An Integrated Approach to Government Financial Policy

In this paper, I address three questions of government financial policy: how should a government’s aversion to financial risk be determined, when are new financial investments justified, and what is the optimal level of reserves in a flexible exchange rate regime. To answer these questions, I modify an integrated financial model developed by Froot and Stein (1998) to describe private sector financial policy. Financial risk aversion in this model is due to the potential of poor financial returns limiting an institution’s future investment opportunities. The potential for poor returns provides governments with incentives to hold reserves and limit new financial investments.

Applying a simple measure of good governance to the debate on fiscal decentralization

Debates about the appropriate role, policies, and institutions of the state are often hampered by the lack of a definition for good government. To provide a quantifiable measure of good government, the authors develop an index for the quality of governance for a sample of 80 countries. They apply the index to the debate on the appropriate level of fiscal decentralization. In measuring the quality of governance, the authors develop indices for the government's ability to: a) Ensure political transparency and a voice for all citizens (the citizen participation index measures political freedom and political stability). b) Provide effective public services efficiently (the government orientation index measures judicial and bureaucratic efficiency and the absence of corruption). c) Promote the health and well-being of its citizens (the social development index measures human development and equitable distribution of income). d) Create a favorable climate for stable economic growth (the economic management index measures outward orientation, independence of the central bank, and an inverted debt-to-GDP ratio). In relating the index of governance quality to degree of fiscal decentralization for the 80 countries, the authors are not surprised to find a positive relationship between fiscal decentralization and quality of governance. But the strength of the correlation is surprising.Banks&Banking Reform,Decentralization,Municipal Financial Management,Economic Theory&Research,Health Economics&Finance,Municipal Financial Management,National Governance,Governance Indicators,Economic Theory&Research,Banks&Banking Reform

Supernova neutrinos and nucleosynthesis

Observations of metal-poor stars indicate that at least two different nucleosynthesis sites contribute to the production of r-process elements. One site is responsible for the production of light r-process elements Z<~50 while the other produces the heavy r-process elements. We have analyzed recent observations of metal-poor stars selecting only stars that are enriched in light r-process elements and poor in heavy r-process elements. We find a strong correlation between the observed abundances of the N=50 elements (Sr, Y and Zr) and Fe. It suggest that neutrino-driven winds from core-collapse supernova are the main site for the production of these elements. We explore this possibility by performing nucleosynthesis calculations based on long term Boltzmann neutrino transport simulations. They are based on an Equation of State that reproduces recent constrains on the nuclear symmetry energy. We predict that the early ejecta is neutron-rich with Ye ~ 0.48, it becomes proton rich around 4 s and reaches Ye = 0.586 at 9 s when our simulation stops. The nucleosynthesis in this model produces elements between Zn and Mo, including 92Mo. The elemental abundances are consistent with the observations of the metal-poor star HD 12263. For the elements between Ge and Mo, we produce mainly the neutron-deficient isotopes. This prediction can be confirmed by observations of isotopic abundances in metal-poor stars. No elements heavier than Mo (Z=42) and no heavy r-process elements are produced in our calculations.Comment: 18 pages, 5 figures, submitted to J. Phys. G: Nucl. Part. Phys. (Focus issue "Nucleosynthesis and the role of neutrinos", ed. Baha Balantekin and Cristina Volpe

Replacement of the Legacy High-Cost Universal Support Fund with a Connect America Fund. Key Economic and Legal Considerations

On April 21, 2010, the Federal Communications Commission (FCC) released a Notice of Inquiry (NOI) and a Notice of Proposed Rulemaking (NPRM) that seek the public’s input on the FCC’s effort to replace the legacy high-cost universal service fund (USF) with a broadband “Connect America” fund (CAF). In effect, the FCC seeks to implement cost-cutting measures for existing voice support (USF) and create a new fund (CAF) to support the provision of broadband communications in areas that would be unserved without such support or that depend on USF support for the maintenance of existing broadband service. An initial review of the NOI/NPRM raises a number of key economic and legal considerations. In the following, we identify some of the considerations, questions, and challenges raised by the FCC’s USF reform attempt, which is likely to have far-reaching consequences not only for operators that currently rely on USF subsidies or broadband providers in high-cost regions but for the entire communications industry.The purpose of this note is not to provide an all-inclusive list of, or responses to, the critical questions raised by the NOI/NPRM, but rather to illustrate the complexities of this proceeding and the impact the proposed reforms may have on industry performance. As the CAF is necessary for the success of the FCC’s National Broadband Plan (NBP), the policy directions taken by the FCC in establishing it are critically important. USF reform is also essential to the performance and competitiveness of the U.S. communications industry and policy missteps could have serious economic and legal consequences.Federal Communications Commission, America Fund

