Civil Law and Common Law: systemic differences or cultural contrast? Evaluating inconsistencies between the Italian, English and Welsh, Federal criminal procedures through the extensive media coverage of the Knox trial

The dissertation, which is entirely drafted in English, hinges on a comparative study of both the Italian and British legal system - including some reference to the American jurisdiction - from the point of view of the criminal procedure rules. Through the analysis of a specific case study, namely the trial for the murder of Meredith Kercher, the paper aims to highlight what the substantial differences between civil law and common law are and the extent to which these divergencies can impact criminal proceedings. Therefore, particular attention is placed on the media coverage that the case has had, both in Italy and in United Kingdom and the United States, and on how this has - perhaps only apparently - influenced the trial and public opinion

Toward a numerical deshaker for PFS

The Planetary Fourier Spectrometer (PFS) onboard Mars Express (MEx) is the instrument with the highest spectral resolution observing Mars from orbit since January 2004. It permits studying the atmospheric structure, major and minor compounds. The present time version of the calibration is limited by the effects of mechanical vibration, currently not corrected. We proposed here a new approach to correct for the vibrations based on semi-blind deconvolution of the measurements. This new approach shows that a correction can be done efficiently with 85% reduction of the artefacts, in a equivalent manner to the stacking of 10 spectra. Our strategy is not fully automatic due to the dependence on some regularisation parameters. It may be applied on the complete PFS dataset, correcting the large-scale perturbation due to microvibrations for each spectrum independently. This approach is validated on actual PFS data of Short Wavelength Channel (SWC), perturbed by microvibrations. A coherence check can be performed and also validate our approach. Unfortunately, the coherence check can be done only on the first 310 orbits of MEx only, until the laser line has been switch off. More generally, this work may apply to numerically "deshake" Fourier Transform Spectrometer (FTS), widely used in space experiments or in the laboratory.Comment: 18 pages, 8 figures, submitted to Planetary and Space Scienc

Characterization of dust activity on Mars from MY27 to MY32 by PFS-MEX observations

We present spatial and temporal distributions of dust on Mars from Ls = 331 in MY26 until Ls = 80 in MY33 retrieved from the measurements taken by the Planetary Fourier Spectrometer (PFS) aboard Mars Express. In agreement with previous observations, large dust opacity is observed mostly in the southern hemisphere spring/summer and particularly over regions of higher terrain and large topographic variation. We present a comparison with dust opacities obtained from Thermal Emission Spectrometer (TES) - Mars Global Surveyor (MGS) measurements. We found good consistency between observations of two instruments during overlapping interval (Ls = 331 in MY26 until Ls = 77 in MY27). We found a different behavior of the dust opacity with latitude in the various Martian years (inter-annual variations). A global dust storm occurred in MY28. We observe a different spatial distribution, a later occurrence and dissipation of the dust maximum activity in MY28 than in other Martian years. A possible precursor signal to the global dust storm in MY 28 is observed at Ls = 200 - 235 especially over west Hellas. Heavy dust loads alter atmospheric temperatures. Due to the absorption of solar radiation and emission of infrared radiation to space by dust vertically non-uniformly distributed, a strong heating of high atmospheric levels (40 - 50 km) and cooling below around 30 km are observed.Comment: in press in Icarus. 47 pages, 15 figure

Daily dust variation from the PFS MEx observations

We collected over 7 Martian years (MY) of data observed by the Planetary Fourier Spectrometer (PFS) to present a daily variation of dust content in the Martian atmosphere. We found three typical behaviors of dust opacities with LT (local time). The most peculiar variation was observed when global dust storms (MYs 28 and 34) or particularly strong regional storms (MY 29) occurred on Mars. Here, large dust opacities were measured at 10 LT (MY 34) and 11 LT (MY 28). Then, relatively small values of dust opacities were found in the evening (20 LT). The non-dusty season, particularly near northern summer solstice, was characterized by a deep minimum of the total dust opacity at late night/early morning, while small variations around the mean value were observed during daytime. The clear trend of dust was observed over both hemispheres during early morning. We noted elevated dust opacities in the second half of the year compared to the non-dusty season in all Martian years without global dust storms. The daily variation of three types of storms occurring in moderately dusty conditions was also investigated. Dust in A storms was present in the atmosphere at all LTs and was mostly confined to the southern hemisphere. The maximum of dust opacities in B storms was found at 15–17 LT, close to the South Pole. C storms were mainly constrained to southern latitudes and occurred from the late morning to midday

