Creative process in globally distributed teams: a study of new product development in Volvo

With the business environments no longer confined to geographical borders, the new wave of digital technologies has given organizations an enormous opportunity to bring together their distributed workforce and develop the ability to work together despite being apart (Prasad & Akhilesh, 2002). resupposing creativity to be a social process, the way that this phenomenon occurs when the configuration of the team is substantially modified will be questioned. Very little is known about the impact of interpersonal relationships in the creativity (Kurtzberg & Amabile, 2001). In order to analyse the ways in which the creative process may be developed, we ought to be taken into consideration the fact that participants are dealing with a quite an atypical situation. Firstly, in these cases socialization takes place amongst individuals belonging to a geographically dispersed workplace, where interpersonal relationships are mediated by the computer, and where trust must be developed among persons who have never met one another. Participants not only have multiple addresses and locations, but above all different nationalities, and different cultures, attitudes, thoughts, and working patterns, and languages. Therefore, the central research question of this thesis is as follows: “How does the creative process unfold in globally distributed teams?” With a qualitative approach, we used the case study of the Business Unit of Volvo 3P, an arm of Volvo Group. Throughout this research, we interviewed seven teams engaged in the development of a new product in the chassis and cab areas, for the brands Volvo and Renault Trucks, teams that were geographically distributed in Brazil, Sweden, France and India. Our research suggests that corporate values, alongside with intrinsic motivation and task which lay down the necessary foundations for the development of the creative process in GDT.

