La governance degli enti locali sulle aziende di gestione dei servizi pubblici. Strumenti di programmazione e controllo in ottica di gruppo

Lo scopo del presente lavoro è delineare un nuovo modello inerente l'organizzazione, i processi e gli strumenti di programmazione e controllo a supporto della governance degli enti locali sulle loro aziende di gestione dei servizi pubblici, con particolare attenzione per la variabile strumentale. E' stata adottata una metodologia mista, deduttivo-induttiva. Nella fase deduttiva è stata analizzata la normativa italiana nonché la dottrina economico aziendale nazionale ed internazionale in tema di gestione dei servizi pubblici locali: in tal modo è stato estrapolato un modello normativo-dottrinale inerente l'organizzazione, i processi e gli strumenti di programmazione e controllo a supporto della governance degli enti locali sulle loro aziende di gestione dei servizi pubblici. Nella fase induttiva è stata realizzata un'indagine empirica che ha coinvolto i comuni capoluogo di Emilia-Romagna e Toscana, in modo tale da testare il livello di utilizzo del modello normativo-dottrinale precedentemente estrapolato Nella fase di feedback sono stati delineati i punti di forza e di debolezza del succitato modello emergenti dalla ricerca. Si è così cercato di proporre un nuovo modello, con particolare attenzione per la variabile strumentale, in grado di porre rimedio ai punti di debolezza e di potenziare i punti di forza del modello normativo-dottrinale.

La contabilità come mezzo per diffondere i valori religiosi. Il caso della diocesi di Ferrara del XV secolo.

Il tema del ruolo della contabilità nella Chiesa, con particolare riferimento al legame esistente tra contabilità e valori religiosi, non appare ad oggi sufficientemente studiato, soprattutto se si considera l’importanza economica e sociale di tale istituzione nel passato e nel presente. Il lavoro intende contribuire a tale indagine analizzando la realtà della Diocesi di Ferrara del XV secolo. Il Quattrocento rappresenta per la Chiesa italiana un’epoca di grande importanza, in quanto caratterizzato da un tentativo di riforma promosso da Papa Eugenio IV, volto a combattere la dilagante corruzione morale all’interno del clero e a riportare quest’ultimo alla sua funzione pastorale. L’appello pontificio venne accolto con particolare attenzione da due vescovi ferraresi, Giovanni Tavelli da Tossignano e Francesco Dal Legname, che attraverso le loro visite pastorali cercarono di divulgare i valori della riforma nella propria Diocesi. La promozione della nuova moralità, nell’esperienza ferrarese, era basata anche sulla diffusione degli strumenti contabili, mezzo essenziale per mettere in luce l’operato dei diversi membri del clero ed in particolare l’utilizzo da parte loro dei beni della Chiesa. Attraverso lo studio di documenti originali del XV secolo, scritti in lingua latina, il contributo si propone di mettere in luce come la contabilità possa assumere un ruolo complementare alla promozione dei valori religiosi.

Gli strumenti di programmazione degli enti locali. Una fotografia della realtà emiliano-romagnola

