DIE EINSCHRÄNKUNG DER VERWENDUNG DER GLAGOLIZA AUF DER SYNODE VON ZADAR 1460

U radu se prikazuje odluka Zadarske sinode od 4. prosinca 1460. na kojoj je nadbiskup Mafej Vallaresso pokušao suzbiti upotrebu liturgije na crkvenoslavenskom jeziku hrvatske redakcije (lingua sclava). Sinodalni akti nisu danas sačuvani već je dostupan samo jedan dio sinodalnog kanona u dvije verzije. Originalnu verziju donosi Carlo F. Bianchi, dok je drugu, neznatno izmijenjenu, pribilježio Ivan Zanotti – Tanzlingher. Poslije interpretcije i konzultacije mjerodavnih vrela zaključuje se kako sinodalna odredba nije posve dokidala liturgijska slavlja na hrvatskom jeziku nego je samo na sinodi poduzet pothvat prostornog i vremenskog suzbijanja »glagoljaške liturgije«. Zadarski su nadbiskupi pokušavali tijekom XVI. stoljeća suzbiti glagoljicu na teritoriju nadbiskupije, ali – kako to pokazuju dostupna vrela – nisu imali znatnijeg uspjeha.In this short discussion author analyzes decisions of the Zadar synod that was held on 4th December 1460. At this diocese council archbishop Mafeo Vallaresso tried to suppress local custom of having the holy service in Church-Slavonic language. The acts from this synod unfortunately are not completely preserved but only one article De celebratione missarum et elebrandi divina official today is known in two versions. The first, and presumably original, version was brought to us by Carlo F. Bianchi, and the second one, just slightly modified, was noted by Ivan Zanotti-Tanzlingher. The both notes deliver basically the same information, and differ only regarding the beginning of this act. Archbishop Vallaresso deeply influenced ecclesiastical life of his diocese at his time: he renovated archbishopric palace, ordered a new bell for the cathedral’s bell tower, and restored organ in the cathedral of St. Anastasia. Still, even though he was a typical renaissance man, he did not care much about the specific local tradition of Zadar and deeply rooted Croatian language. Moreover, through the synod he tried to restrain Glagolitic liturgy only to two town churches: St. Donatus (Holy Trinity) and St. Mary the Great. Similarly, a century later, archbishops of the sixteenth century also tried to suppress Glagolitic script in Zadar, for example on the synods of 1566 and 1594. However, in spite of their endeavors, as it is clearly visible from the extant sources, they did not have much success, and Church Slavonic remained an integral part of local liturgy until the reform of the Second Vatican Council.In dieser kleinen Abhandlung wird die synodale Entscheidung über die Einschränkung der Liturgie in der kirchenslavischen Sprache (der kroatischen Redaktion) analysiert. Der venezianische Patrizier und der Erzbischof von Zadar, Maphäus Vallaresso (1450-1496) hat am 4. Dezember 1460 die Synode in Zadar einberufen; ihre Akten oder Entscheidungen sind nicht erhalten, nur ein kleiner Ausschnitt aus dem Kanon »De celebratione missarum et celebrandi divina officia«. Dieser ist heute in zwei Versionen zugänglich, die sich sprachlich nur geringfügig voneinander unterscheiden. Die Originalversion hat schon Carlo F. Bianchi veröffentlicht und die zweite hat Johannes Zanotti – Tanzlingher in seinem Werk Epitome synodorum dioecesis Iadrensis vermerkt. Die synodale Entscheidung versucht die Liturgie in der kirchenslavischen Sprache der kroatischen Redaktion für bestimmte Zeit nur auf zwei Kirchen in Zadar zu reduzieren: Die Kirche der Hl. Dreifaltigkeit (heute hl. Donat) und die Kirche der hl. Maria. Diese Entscheidung ließ sich nicht verwirklichen, da die Liturgie in lingua slava (d. h. in kroatischer Sprache) eine lange Tradition hat und in allen Pfarreien verbreitet war. Die Erzbischöfe von Zadar, Mutius Callinus (1555-1566) und auch Aloysius Molinus (1592-1595) haben diese Entscheidung auf den Synoden 1566 und 1594 noch einmal verbindlich erklärt; die Versuche sind gescheitert. Erzbischof Oktavian Garzzadoro (1623-1644), der aus gesundheitlichen Gründen Papst Urban VIII. um die Entbindung von den Pflichten bat, fügte seiner Begründung hinzu, dass er die Sprache der Gläubigen seines Bistums nicht versteht. Dies ist ein klarer Beweis dafür, dass in Zadar die Bevölkerung kroatisch gesprochen hat und die Liturgie bis zur Reform des II. Vatikanischen Konzils in der Landessprache gefeiert wurde