Statistical properties of Radio Halos and the re-acceleration model

Galaxy clusters occupy a special position in the cosmic hierarchy as they are the largest bound structures in the Universe. There is now general agreement on a hierarchical picture for the formation of cosmic structures, in which galaxy clusters are supposed to form by accretion of matter and merging between smaller units. During merger events, shocks are driven by the gravity of the dark matter in the diffuse barionic component, which is heated up to the observed temperature. Radio and hard-X ray observations have discovered non-thermal components mixed with the thermal Intra Cluster Medium (ICM) and this is of great importance as it calls for a “revision” of the physics of the ICM. The bulk of present information comes from the radio observations which discovered an increasing number of Mpcsized emissions from the ICM, Radio Halos (at the cluster center) and Radio Relics (at the cluster periphery). These sources are due to synchrotron emission from ultra relativistic electrons diffusing through µG turbulent magnetic fields. Radio Halos are the most spectacular evidence of non-thermal components in the ICM and understanding the origin and evolution of these sources represents one of the most challenging goal of the theory of the ICM. Cluster mergers are the most energetic events in the Universe and a fraction of the energy dissipated during these mergers could be channelled into the amplification of the magnetic fields and into the acceleration of high energy particles via shocks and turbulence driven by these mergers. Present observations of Radio Halos (and possibly of hard X-rays) can be best interpreted in terms of the reacceleration scenario in which MHD turbulence injected during these cluster mergers re-accelerates high energy particles in the ICM. The physics involved in this scenario is very complex and model details are difficult to test, however this model clearly predicts some simple properties of Radio Halos (and resulting IC emission in the hard X-ray band) which are almost independent of the details of the adopted physics. In particular in the re-acceleration scenario MHD turbulence is injected and dissipated during cluster mergers and thus Radio Halos (and also the resulting hard X-ray IC emission) should be transient phenomena (with a typical lifetime <» 1 Gyr) associated with dynamically disturbed clusters. The physics of the re-acceleration scenario should produce an unavoidable cut-off in the spectrum of the re-accelerated electrons, which is due to the balance between turbulent acceleration and radiative losses. The energy at which this cut-off occurs, and thus the maximum frequency at which synchrotron radiation is produced, depends essentially on the efficiency of the acceleration mechanism so that observations at high frequencies are expected to catch only the most efficient phenomena while, in principle, low frequency radio surveys may found these phenomena much common in the Universe. These basic properties should leave an important imprint in the statistical properties of Radio Halos (and of non-thermal phenomena in general) which, however, have not been addressed yet by present modellings. The main focus of this PhD thesis is to calculate, for the first time, the expected statistics of Radio Halos in the context of the re-acceleration scenario. In particular, we shall address the following main questions: • Is it possible to model “self-consistently” the evolution of these sources together with that of the parent clusters? • How the occurrence of Radio Halos is expected to change with cluster mass and to evolve with redshift? How the efficiency to catch Radio Halos in galaxy clusters changes with the observing radio frequency? • How many Radio Halos are expected to form in the Universe? At which redshift is expected the bulk of these sources? • Is it possible to reproduce in the re-acceleration scenario the observed occurrence and number of Radio Halos in the Universe and the observed correlations between thermal and non-thermal properties of galaxy clusters? • Is it possible to constrain the magnetic field intensity and profile in galaxy clusters and the energetic of turbulence in the ICM from the comparison between model expectations and observations? Several astrophysical ingredients are necessary to model the evolution and statistical properties of Radio Halos in the context of re-acceleration model and to address the points given above. For these reason we deserve some space in this PhD thesis to review the important aspects of the physics of the ICM which are of interest to catch our goals. In Chapt. 1 we discuss the physics of galaxy clusters, and in particular, the clusters formation process; in Chapt. 2 we review the main observational properties of non-thermal components in the ICM; and in Chapt. 3 we focus on the physics of magnetic field and of particle acceleration in galaxy clusters. As a relevant application, the theory of Alfv´enic particle acceleration is applied in Chapt. 4 where we report the most important results from calculations we have done in the framework of the re-acceleration scenario. In this Chapter we show that a fraction of the energy of fluid turbulence driven in the ICM by the cluster mergers can be channelled into the injection of Alfv´en waves at small scales and that these waves can efficiently re-accelerate particles and trigger Radio Halos and hard X-ray emission. The main part of this PhD work, the calculation of the statistical properties of Radio Halos and non-thermal phenomena as expected in the context of the re-acceleration model and their comparison with observations, is presented in Chapts.5, 6, 7 and 8. In Chapt.5 we present a first approach to semi-analytical calculations of statistical properties of giant Radio Halos. The main goal of this Chapter is to model cluster formation, the injection of turbulence in the ICM and the resulting particle acceleration process. We adopt the semi–analytic extended Press & Schechter (PS) theory to follow the formation of a large synthetic population of galaxy clusters and assume that during a merger a fraction of the PdV work done by the infalling subclusters in passing through the most massive one is injected in the form of magnetosonic waves. Then the processes of stochastic acceleration of the relativistic electrons by these waves and the properties of the ensuing synchrotron (Radio Halos) and inverse Compton (IC, hard X-ray) emission of merging clusters are computed under the assumption of a constant rms average magnetic field strength in emitting volume. The main finding of these calculations is that giant Radio Halos are naturally expected only in the more massive clusters, and that the expected fraction of clusters with Radio Halos is consistent with the observed one. In Chapt. 6 we extend the previous calculations by including a scaling of the magnetic field strength with cluster mass. The inclusion of this scaling allows us to derive the expected correlations between the synchrotron radio power of Radio Halos and the X-ray properties (T, LX) and mass of the hosting clusters. For the first time, we show that these correlations, calculated in the context of the re-acceleration model, are consistent with the observed ones for typical µG strengths of the average B intensity in massive clusters. The calculations presented in this Chapter allow us to derive the evolution of the probability to form Radio Halos as a function of the cluster mass and redshift. The most relevant finding presented in this Chapter is that the luminosity functions of giant Radio Halos at 1.4 GHz are expected to peak around a radio power » 1024 W/Hz and to flatten (or cut-off) at lower radio powers because of the decrease of the electron re-acceleration efficiency in smaller galaxy clusters. In Chapt. 6 we also derive the expected number counts of Radio Halos and compare them with available observations: we claim that » 100 Radio Halos in the Universe can be observed at 1.4 GHz with deep surveys, while more than 1000 Radio Halos are expected to be discovered in the next future by LOFAR at 150 MHz. This is the first (and so far unique) model expectation for the number counts of Radio Halos at lower frequency and allows to design future radio surveys. Based on the results of Chapt. 6, in Chapt.7 we present a work in progress on a “revision” of the occurrence of Radio Halos. We combine past results from the NVSS radio survey (z » 0.05 − 0.2) with our ongoing GMRT Radio Halos Pointed Observations of 50 X-ray luminous galaxy clusters (at z » 0.2−0.4) and discuss the possibility to test our model expectations with the number counts of Radio Halos at z » 0.05 − 0.4. The most relevant limitation in the calculations presented in Chapt. 5 and 6 is the assumption of an “averaged” size of Radio Halos independently of their radio luminosity and of the mass of the parent clusters. This assumption cannot be released in the context of the PS formalism used to describe the formation process of clusters, while a more detailed analysis of the physics of cluster mergers and of the injection process of turbulence in the ICM would require an approach based on numerical (possible MHD) simulations of a very large volume of the Universe which is however well beyond the aim of this PhD thesis. On the other hand, in Chapt.8 we report our discovery of novel correlations between the size (RH) of Radio Halos and their radio power and between RH and the cluster mass within the Radio Halo region, MH. In particular this last “geometrical” MH − RH correlation allows us to “observationally” overcome the limitation of the “average” size of Radio Halos. Thus in this Chapter, by making use of this “geometrical” correlation and of a simplified form of the re-acceleration model based on the results of Chapt. 5 and 6 we are able to discuss expected correlations between the synchrotron power and the thermal cluster quantities relative to the radio emitting region. This is a new powerful tool of investigation and we show that all the observed correlations (PR − RH, PR − MH, PR − T, PR − LX, . . . ) now become well understood in the context of the re-acceleration model. In addition, we find that observationally the size of Radio Halos scales non-linearly with the virial radius of the parent cluster, and this immediately means that the fraction of the cluster volume which is radio emitting increases with cluster mass and thus that the non-thermal component in clusters is not self-similar.