Fabrication and Application of Flexible Sensors

A transfer printing method was developed to transfer carbon nanotubes (CNTs) from polyethylene terephthalate (PET) film to poly(dimethyl siloxane) (PDMS) polymer. Carbon nanotubes are composed of carbon atoms arranged in a honeycomb lattice structure, which are electrically conducting. When embedded in a nonconducting polymer, carbon nanotubes impart electrical conductivity to the nanocomposite, thus forming a nanocomposite that has potential applications in highly sensitive strain and pressure sensors. Several printing methods have been studied to deposit carbon nanotubes onto PDMS, including inkjet printing. Inkjet printing is a desirable deposition method since it is low-cost, simple, and allows the processing of aqueous-based inks. However, directly inkjet printing carbon nanotubes onto PDMS has been a challenge because the printed film becomes non-uniform due to the uneven drying of the droplets. Therefore, a method of transfer printing was developed to embed carbon nanotubes uniformly in PDMS. The transfer printing method consists of first inkjet printing patterns of carbon nanotubes onto a PET film, which quickly absorbs the aqueous ink and allows uniformity of the printed carbon nanotube patterns. The next step is spin-coating PDMS on the PET film to cover the carbon nanotube patterns, followed by curing the PDMS. The following step is thermally treating the PET film to promote the transfer of carbon nanotubes to PDMS, and finally peeling off PDMS from PET film to complete the transfer of carbon nanotube patterns. The transferred patterns had widths as small as 125 µm, while the obtained PDMS thickness was as low as 27.1 µm, which enabled the fabrication of highly sensitive force and pressure sensors. The transfer printing method was employed to fabricate a two-dimensional force sensor, which was composed of lines of carbon nanotubes in the x and y directions. The transduction mechanism lies in the generation of strain on the carbon nanotube pattern. When strain is produced, the resistance of the pattern changes due to the increase or decrease of the number of conduction paths in the carbon nanotube pattern. The practical application as a two-dimensional sensor was shown by monitoring the touch force exerted by multiple objects on the sensor. Due to the flexibility and stretchability of PDMS, fabricated air pressure sensors were capable of detecting small pressure differences. The sensors were composed of a circular diaphragm containing inkjet-printed carbon nanotube patterns. When air pressure increased on one side of the diaphragm, the deflection caused a strain on the CNT line, thus changing its resistance. Pressure sensors with a diaphragm diameter of five millimeters, diaphragm thickness of 27.1 µm showed sensitivity of 10.99 percent change in resistance per kilopascal (%/kPa) and limit of detection of 3.1 Pa. The pressure sensor has potential applications in monitoring minute air pressure differences such as those generated by the breathing pattern. The application of the highly sensitive and biocompatible pressure sensor was shown through the measurement of the pressure generated by a 3D-printed respiratory system

Neutrino Nucleosynthesis of radioactive nuclei in supernovae

We study the neutrino-induced production of nuclides in explosive supernova nucleosynthesis for progenitor stars with solar metallicity and initial main sequence masses between 15 M$_\odot$ and 40 M$_\odot$. We improve previous investigations i) by using a global set of partial differential cross sections for neutrino-induced charged- and neutral-current reactions on nuclei with charge numbers $Z < 76$ and ii) by considering modern supernova neutrino spectra which have substantially lower average energies compared to those previously adopted in neutrino nucleosynthesis studies. We confirm the production of $^7$Li, $^{11}$B, $^{138}$La, and $^{180}$Ta by neutrino nucleosynthesis, albeit at slightly smaller abundances due to the changed neutrino spectra. We find that for stars with a mass smaller than 20 M$_\odot$, $^{19}$F is produced mainly by explosive nucleosynthesis while for higher mass stars it is produced by the $\nu$ process. We also find that neutrino-induced reactions, either directly or indirectly by providing an enhanced abundance of light particles, noticeably contribute to the production of the radioactive nuclides $^{22}$Na and $^{26}$Al. Both nuclei are prime candidates for gamma-ray astronomy. Other prime targets, $^{44}$Ti and $^{60}$Fe, however, are insignificantly produced by neutrino-induced reactions. We also find a large increase in the production of the long-lived nuclei $^{92}$Nb and $^{98}$Tc due to charged-current neutrino capture.Comment: 6 pages, 2 figures, 2 table