Colour and cloud structure in the atmospheres of the giant planets

For decades, the origin of colour-carrying compounds ('chromophores') in Jupiter and Saturn's atmospheres has remained elusive. Changes in colour are often associated with cyclical meteorological events ('upheavals') on Jupiter. Multiple datasets were obtained from the VLT/MUSE instrument between 2014 and 2018, each containing spatially-resolved spectra of Jupiter and Saturn between 0.48um and 0.93um. We describe the analysis of these datasets to characterise Jovian and Saturnian chromophores and to retrieve abundance profiles of aerosol and gaseous ammonia. Through limb-darkening analysis of Jupiter's NEB, we retrieved chromophore optical constants similar to the laboratory chromophore of (Carlson et al. [2016] Icarus 274, 106-115). These also provided a good fit to spectra of the Great Red Spot, but not to spectra of Jupiter's zones. We applied these chromophore optical constants to other regions of Jupiter, and found that red haze in the NTBs was initially associated with elevated aerosol abundances, but remained in the atmosphere long after upwelling had subsided. We verified previous findings of colour and haze structure changes relating to the shrinkage of the Great Red Spot, where we retrieved the altitude of the chromophore layer at the tropopause. We found no evidence of changes to the cloud structure of Oval BA to explain its fade in colour in 2018. An equivalent retrieval of chromophore optical constants from Saturn's NEB resulted in an absorption spectrum similar to the laboratory chromophore of (Noy et al. [1981] JGR:Oceans 86, 11985-11988), which we located just above Saturn's tropospheric haze. However, we found considerable variability in Saturn spectra that was not entirely consistent with a single chromophore compound. We believe that this work provides a significant contribution to our understanding of both colour and tropospheric aerosol structure on Jupiter and Saturn, and sheds light on the origin of spatial and temporal changes in the visible appearance of the two planets.</p

Colour and cloud structure in the atmospheres of the giant planets

For decades, the origin of colour-carrying compounds ('chromophores') in Jupiter and Saturn's atmospheres has remained elusive. Changes in colour are often associated with cyclical meteorological events ('upheavals') on Jupiter. Multiple datasets were obtained from the VLT/MUSE instrument between 2014 and 2018, each containing spatially-resolved spectra of Jupiter and Saturn between 0.48um and 0.93um. We describe the analysis of these datasets to characterise Jovian and Saturnian chromophores and to retrieve abundance profiles of aerosol and gaseous ammonia. Through limb-darkening analysis of Jupiter's NEB, we retrieved chromophore optical constants similar to the laboratory chromophore of (Carlson et al. [2016] Icarus 274, 106-115). These also provided a good fit to spectra of the Great Red Spot, but not to spectra of Jupiter's zones. We applied these chromophore optical constants to other regions of Jupiter, and found that red haze in the NTBs was initially associated with elevated aerosol abundances, but remained in the atmosphere long after upwelling had subsided. We verified previous findings of colour and haze structure changes relating to the shrinkage of the Great Red Spot, where we retrieved the altitude of the chromophore layer at the tropopause. We found no evidence of changes to the cloud structure of Oval BA to explain its fade in colour in 2018. An equivalent retrieval of chromophore optical constants from Saturn's NEB resulted in an absorption spectrum similar to the laboratory chromophore of (Noy et al. [1981] JGR:Oceans 86, 11985-11988), which we located just above Saturn's tropospheric haze. However, we found considerable variability in Saturn spectra that was not entirely consistent with a single chromophore compound. We believe that this work provides a significant contribution to our understanding of both colour and tropospheric aerosol structure on Jupiter and Saturn, and sheds light on the origin of spatial and temporal changes in the visible appearance of the two planets.</p

Colour and Tropospheric Cloud Structure of Jupiter from MUSE/VLT: Retrieving a Universal Chromophore

Recent work by Sromovsky et al. (2017, Icarus 291, 232-244) suggested that all red colour in Jupiter's atmosphere could be explained by a single colour-carrying compound, a so-called 'universal chromophore'. We tested this hypothesis on ground-based spectroscopic observations in the visible and near-infrared (480-930 nm) from the VLT/MUSE instrument between 2014 and 2018, retrieving a chromophore absorption spectrum directly from the North Equatorial Belt, and applying it to model spatial variations in colour, tropospheric cloud and haze structure on Jupiter. We found that we could model both the belts and the Great Red Spot of Jupiter using the same chromophore compound, but that this chromophore must exhibit a steeper blue-absorption gradient than the proposed chromophore of Carlson et al. (2016, Icarus 274, 106-115). We retrieved this chromophore to be located no deeper than 0.2+/-0.1 bars in the Great Red Spot and 0.7+/-0.1 bars elsewhere on Jupiter. However, we also identified some spectral variability between 510 nm and 540 nm that could not be accounted for by a universal chromophore. In addition, we retrieved a thick, global cloud layer at 1.4+/-0.3 bars that was relatively spatially invariant in altitude across Jupiter. We found that this cloud layer was best characterised by a real refractive index close to that of ammonia ice in the belts and the Great Red Spot, and poorly characterised by a real refractive index of 1.6 or greater. This may be the result of ammonia cloud at higher altitude obscuring a deeper cloud layer of unknown composition