Response of dust on thermal emission spectra observed by Planetary Fourier Spectrometer (PFS) on-board Mars Express (MEX)

38-44The thermal emission spectra have provided many useful insights about the Martian atmosphere and surface. The interpretation of the thermal emission spectra can give us information about atmospheric temperature, pressure, mineralogy and presence of atmospheric constituents including their isotopes. In the present work, we have analysed the thermal emission data for dust storm season on Mars. The signature of dust in the thermal emission spectra for Martian Year (MY) 28 confirm the presence (Ls=280o and 300o) and the absence (Ls=240o and 320o) of the dust storm at latitude range 0o-10oS, 10o-20oS and 20o-30oS. We have compared our results with earlier mission data with thermal emission measurements made by Planetary Fourier Spectrometer (PFS) on-board Mars Express (MEX) between wave numbers 250-1400 cm-1. We have observed features at wave numbers 600-750 cm-1 and 900-1200 cm-1 due to absorptions by CO2 and dust respectively. We have obtained brightness temperatures from thermal emission spectra by inverting the Planck function. The maximum brightness temperature ~280o K was measured at Ls=240o when Mars received a large amount of solar radiation at perihelion. The minimum brightness temperature ~ 220o K was observed at Ls=320o in the absence of dust storm. In presence of dust storm, thermal emission spectra and brightness temperatures were reduced by factors of ~ 3.0 and ~1.3, respectively, between wave numbers 900-1200 cm-1 in comparison to that observed in absence of dust storm

Response of dust on thermal emission spectra observed by Planetary Fourier3 Spectrometer (PFS) on-board Mars Express (MEX)

The thermal emission spectra have provided many useful insights about the Martian atmosphere and surface. The interpretation of the thermal emission spectra can give us information about atmospheric temperature, pressure, mineralogy and presence of atmospheric constituents including their isotopes. In the present work, we have analysed the thermal emission data for dust storm season on Mars. The signature of dust in the thermal emission spectra for Martian Year (MY) 28 confirms presence (Ls=280o and 300o) and absence (Ls=240o and 320o) of the dust storm at latitude range 0o-10oS, 10o-20oS and 20o-30oS. We have compared our results with earlier mission data with thermal emission measurements made by Planetary Fourier Spectrometer (PFS) on-board Mars Express (MEX) between wave numbers 250-1400 cm-1. We have observed features at wave numbers 600-750 cm-1 and 900-1200 cm-1 due to absorptions by CO2 and dust respectively. We have obtained brightness temperatures from thermal emission spectra by inverting the Planck function. The maximum brightness temperature ~280 K is measured at Ls=240o when Mars received a large amount of solar radiation at perihelion. The minimum brightness temperature ~ 220o K is observed at Ls=320o in the absence of dust storm. In presence of dust storm thermal emission spectra and brightness  temperatures are reduced by factors of ~ 3.0 and ~1.3 respectively between wave numbers 900-1200 cm-1 in comparison to that observed in absence of dust storm

Modeling infrared thermal emissions on Mars during dust storm of MY28: PFS/MEX observation

We have analysed thermal emission spectra obtained from Planetary Fourier Spectrometer (PFS) onboard Mars Express (MEX) for Martian Year (MY) 28 in presence and absence of dust storm at low latitude. A radiative transfer model for dusty atmosphere of Mars is developed to estimate the thermal emission spectra at latitude range 0-10oS, 10-20oS and 20-30oS. These calculations are made at Ls=240o, 280o, 300o, and 320o between wave numbers 250-1400 cm-1. We have also retrieved brightness temperatures from thermal emission spectra by inverting the Planck function. The model reproduces the observed features at wave numbers 600-750 cm-1 and 900-1200 cm-1 due to absorptions by CO2 and dust respectively. In presence of dust storm thermal emission spectra and brightness temperature are reduced by a factor of ~ 2 between wave numbers 900-1200 cm-1. The altitude profiles of dust concentration are also estimated for different aerosol particles of sizes 0.2 to 3 micron. The best fit to the PFS measurements is obtained in presence of aerosol particle of size 0.2 micron