Chimeras

What types of human-animal interspecific entities are used in biomedical research? Is creating such entities morally wrong? And what do interspecifics tell us about the moral significance of species? This thesis offers an introduction to the field of human-animal interspecifics from a bioethical perspective, with a special focus on the question of speciesism

Nucleosynthesis in neutrino-driven winds

In this thesis the influence of neutrino-induced spallation rates on the nucleosynthesis is investigated. These neutrino-induced rates are studied in various nucleosynthesis processes such as the ν p-process, the r-process and the ν-process. The astrophysical site connecting all these different processes is the core-collapse supernova. Therefore our nucleosynthesis results are dependent on the information obtained by core-collapse supernova simulations and their correct input physics. The production of heavy elements in the core-collapse supernova is dominantly related to the neutrino-driven wind phase, in which matter is ejected from the proto-neutron star due to neutrino-nucleon interactions. Astrophysical parameters in the neutrino-driven wind, such as entropy and electron fraction, will determine which nucleosynthesis process occurs. The traversing shock will, when passing through the outer layers of the star, also have influence on the final nucleosynthesis. The matter in the outer layers of the star will also be subject to the neutrino fluxes from the proto-neutron star. The question that we would like to raise in this thesis is, if neutrino-induced spallation processes have influence on the nucleosynthesis. The neutrino-induced spallation rates have been obtained in a two-step process. In a first step the excitation of the nucleus is described. The second step describes the decay of the excited nucleus. The neutrino- nucleus excitation rates have been calculated for charged-current and neutral-current processes. The nuclear excitation spectra of the target nuclei are calculated with the help of a spherical RPA based on Woods-Saxon single-particle states, adjusted to reproduce the correct separation energies. The used interaction has been of the Landau-Migdal type. The excitation-spectrum includes excitations up to J = 4. For the neutrino energies in a core-collapse supernova, the excitation spectra peaks in the region of the giant resonances, which can be located above the particle threshold. Thus, it it necessary to consider not only the total cross section, but instead to consider partial cross sections for the spallation of light particles from the excited nucleus. This approach is described in a statistical model, where the usual formation cross section is replaced by the neutrino-induced nuclear excitation cross section. The one-particle spallation probability has been calculated with the statistical code MOD-SMOKER which is based on SMOKER – a statistical reaction code with wide application in astrophysics [4, 5, 6, 7]. This code has the advantages that it has explicit knowledge of low lying experimental states, as long as they are experimentally known with its spin and parity value. Furthermore the transmission through the Coulomb potential is treated correctly by confluent hypergeometric functions. The largest disadvantage is, that it only allows for one-particle spallation and does not cover cascade reactions that might occur, if the energies of the neutrinos coming from the proto-neutron star are high enough, or the separation energies are small. Therefore, below the first two-particle emission channel opening, we change the description of the decay probabilities to a model that allows for multi-particle spallation. The code used for this description is the dynamical code ABLA07, that explicitly allows for several particle emissions. Which decay channels will be available for each nucleus is very sensitive to the energy distribution of the neutrinos. We calculated the decay probabilities up to four particle evaporation processes to determine the partial cross section. We made sure that the decay probabilities at the transition between the two models agree and give a smooth transition. The partial cross sections – obtained as a function of incoming neutrino energy – have been folded with a respective supernova neutrino spectrum, parameterized as a Fermi-Dirac function with the parameters neutrino temperature Tν and chemical potential μν . The chemical potential is usually assumed to be zero. This distribution type has been utilized extensively in the past decades, which is the reason why we kept this description also in this work, although different descriptions are available for the neutrino spectra. Changing to one of these alternative descriptions within our model for the neutrino-spectra, such as the α-fit, can be done quite easily. Once our neutrino induced evaporation processes were calculated, we required to implement the neutrino rates in a nuclear reaction network. The utilized nuclear reaction network has so far only been used for the calculation of r-process nucleosynthesis studies including fission cycling [8, 9]. For a better description of the weak interactions close to the proto-neutron star where high densities are available that can influence the electron capture rates, the weak interaction rates from [10] have been included. After generating a working network that accounts for our neutrino-nucleus interactions, we could observe their influence in several nucleosynthesis studies where high neutrino fluxes are expected. These studies were related to various different nucleosynthesis processes assigned to core-collapse supernovae scenarios. These reach from the nucleosynthesis in the neutrino-driven wind to the shock passage through the outer layers of the former star. Within our thesis we have considered different astrophysical parameters for the neutrino-driven wind nucleosynthesis, that actually are based on data from core-collapse supernova simulations. The main input parameter are the neutrino and antineutrino