MOTIVAZIONI DI PARTENZA Gli studi sul processo di aziendalizzazione delle pubbliche amministrazioni (Hood 1991, Mussari 1994, Valotti 2000) hanno evidenziato che esse possono essere considerate aziende per tre ragioni: istituzionale, costitutiva e comportamentale (Deidda Gagliardo 2002). In particolare, gli enti locali che intendano agire come aziende dovrebbero adottare sistemi (Bertini 1990) di programmazione e controllo (D’Alessio 1992, Borgonovi 2005), funzionali ad un miglioramento delle performances economico-sociali (Anselmi 1993, Farneti 2004). Il presente lavoro è incentrato sul sub-sistema di programmazione delle amministrazioni territoriali: si focalizza l’attenzione sugli enti locali emiliano-romagnoli in quanto caratterizzati da un buon livello di aziendalizzazione (Orelli 2005). RISULTATI ATTESI L’analisi verterà sugli strumenti di programmazione utilizzati dagli enti in oggetto e sui rapporti -orizzontali e verticali (Deidda Gagliardo 2007)- intercorrenti tra gli stessi, mirando a verificarne livello e modalità di applicazione. Lo studio partirà dai risultati della ricerca “Il contributo dei sistemi di programmazione e controllo alla governance locale in Emilia-Romagna”, coordinata dal Prof. Deidda Gagliardo e condotta, rispetto all’universo di 350 enti potenziali, sul campione delle 178 amministrazioni che hanno risposto, rappresentativo di tutte le fasce dimensionali e di tutte le zone geografiche della regione. Tale ricerca, chiusa a fine 2007, ha indagato l’arco temporale 1996 - 2006. Dall’analisi dei dati ci si attende che tutti gli enti osservati adottino gli strumenti di programmazione “obbligatori”, e che l’utilizzo di quelli “facoltativi” sia circoscritto a quelli più virtuosi. La metodologia di ricerca è di tipo misto: • fase deduttiva: sono stati studiati i principali contributi teorici; • fase induttiva: è stato somministrato un questionario strutturato a risposte chiuse ai responsabili dei servizi finanziari; • fase di feedback: si procederà all’analisi critica dei risultati al fine di verificare livello e modalità di utilizzo degli strumenti di programmazione.

A statistical analysis of circumstellar material in Type Ia supernovae

A key tracer of the elusive progenitor systems of Type Ia supernovae (SNe Ia) is the detection of narrow blueshifted time-varying Na I D absorption lines, interpreted as evidence of circumstellar material surrounding the progenitor system. The origin of this material is controversial, but the simplest explanation is that it results from previous mass-loss in a system containing a white dwarf and a non-degenerate companion star. We present new single-epoch intermediate-resolution spectra of 17 low-redshift SNe Ia taken with XShooter on the European Southern Observatory Very Large Telescope. Combining this sample with events from the literature, we confirm an excess (∼20 per cent) of SNe Ia displaying blueshifted narrow Na I D absorption features compared to redshifted Na I D features. The host galaxies of SNe Ia displaying blueshifted absorption profiles are skewed towards later-type galaxies, compared to SNe Ia that show no Na I D absorption and SNe Ia displaying blueshifted narrow Na I D absorption features have broader light curves. The strength of the Na I D absorption is stronger in SNe Ia displaying blueshifted Na I D absorption features than those without blueshifted features, and the strength of the blueshifted Na I D is correlated with the B − V colour of the SN at maximum light. This strongly suggests the absorbing material is local to the SN. In the context of the progenitor systems of SNe Ia, we discuss the significance of these findings and other recent observational evidence on the nature of SN Ia progenitors. We present a summary that suggests that there are at least two distinct populations of normal, cosmologically useful SNe Ia.

Di-mu-chloro-bis({2-[(2-hydroxyethyl)iminomethyl]phenolato-kappa N-3,O,O '} nickel(II)) methanol solvate

The title compound, [Ni2Cl2(C9H10NO2)(2)]center dot CH3OH, is a dinuclear unit built up by two nickel(II) complexes, bridged by two Cl atoms. The coordination geometry around each Ni-II atom can be considered as distorted square-pyramidal, with the tridendate chelate Schiff base ligands coordinating in a trans conformation through their imine N atom and phenoxy and alkoxy O atoms.

Poly[mercury(II)-di-mu-chloro-mu-pyrazine-kappa N-2 : N ']

In [HgCl2(Pyp)](n) (Pyp = pyrazine, C4H4N2), chloride-bridged HgCl4/2 strands are connected into layers by pyrazine molecules. The Hg atom is on a site of symmetry 2/m, the unique Cl atom is on a mirror plane, the unique N atom is on a twofold rotation axis, and the unique C and H atoms are in general positions.

catena-poly[mercury(II)-di-mu-chloro-mu-pyridazine-kappa N-2 : N ']

The crystal structure of [HgCl2(Pyo)](n) (Pyo = pyridazine, C4H4N2) consists of chloride-bridged strands of octahedrally coordinated mercuric centers, connected by the two neighboring N atoms of pyridazine molecules. All atoms lie in special positions:Hg with site symmetry 2/m and the others on mirror planes.

catena-poly[mercury(II)-di-mu-bromo-mu-pyridazine-kappa N-2 : N ']

The crystal structure of [HgBr2(Pyo)](n) (Pyo = pyridazine, C4H4N2) consists of strands of octahedrally coordinated mercuric centers asymmetrically bridged by bromide and connected by the two neighboring N atoms of pyridazine molecules to complete the octahedral coordination of mercury. The Hg atoms lie on inversion centers.