Melanocortin-4 Receptor and Lipocalin 2 Gene Variants in Spanish Children with Abdominal Obesity: Effects on BMI-SDS after a Lifestyle Intervention

Mutations leading to a reduced function of the melanocortin-4 receptor (MC4R) exert a major gene effect on extreme obesity. Recently it was shown that the bone derived hormone lipocalin 2 (LCN2) binds to the MC4R and activates a MC4R dependent anorexigenic pathway. We identified mutations in both genes and screened the effects of MC4R and LCN2 mutations on eating behavior and weight change after a lifestyle intervention. One hundred and twelve children (11.24 ± 2.6 years, BMI-SDS 2.91 ± 1.07) with abdominal obesity participated in a lifestyle intervention. MC4R and LCN2 coding regions were screened by Sanger sequencing. Eating behavior was assessed at baseline with the Children Eating Behavior Questionnaire (CEBQ). We detected three previously described non-synonymous MC4R variants (Glu42Lys, Thr150Ile, and Arg305Gln) and one non-synonymous polymorphism (Ile251Leu). Regarding LCN2, one known non-synonymous variant (Thr124Met) was detected. Eating behavior was described in carriers of the MC4R and LCN2 mutation and in non-carriers. MC4R and LCN2 mutations were detected in 2.42% and 0.84%, respectively, of Spanish children with abdominal obesity. A number of subjects with functional mutation variants in MC4R and LCN2 were able to achieve a reduction in BMI-SDS after a lifestyle intervention

New near-IR observations of mesospheric CO2 and H2O clouds on Mars

Carbon dioxide clouds, which are speculated by models on solar and extra-solar planets, have been recently observed near the equator of Mars. The most comprehensive identification of Martian CO2 ice clouds has been obtained by the near-IR imaging spectrometer OMEGA. CRISM, a similar instrument with a higher spatial resolution, cannot detect these clouds with the same method due to its shorter wavelength range. Here we present a new method to detect CO2 clouds using near-IR data based on the comparison of H2O and CO2 ice spectral properties. The spatial and seasonal distributions of 54 CRISM observations containing CO2 clouds are reported, in addition to 17 new OMEGA observations. CRISM CO2 clouds are characterized by grain size in the 0.5-2\mum range and optical depths lower than 0.3. The distributions of CO2 clouds inferred from OMEGA and CRISM are consistent with each other and match at first order the distribution of high altitude (>60km) clouds derived from previous studies. At second order, discrepancies are observed. We report the identification of H2O clouds extending up to 80 km altitude, which could explain part of these discrepancies: both CO2 and H2O clouds can exist at high, mesospheric altitudes. CRISM observations of afternoon CO2 clouds display morphologies resembling terrestrial cirrus, which generalizes a previous result to the whole equatorial clouds season. Finally, we show that morning OMEGA observations have been previously misinterpreted as evidence for cumuliform, and hence potentially convective, CO2 clouds.Comment: Vincendon, M., C. Pilorget, B. Gondet, S. Murchie, and J.-P. Bibring (2011), New near-IR observations of mesospheric CO2 and H2O clouds on Mars, J. Geophys. Res., 116, E00J0

Similarities and Differences of Global Dust Storms in MY 25, 28, and 34

To better understand the dust cycle on Mars during years with planet-encircling dust storms, we analyze the last three events that took place in Mars Year (MY) 25, MY 28, and MY 34. Global dust storms that occurred in MY 25 and MY 34 (June 2018) were taking place during equinox, while the MY 28 storm had an onset after perihelion. Before the expansion phase of the MY 25 and MY 34 storms, we find similar regions (northern rim of Hellas, Arabia Terra, and Utopia Planitia) where dust is present. Possible precursor dust storms over Hellas and the southern polar cap edges were observed during MY 28 as a component of background dust activity. These features are not found in equinoctial dust storms on this scale. Dust during the MY 25 and MY 34 storms encircled the entire planet by the similar season (Ls = 193°). The MY 34 storm is characterized by a shorter decay phase compared to the events in MY 25 and MY 28. Dust opacity is correlated with atmospheric temperatures at 0.5 mbar and nighttime surface temperatures, while daytime surface temperatures are anticorrelated with dust opacity