spectra from the cooling of the proto-neutron star, since these will determine the electron fraction. The astrophysical parameters for the neutrino-driven wind of current core simulations are such that the values of entropy and electron fraction are not extreme enough to fulfill the requirements for a successful r-process. Before 2012 it has been shown that the ejecta from the PNS surface are proton rich ( Ye > 0.5) [11]. Due to νp-nucleosynthesis this proton rich matter can contribute to the heavy element nucleosynthesis [48]. Therefore we calculated the nucleosynthesis of this proton rich neutrino-driven wind with the inclusion of our newly determined spallation rates. It turned out that the nucleosynthesis is governed by the antineutrino capture processes on free protons, since the abundance of free protons is high. Furthermore are we able to see, that the partial cross section for neutron emission in neutron deficient nuclei is very small, since proton emissions are more favorable. The second argument against strong changes due to the inclusion of neutrino-nucleus spallation processes is, that the abundance of these heavy elements is substantially lower than the abundance of free protons. Within our study we also posed the question if the observed abundance pattern of r-process poor stars – such as HD 122563 – can be explained with the nucleosynthesis in neutrino-driven wind nucleosynthesis. Therefore we calculated the integrated neutrino-driven wind nucleosynthesis of long-term core-collapse supernovae simulations with different progenitor masses. We were able to observe that with increasing mass of the progenitor, ν p-nucleosynthesis acts more efficiently due to the fact that matter is expanding slower and therefore keeping matter longer in the right conditions for ν p-nucleosynthesis. Thus for an 18 M model an agreement with the metal-poor star’s abundance can be obtained between the elemental abundance pattern and the obtained nucleosynthetic result up to a mass number of roughly Z = 44. The newly included neutrino-spallation rates do not contribute so much that the heavy element nucleosynthesis is changed strongly. Changes can nevertheless be observed in the region of light elements. For example does 7 11the inclusion of neutrinos severely influence the creation of elements as Li and B. However, the total ejected mass of these light elements is too little to contribute to the total nucleosynthesis of the star. In mid of 2012 core-collapse supernova simulations showed that ejecta in the neutrino-driven wind with improved charged-current neutrino nucleon processes, that are treated consistently with the underlying equation of state, can reach values that are initially below 0.5 and are therefore neutron-rich [140]. Later ejecta will become proton rich again, due to the fact that during the cooling of the PNS the spectra become more and more similar. Thus late ejecta will undergo νp-nucleosynthesis, while this is not possible for the early neutron rich ejecta. Within this work we studied the integrated neutrino-driven wind of a current core-collapse supernova model, that includes the above improved treatment, with a progenitor mass of 11.2 M . The electron fraction shows initially neutron rich ejecta ( Ye = 0.474), while later material will again become proton rich. The nucleosynthesis is hereby dominated by the initial neutron rich ejecta, since the mass flux from the PNS decreases very fast. Thus, depending on the mass flux from the proto-neutron star, this will hinder the matter production over the ν p-process. However, the elements usually assigned to the ν p-process – such as 92Mo – are also created in the neutron-rich ejecta, that still produces dominantly neutron deficient material. The neutron rich ejecta show a minor influence on the newly included spallation rates in the nucleosynthesis. In the integrated result these influences are noticeable for the neutron rich stable elements. Large changes due to the inclusion of neutrino-nucleus processes can again be found for the lighter elements, where elements such as 7Li and 11 B are produced due to the inclusion of neutral-current neutrino spallation processes. However, the production factor is too small to be considered as an astrophysical site for the production of these elements. The elemental abundance pattern has been compared to the metal-poor star HD 122563, where it is found that matter can reproduce the abundance pattern up to Z = 42. Heavier elements than Z = 42 could not be produced, due to the neutron shell closure of N = 50. By comparison with the data from the metal-poor star HD 122563, we are only able to gain information on the elemental abundance pattern. As we can see from the isotopic distribution of our nucleosynthesis results in figure 4.17, we see that we overproduce the neutron deficient nuclei in comparison to the solar abundance, whereas neutron rich stable isotopes are underproduced. We are not able to say if this abundance pattern can be also observed in metal-poor stars like HD 122563, because we do not have information on the isotopic abundance. If the abundance pattern would be as it is in our solar system, it would require for another astrophysical site that can explain the creation of the neutron rich elements. The next astrophysical process that we studied in our work was r-process nucleosynthesis in the neutrino-driven wind. Due to the fact that the astrophysical site for r-process nucleosynthesis is still not fully settled and galactic chemical evolution models favor the core-collapse supernova environment as a possible site for the r-process, we utilized a neutrino-driven wind scenario in which an electron fraction of 0.469 at a temperature of T=3 × 109 K was reached. To obtain an r-process that is able to reach mass numbers around A=195, the entropy has been increased by a factor of 2. The luminosities and mean energies for the neutrino spectra have been taken from the original simulation [13]. Since no data has been given for μ- and τ-flavor