Bis(tetraethylammonium) di-mu-bromo-bis[dibromomercurate(II)], (Et4N)(2)[Hg2Br6]

The structure of (Et4N)(2)[Hg2Br6] contains dinuclear [Hg2Br6](2-) species as isolated anions. Charge balance is achieved by ordered [Et4N](+) cations. An inversion centre is located at the centre of the [Hg2Br6](2-) unit.

Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for type ia supernovae

We investigate whether pure deflagration models ofChandrasekhar-mass carbon-oxygen white dwarf stars can account for one or more subclass of the observed population of Type Ia supernova (SN Ia) explosions. We compute a set of 3D full-star hydrodynamic explosion models, in which the deflagration strength is parametrized using the multispot ignition approach. For each model, we calculate detailed nucleosynthesis yields in a post-processing step with a 384 nuclide nuclear network. We also compute synthetic observables with our 3D Monte Carlo radiative transfer code for comparison with observations. For weak and intermediate deflagration strengths (energy release E {less-than or approximate} 1.1 × 10 erg), we find that the explosion leaves behind a bound remnant enriched with 3 to 10 per cent (by mass) of deflagration ashes. However, we do not obtain the large kick velocities recently reported in the literature. We find that weak deflagrations with E ~ 0.5 × 10 erg fit well both the light curves and spectra of 2002cx-like SNe Ia, and models with even lower explosion energies could explain some of the fainter members of this subclass. By comparing our synthetic observables with the properties of SNe Ia, we can exclude the brightest, most vigorously ignited models as candidates for any observed class of SN Ia: their B-V colours deviate significantly from both normal and 2002cx-like SNe Ia and they are too bright to be candidates for other subclasses.

A spectral synthesis code for rapid modelling of supernovae

We present TARDIS-an open-source code for rapid spectral modelling of supernovae (SNe). Our goal is to develop a tool that is sufficiently fast to allow exploration of the complex parameter spaces of models for SN ejecta. This can be used to analyse the growing number of highquality SN spectra being obtained by transient surveys. The code uses Monte Carlo methods to obtain a self-consistent description of the plasma state and to compute a synthetic spectrum. It has a modular design to facilitate the implementation of a range of physical approximations that can be compared to assess both accuracy and computational expediency. This will allow users to choose a level of sophistication appropriate for their application. Here, we describe the operation of the code and make comparisons with alternative radiative transfer codes of differing levels of complexity (SYN++, PYTHON and ARTIS). We then explore the consequence of adopting simple prescriptions for the calculation of atomic excitation, focusing on four species of relevance to Type Ia SN spectra-Si II, SII, MgII and Ca II. We also investigate the influence of three methods for treating line interactions on our synthetic spectra and the need for accurate radiative rate estimates in our scheme.

The effect of helium accretion efficiency on rates of Type Ia supernovae: Double detonations in accreting binaries

he double-detonation explosion scenario of Type Ia supernovae (SNe Ia) has gained increased support from the SN Ia community as a viable progenitor model, making it a promising candidate alongside the well-known single degenerate and double degenerate scenarios. We present delay times of double-detonation SNe, in which a sub-Chandrasekhar mass carbon–oxygen white dwarf (WD) accretes non-dynamically from a helium-rich companion. One of the main uncertainties in quantifying SN rates from double detonations is the (assumed) retention efficiency of He-rich matter. Therefore, we implement a new prescription for the treatment of accretion/accumulation of He-rich matter on WDs. In addition, we test how the results change depending on which criteria are assumed to lead to a detonation in the helium shell. In comparing the results to our standard case (Ruiter et al.), we find that regardless of the adopted He accretion prescription, the SN rates are reduced by only ∼25 per cent if low-mass He shells (≲0.05 M⊙) are sufficient to trigger the detonations. If more massive (0.1 M⊙) shells are needed, the rates decrease by 85 per cent and the delay time distribution is significantly changed in the new accretion model – only SNe with prompt (<500 Myr) delay times are produced. Since theoretical arguments favour low-mass He shells for normal double-detonation SNe, we conclude that the rates from double detonations are likely to be high, and should not critically depend on the adopted prescription for accretion of He.