Color and aerosol changes in Jupiter after a North Temperate Belt disturbance

International audienceThe banded appearance of Jupiter’s atmosphere shows significant changes over time, sometimes even transforming the reflectivity of a whole latitudinal band in a few weeks, and staying for years with an aspect different from the usual one. The origin of some of these disturbances may be associated with the creation and destruction of the chromophore species that provides Jovian clouds their reddish coloration. In this work, we have focused on the North Temperate Belt (NTB) disturbance detected during the second flyby of Juno mission (NASA) on October 2016, as a series of convective storms interacted with the fastest zonal jet on Jupiter at 24N over months and left a quiet belt characterized by an intense red coloration Sánchez-Lavega et al. (2017). In order to determine the corresponding changes in the upper clouds and hazes we have used images taken in 2016 and 2017 with the Hubble Space Telescope Wide Field Camera 3. Such images were acquired before and after the outbreak, showing an intense color change in a narrow latitude band. The images cover the wavelength range from 250 nm up to the methane absorption band at 890 nm, thus sensitive to a number of atmospheric levels from the lower stratosphere to the upper troposphere where the ammonia condensation cloud is expected to be located. Here we use the radiative transfer suite NEMESIS Irwin et al. (2008) to determine the vertical distribution and properties of the upper hazes that best match the observed dependence of reflectivity with wavelength and geometry. We use two models for the Jovian chromophore: (A) an extended layer whose imaginary refractive index is left as a free parameter; and (B) a concentrated chromophore as in Sromovsky et al. (2017) using the optical properties by Carlson et al. (2016). Both scenarios show an increase in the number of particles responsible for the blue absorption approximately by a factor of 2, and require only small changes in the rest of the atmospheric parameters. We find that, even though results provided by scenario B are also compatible with observations, the limb-darkening is better described by scenario A, where there is also an increase of the particle absorption at the shortest wavelengths. In this work, we also provide an extension of the expected imaginary refractive indices to wavelengths beyond those covered in previous laboratory works, which will be useful for future studies

1.5 Martian Years of Monitoring of the Martian Water Ice Clouds with TGO/ACS-MIR

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Seasonal, latitudinal, and longitudinal trends in night‐time ozone vertical structure on Mars from MAVEN/IUVS stellar occultations

International audienceStellar occultation measurements conducted by the MAVEN/IUVS instrument were able to make vertically-resolved measurements of ozone density in the middle atmosphere of Mars that offered good coverage with respect to latitude, longitude and local time. These measurements were used to identify systematic variations in the vertical structure of ozone with longitude that could be distinguished from general trends in the evolution of ozone with respect to season and latitude. A total of 583 individual nightside occultations between Martian years 32 and 36 were analysed, of which 224 were confirmed to have ozone, all found between Ls = 15 - 165°. Close to aphelion (Ls= 60 - 90°), peak ozone densities between 30 - 40 km altitude were observed to be within error of model predictions at all measured latitudes, but diverged from model predictions before and after this time. At low latitudes, seasonal changes were seen to have the greatest effect on the observed vertical structure of ozone, with detached ozone layer densities at altitudes above 30 km usually varying within approximately a factor of two along a given latitudinal band at a given time of year. Nonetheless, evidence of a persistent regional enhancement of ozone abundance was observed over equatorial latitudes during the aphelion season, spanning a longitude range of approximately 50 - 130° E longitude. Planetary waves were clearly observed at higher Southern latitudes during Southern winter, often resulting in order of magnitude variations in ozone density with longitude

1.5 Martian Years of Monitoring of the Martian Water Ice Clouds with TGO/ACS-MIR

International audienc

1.5 Martian Years of Monitoring of the Martian Water Ice Clouds with TGO/ACS-MIR

International audienc

A stringent upper limit of 20 pptv for methane on Mars and constraints on its dispersion outside Gale crater

International audienceReports on the detection of methane in the Martian atmosphere have motivated numerous studies aiming to confirm orexplain its presence on a planet where it might imply a biogenic or more likely a geophysical origin. Our intent is to complement and improve on the previously reported detection attempts by the Atmospheric Chemistry Suite(ACS) on board the ExoMars Trace Gas Orbiter (TGO). This latter study reported the results of a campaign that was a few months inlength, and was significantly hindered by a dusty period that impaired detection performances. We unveil 640 solar occultation measurements gathering 1.44 Martian years worth of data produced by the ACS. No methane was detected. Probing the clear northern summer season allowed us to reach 1-σupper limits of around 10pptv (20 pptv at 2-σ), with an annual mean of the smallest upper limits of 20 pptv. Upper limits are controlled by the amount ofdust in the atmosphere, which impairs detection performance around the equator and during the southern spring and summer seasons.Observations performed near Gale crater yielded 1-σupper limits of up to four times less than the background values measured bythe Curiosity rover during the corresponding seasons. Reconciliation of the absence of methane in the TGO spectra with the positive detections by Curiosity is even moredifficult in light of this annual survey performed by ACS. Stronger constraints are placed on the physical and chemical mechanismcapable of explaining why the mean of the best overall upper limits of ACS is ten times below the smallest methane abundancesmeasured by Curiosity