neutrinos, a variation of these values – within a physical reasonable regime – could be used to observe the influence on neutral-current neutrino-induced particle spallation. To observe only the changes due to the inclusion of neutrino-nucleus processes, we kept for all calculations the rates of free protons and neutrons such, that the electron fraction does not change due to the neglect of these processes. We recognized that the inclusion of charged-current neutrino processes on nuclei do not change the final r-process nucleosynthesis much, whereas neutral-current processes lead to a reduction of the heavy elements produced in this ejecta. Therefore the inclusion of all neutrino rates is dominated by neutral-current processes. The relevant process for neutral-current nucleus processes is the spallation of 4 He, where proton-spallation leads to the reduction of the neutron- to-seed ratio, due to the increased production of heavy elements by subsequent α-captures, starting with the 3H(α, γ)7 Li reaction. We saw that the nucleosynthesis is sensitive to the used neutrino spectra for μ- and τ-flavor, since they have the most influence on neutral-current neutrino processes, as long as the usual energy hierarchy is valid. We should note once more that the astrophysical conditions from state-of-the-art core-collapse simulations favor the production of these light r-process elements (Sr, Y, Zr) over the ν p-processs or slightly neutron rich matter in their wind ejecta, as we have shown above. The question that cannot be explained in current models is, how the abundance pattern of heavy r-process elements (e.g. europium) are created, which are also observed in metal-poor stars such as HD 122563 [36]. Furthermore we studied the hot convective bubble, in which matter is ejected due to neutrino interactions [12, 47]. The matter emission does not occur directly from the proto-neutron star surface, instead it is further away in a region of a few hundred kilometers. The electron-fraction of these ejecta resides between 0.5 and 0.54, where early ejecta have values close to 0.5 and later ejecta become more proton rich. Note that these simulations do not consider the improved description of microphysics in the proto-neutron star. For these ejecta the inclusion of neutrino-nucleus processes do not change the heavy element production tremendously. The only fact that we could observe is that some production of heavy elements over the ν p-process could be made, which however is also very minimal. In a next step we focused on the nucleosynthesis in the outer shells of the exploding star, where the neutrinos, produced by the proto-neutron star, traverse through. The neutrino fluxes are of course less than in the case of the neutrino-driven wind – due to the radial decrease with 1/r 2 . As already shown in previous works [2, 3] the inclusion of neutrino interactions in this region does have influence on the odd-Z elements in the nucleosynthesis. The reason can be found in the elemental abundance ratio, where odd-Z elements show always less abundance than the even-Z nuclei. As it has been noted by [158, 159], if the ratio of the mother nucleus to the daughter nucleus is of the order 103, a production over ν-nucleosynthesis might be possible. Specifically for the light elements 7 Li and 11B the production in this explosive environment has shown to be an important part for the amount of these elements in our solar system. Within this work we utilized a rather phenomenological model for the shock passage and the expansion afterwards. Furthermore the neutrino luminosities have been assumed to be very high, especially for μ and τ flavor neutrinos, which are the dominating contributions for neutral-current processes.10 We used this high values to be able to compare with [2]. Due to this high values it is understandable that the dominating processes in ν -nucleosynthesis are neutral-current processes. However, charged-current processes also contribute and cannot be neglected. The main difference why in this astrophysical process neutrino-nucleus processes show prominent features, whereas in the case of the neutrino-driven wind the difference is barely noticeable, can be explained as follows. The argument is that – contrary to the neutrino- driven wind – in the ν -process the matter is already produced before the expansion starts. Thus the time window for neutrino interaction is longer, than in the neutrino-driven wind. In the neutrino-driven wind heavy elements are created by (n, p) reactions that mimic β + -decays, whereas in ν -nucleosynthesis the elements are created by spallation of the abundant nuclei. The abundance of the elements acting as a target for neutrino-nucleus interactions is in the outer shells substantially higher in comparison to the same elements in the neutrino-driven wind. Thus the relevant quantity of abundance times cross section will be generally higher, which allows converting more matter over spallation reactions in the ν -process. Globally we can say that the inclusion of neutrino-nucleus processes does not have influence on the nucleosynthesis of core-collapse supernovae. For an efficient production of some elements such as 7Li, 9Be, 11 B, but also 138La and 180Ta, neutrino-nucleus interactions are required. However this fact has already been mentioned in [2]. For r-process calcula- tions we can observe that the inclusion of neutrino-processes changes the final abundance. Thus, if the r-process would occur in neutrino-driven winds, at least the neutrino-nucleus interactions on 4He need to be incorporated. However, a full treatment will be always better. Within proton-rich winds on the other hand, the effect of neutrino-nucleus interac- tions on heavy element nucleosynthesis is very small. However, the fact that we now have a full set of rates, allows us to explore the impact of various astrophysical sites and their nucleosynthesis processes in a more sophisticated model, which includes the possible relevant neutrino-nucleus processes in these environments