Synthetic light curves and spectra for three-dimensional delayed-detonation models of type ia supernovae

In a companion paper, Seitenzahl et al. have presented a set of three-dimensional delayed detonation models for thermonuclear explosions of near-Chandrasekhar-mass white dwarfs (WDs). Here,we present multidimensional radiative transfer simulations that provide synthetic light curves and spectra for those models. The model sequence explores both changes in the strength of the deflagration phase (which is controlled by the ignition configuration in our models) and the WD central density. In agreement with previous studies, we find that the strength of the deflagration significantly affects the explosion and the observables. Variations in the central density also have an influence on both brightness and colour, but overall it is a secondary parameter in our set of models. In many respects, the models yield a good match to the observed properties of normal Type Ia supernovae (SNe Ia): peak brightness, rise/decline time-scales and synthetic spectra are all in reasonable agreement. There are, however, several differences. In particular, the models are systematically too red around maximum light, manifest spectral line velocities that are a little too high and yield I-band light curves that do not match observations. Although some of these discrepancies may simply relate to approximations made in the modelling, some pose real challenges to the models. If viewed as a complete sequence, our models do not reproduce the observed light-curve width- luminosity relation (WLR) of SNe Ia: all our models show rather similar B-band decline rates, irrespective of peak brightness. This suggests that simple variations in the strength of the deflagration phase in Chandrasekhar-mass deflagration-to-detonation models do not readily explain the observed diversity of normal SNe Ia. This may imply that some other parameter within the Chandrasekhar-mass paradigm is key to the WLR, or that a substantial fraction of normal SNe Ia arise from an alternative explosion scenario.

'Super-Chandrasekhar' Type Ia Supernovae at nebular epochs

We present a first systematic comparison of superluminous Type Ia supernovae (SNe Ia) at late epochs, including previously unpublished photometric and spectroscopic observations of SN 2007if, SN 2009dc and SNF20080723-012. Photometrically, the objects of our sample show a diverse late-time behaviour, some of them fading quite rapidly after a light-curve break at ∼ 150-200 d. The latter is likely the result of flux redistribution into the infrared, possibly caused by dust formation, rather than a true bolometric effect. Nebular spectra of superluminous SNe Ia are characterized by weak or absent [Fe III] emission, pointing at a low ejecta ionization state as a result of high densities. To constrain the ejecta and Ni masses of superluminous SNe Ia, we compare the observed bolometric light curve of SN 2009dc with synthetic model light curves, focusing on the radioactive tail after ∼60 d. Models with enough Ni to explain the light-curve peak by radioactive decay, and at the same time sufficient mass to keep the ejecta velocities low, fail to reproduce the observed light-curve tail of SN 2009dc because of too much γ -ray trapping.We instead propose a model with ∼1M of Ni and ∼2 M of ejecta, which may be interpreted as the explosion of a Chandrasekhar-mass white dwarf (WD) enshrouded by 0.6-0.7 M of C/O-rich material, as it could result from a merger of two massive C/O WDs. This model reproduces the late light curve of SN 2009dc well. A flux deficit at peak may be compensated by light from the interaction of the ejecta with the surrounding material.

Preparation and characterisation of palladium, platinum and manganese di(organo)carbene complexes from quinolinone and quinolinium precursors

A series of palladium, platinum and manganese di(organo) carbene complexes have been prepared from 4-chloro-N-methylquinolinone by processes that involve alkylation before or after attachment to the metal unit; the nucleophilic heteroatoms necessary for eventual carbene formation and stabilisation are separated from the C-donor atom by three bonds.