale field and add this to the Zeeman-Doppler maps of the magnetic fields of a sample of 12 M dwarfs. We extrapolate this combined field and determine the structure of a hydrostatic, isothermal corona. The addition of small-scale surface field produces a carpet of low-lying magnetic loops that covers most of the surface, including the stellar equivalent of solar 'coronal holes' where the large-scale field is opened up by the stellar wind and hence would be X-ray dark. We show that the trend of the X-ray emission measure with rotation rate (the so-called 'activity-rotation relation') is unaffected by the addition of small-scale field, when scaled with respect to the large-scale field of each star. The addition of small-scale field increases the surface flux; however, the large-scale open flux that governs the loss of mass and angular momentum in the wind remains unaffected. We conclude that spin-down times and mass-loss rates calculated from surface magnetograms are unlikely to be significantly influenced by the neglect of small-scale field.Peer reviewe
A perspective on surface-adsorbed single atom magnets as atomic-scale magnetic memory
No full text© 2021 Author(s).Downscaling single magnetic bits to the ultimate size of individual atoms would open the possibility to maximize the magnetic storage density on a solid surface. However, realizing stable magnets of the size of one atom remained an elusive challenge for more than a decade. Recent advances show that single lanthanide atoms on suitable surfaces can preserve their magnetization on a timescale of days at a temperature of 1 K or below. Such properties enable the use of these atoms as stable magnets for low temperature experiments, opening a platform for testing magnetic recording techniques at the atomic scale. In this article, we describe the single atom magnets that have been investigated and the methods employed to address their magnetic properties. We will discuss the limitations of the present systems and techniques and identify the challenges to close the gap toward potential future technological applications.11Nsciescopu
Magnetic activity and hot Jupiters of young Suns : the weak-line T Tauri stars V819 Tau and V830 Tau
No full textSGG acknowledges support from the Science & Technology Facilities Council (STFC) via an Ernest Rutherford Fellowship [ST/J003255/1]. SHPA acknowledges financial support from CNPq, CAPES and Fapemig. AAV acknowledges support from the Swiss National Science Foundation (SNSF) via the allocation of an Ambizione Followship. Date of Acceptance: 06/08/2015We report results of a spectropolarimetric and photometric monitoring of the weak-line T Tauri stars (wTTSs) V819 Tau and V830 Tau within the MaTYSSE (Magnetic Topologies of Young Stars and the Survival of close-ingiant Exoplanets) programme, involving the ESPaDOnS spectropolarimeter at the Canada-France-Hawaii Telescope. At ≃3 Myr, both stars dissipated their discs recently and are interesting objects for probing star and planet formation. Profile distortions and Zeeman signatures are detected in the unpolarized and circularly polarized lines, whose rotational modulation we modelled using tomographic imaging, yielding brightness and magnetic maps for both stars. We find that the large-scale magnetic fields of V819 Tau and V830 Tau are mostly poloidal and can be approximated at large radii by 350-400 G dipoles tilted at≃30° to the rotation axis. They are significantly weaker than the field of GQ Lup, an accreting classical T Tauri star (cTTS) with similar mass and age which can be used to compare the magnetic properties of wTTSs and cTTSs. The reconstructed brightness maps of both stars include cool spots and warm plages. Surface differential rotation is small, typically ≃4.4 times smaller than on the Sun, in agreement with previous results on wTTSs. Using our Doppler images to model the activity jitter and filter it out from the radial velocity(RV) curves, we obtain RV residuals with dispersions of 0.033 and 0.104km s-1 for V819 Tau and V830 Tau, respectively. RV residuals suggest that a hot Jupiter may be orbiting V830 Tau, though additional data are needed to confirm this preliminary result. We find no evidence for close-in giant planet around V819 Tau.Peer reviewe
Physics-based simulation techniques for small- and large-signal device noise analysis in RF applications
No full textPhysics-based SS and SSLS variability assessment of microwave devices through efficient sensitivity analysis
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