Jules Romains, « poète de la sociologie »

Jules Romains, homme de lettres, auteur à succès dans la première moitié du xxe siècle, entretint des rapports ambigus avec la sociologie de son époque. Sa doctrine littéraire, l’unanimisme, lui paraissait rejoindre la démarche des sociologues. Cette attitude à l’égard de la sociologie prenait appui sur une tradition française d’émulation entre littérature et sciences sociales. Le manifeste de l’unanimisme qu’il écrivit dans sa jeunesse se présente sous la forme d’un long poème qui attira l’attention de Durkheim. Son œuvre majeure, Les Hommes de bonne volonté, suite romanesque en vingt-sept volumes, se caractérise par un esprit sociologique marqué. L’auteur décrit une foule de personnages insérés dans leurs rapports sociaux respectifs. Les effets de groupe jouent un rôle important dans cette création littéraire. Quant aux rapports entre Jules Romains et les sociologues durkheimiens, particulièrement Halbwachs, ils suggèrent une estime réciproque entre le monde de la littérature et celui de la sociologie.Jules Romains, man of letters, was a successful author in the first half of the xxth century. His relationship to sociology was rather ambiguous. According to him, “unanimism”, the literary doctrine he favored, converged with the sociological approach. His attitude toward sociology relied on a French tradition of competition between literature and social sciences. The manifesto of unanimism he wrote when he was young takes the form of a long poem which attracted Durkheim’s attention. A distinctive sociological outlook marks out his major work, Les Hommes de bonne volonté, a saga in twenty-seven volumes. The author describes numerous characters inserted in their respective social environment. Group dynamics play an important role in that literary fiction. As for the relations between Jules Romains and Durkheimian sociologists, especially Halbwachs, they point towards a mutual esteem between the world of literary and that of sociology

À propos du bicentenaire de Tocqueville

Dans les premières années du XXe siècle, un commentateur de l’œuvre tocquevillienne écrivait : « Malgré ses mérites, Tocqueville est presque abandonné » (Pierre-Marcel, 1910, p. 457). En l’année du bicentenaire de sa naissance, marquée par un foisonnement de colloques et de publications, c’est un Tocqueville consacré qui a fait place au Tocqueville oublié d’autrefois, avec tous les effets de mode que recèle ce renouveau d’intérêt. Loin d’être le résultat d’un consensus réalisé sur son œuvre, ..