Benvenuto Rambaldi da Imola: dantista in progress

Si procede ad un’analisi diacronica delle tre redazioni del commento dantesco di Benvenuto da Imola (dalle "recollectae" bolognesi e ferraresi al "Comentum"), considerando il testo benvenutiano quale «opera umana o lavoro in fieri», di cui rappresentare «drammaticamente la vita dialettica», così come il Contini iniziava a fare, negli anni ’30, con gli ʻscartafacciʼ ariosteschi. Secondo tale impostazione, si prende in esame la multiforme attitudine pedagogica di Benvenuto, di cui si indica, con riferimento ad altri commentatori coevi, danteschi e non, il contesto operativo. Nella seconda parte si ricostruisce, in senso sempre diacronico, la problematica oscillazione del commentatore tra tendenze avanguardistiche in direzione umanistico-petrarchesca e strenua apologia del testo dantesco. Nella terza ed ultima parte sono vagliate le originali idee benvenutiane riguardo alla lingua e alla poesia della Commedia, delle quali si ripercorre, attraverso l’esame delle varianti redazionali, la progressiva messa a fuoco. Obiettivo dell’elaborato, insomma, è restituire una descrizione organica e problematica della ricerca dantesca, "in progress", portata avanti da Benvenuto da Imola.

History of Restoration in Iran: Origins and Developments from 1900 to 1978

This thesis tends to study the origins and developments of the restoration in Iran from its very first moments till the Islamic revolution of 1978. The thesis is its first study of its kind. While almost all recent occidental ideologies regarding the thematic of restoration and conservation of historic monuments are translated and published in Iran, very little efforts have been done regarding the study of the origins of the formation of restoration in the country. The diversity of Iranian contexts, multiplicity of the intervening factors and other factors characterized a different background for the raise and developments of restoration in the country; in the thesis the influencing and characterizing factors in the formation and development of restoration in Iran will be defined and studied in detail with relative examples; due to the complexity of the Iranian context and in order to consider all influencing and characterizing factors the thesis, parallel to have formation and development of restoration, as the main scope of the research, the developments influencing factors will be confronted with necessary flashbacks to the main theme, when and where necessary. A great care will be given to the period of the activity of the restoration experts of IsMEO which is thesis will be called as the period of the introduction of the modern principles of restoration into Iranian context; the fundamental ideologies, practical and theoretical principles of IsMEO will be identified and studied in details; important case of studies of the restoration of IsMEO will be analyzed in details and the innovative aspect of the presence of Italian experts of IsMEO will be revealed.

In campo. Il ruolo pubblico dell'antropologia

La tesi riflette sulla necessità di un ripensamento delle scienze antropologiche nel senso di un loro uso pubblico e del loro riconoscimento al di fuori dell’accademia. Viene introdotto il dibattito sulla dimensione applicata dell’antropologia a partire dalle posizioni in campo nel panorama internazionale. Negli Stati Uniti la riflessione si sviluppa dalla proposta della public anthropology, l’antropologo pubblico si discosta dalla tradizionale figura europea di intellettuale pubblico. Alla luce delle varie posizioni in merito, la questione dell’applicazione è esaminata dal punto di vista etico, metodologico ed epistemologico. Inizialmente vengono prese in considerazione le diverse metodologie elaborate dalla tradizione dell’applied anthropology a partire dalle prime proposte risalenti al secondo dopoguerra. Successivamente viene trattata la questione del rapporto tra antropologia, potere coloniale e forze armate, fino al recente caso degli antropologi embedded nello Human Terrain System. Come contraltare vengono presentate le diverse forme di engagement antropologico che vedono ricercatori assumere diversi ruoli fino a casi estremi che li vedono divenire attivisti delle cause degli interlocutori. La questione del ruolo giocato dal ricercatore, e di quello che gli viene attribuito sul campo, viene approfondita attraverso la categoria di implication elaborata in contesto francese. Attraverso alcune esperienze di campo vengono presentate forme di intervento concreto nel panorama italiano che vogliono mettere in luce l’azione dell’antropologo nella società. Infine viene affrontato il dibattito, in corso in Italia, alla luce della crisi che sta vivendo la disciplina e del lavoro per la costituzione dell’associazione nazionale di antropologia professionale.