Monumentul, realizat din marmură albă, este un obelisc deasupra căruia este fixată o cruce. Este inscripționat pe fețele laterale și pe față cu dedicații și cu nume de eroi. Monumentul este ...împrejmuit cu un gard realizat din fier și beton. Dimensiuni monument: 67 x 60 x 67.
Mențiuni despre monument: Stare proastă de conservare.
Inscripții pe monument: Inscripție în șimba sârbă, cu litere slavone: „VECINI SLAVA HEROIMI U RATU OD 1914-18 G. IZGHINULI SRBIMA SRP. SV. PETARNIȚA. SPOMENIC POLIJU 1926 G. VAȘI POȘTOVAOȚI KOIIVAS ISCRENO OPLACUIU” Pe verso: NUME DE EROI (22) În stânga: NUME DE EROI (28) În dreapta: NUME DE EROI ()
The monument, made of white marble, is an obelisk above which is fixed a cross. It is inscribed on the side faces and face with dedications and with names of heroes. The monument is fenced with a fence made of iron and concrete. Dimensions monument: 67 x 60 x 67.
Monumentul, realizat din marmură albă, este un obelisc deasupra căruia este fixată o cruce. Este inscripționat pe fețele laterale și pe față cu dedicații și cu nume de eroi. Monumentul este împrejmuit cu un gard realizat din fier și beton. Dimensiuni monument: 67 x 60 x 67.
Mențiuni despre monument: Stare proastă de conservare.
Inscripții pe monument: Inscripție în șimba sârbă, cu litere slavone: „VECINI SLAVA HEROIMI U RATU OD 1914-18 G. IZGHINULI SRBIMA SRP. SV. PETARNIȚA. SPOMENIC POLIJU 1926 G. VAȘI POȘTOVAOȚI KOIIVAS ISCRENO OPLACUIU” Pe verso: NUME DE EROI (22) În stânga: NUME DE EROI (28) În dreapta: NUME DE EROI ()
Lunar mare basalts provide a probe to study the magmatic and thermal evolution of the Moon. The Chang'e-5 (CE-5) mission returned samples from a young and hitherto unsampled mare terrain, providing ...fresh opportunities to understand lunar volcanic history. A detailed petrologic survey was conducted in this study on basalt fragments and glasses from the returned CE-5 soil samples. Relatively large-sized (100–400 μm) basaltic fragments were hand-picked and examined for texture, mineral assemblage and mineral chemistries. Basaltic fragments exhibit dominantly subophitic textures and are phenocryst-free, with low to intermediate-Ti (2.1–5.5 wt%) and low Mg# (Mg/(Mg + Fe) × 100, 19–47, with an average whole-rock Mg# of 33) consistent with olivine-melt equilibrium calculation (Mg# = 34). A range of highly evolved basaltic materials have been identified, in which abundant fayalitic olivine, symplectitic intergrowths, and Si + K-rich mesostasis co-exist were found resulting from late-stage silicate liquid immiscibility. Basaltic glass compositions largely overlap with basaltic fragment compositions suggesting they are locally derived. The CE-5 basalts have a relatively limited range of eruption temperatures of 1150–1230 °C. Based on their petrographic and geochemical characteristics, some CE-5 mare basalts are highly evolved and some of the resultant basaltic melt products underwent high crystallization. Thermodynamic modeling using MELTS suggests highly evolved basaltic magma was produced by a low-pressure and simple fractional crystallization under reduced conditions. This may have occurred at the surface in the inflated Em4/P58 flow with a thickness of ~50 m. The low degree of partial melting mantle source of the parental melts is the late-stage lunar magma ocean cumulates in a similar manner to some evolved low-Ti mare basalt meteorites, although the source of CE-5 basalts may have been slightly more Ti-rich.
•Young low to intermediate-Ti basaltic lavas of the Chang'e-5 site are highly evolved, with average Mg# = 33•Some basalts show silicate liquid immiscibility (SLI) textures underwent significant fractional crystallization•Relatively low-pressure (1 bar to 5 kbar) simple fractional crystallization under reduced conditions could produce the highly evolved magma•The crystallization of the CE-5 basalts leading to the compositions and the SLI textures are likely to have occurred in the 50 m thick Em4/P58 flow that CE-5 sampled
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NLZOH, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UILJ, UL, UM, UPCLJ, UPUK, ZAGLJ, ZRSKP
Precise crystallisation ages have been determined for a range of Apollo basalts from Pb-Pb isochrons generated using Secondary Ion Mass Spectrometry (SIMS) analyses of multiple accessory phases ...including K-feldspar, K-rich glass and phosphates. The samples analysed in this study include five Apollo 11 high-Ti basalts, one Apollo 14 high-Al basalt, seven Apollo 15 low-Ti basalts, and five Apollo 17 high-Ti basalts. Together with the samples analysed in two previous similar studies, Pb-Pb isochron ages have been determined for all of the major basaltic suites sampled during the Apollo missions. The accuracy of these ages has been assessed as part of a thorough review of existing age determinations for Apollo basalts, which reveals a good agreement with previous studies of the same samples, as well as with average ages that have been calculated for the emplacement of the different basaltic suites at the Apollo landing sites. Furthermore, the precision of the new age determinations helps to resolve distinctions between the ages of different basaltic suites in more detail than was previously possible. The proposed ages for the basaltic surface flows at the Apollo landing sites have been reviewed in light of these new sample ages. Finally, the data presented here have also been used to constrain the initial Pb isotopic compositions of the mare basalts, which indicate a significant degree of heterogeneity in the lunar mantle source regions, even among the basalts collected at individual landing sites.
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NLZOH, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UILJ, UL, UM, UPCLJ, UPUK, ZAGLJ, ZRSKP
Surface roughness of Titan's hydrocarbon seas Grima, Cyril; Mastrogiuseppe, Marco; Hayes, Alexander G. ...
Earth and planetary science letters,
09/2017, Volume:
474
Journal Article
Peer reviewed
Open access
We derive fields of solutions for the surface properties (roughness and permittivity) of the liquid hydrocarbon bodies Ligeia, Kraken and Punga Mare on Titan by applying the Radar Statistical ...Reconnaissance (RSR) technique to the Cassini RADAR observations in altimeter mode during the northern early summer. At the time of observation, Kraken and Ligeia were confined within root-mean-square heights of 1.5–2.5 mm (similar to wave heights of 6–10 mm), correlation lengths of 45–115 mm, and corresponding to effective slopes of 1.1–2.4°. The latter extends up to 3.6–4.9° if the rougher Punga is included. The lower bound of those ranges has to be considered if the composition of the seas is methane-dominant. These are the first measurements to simultaneously constrain both the vertical and horizontal roughness parameters of Titan's seas from the same observations. Our results are representative for the global properties of the sea-scaled portion of the studied tracks and suggest that quiet surfaces are a dominant trend over the seas during the northern early summer. Fields of rougher textures, if existent, might develop mainly over local patches and/or might not be sustained over significant periods of time.
•We estimate roughness for Titan's northern seas in the early summer.•Both vertical and horizontal roughness parameters are derived.•The surfaces are quiet and smooth, consistent with former radar observations.•Fields of wave activity might be transient or occur at local scales.
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UL, UM, UPCLJ, UPUK, ZRSKP
Recently a number of studies have identified small lunar geologic structures to be <100 Ma in age using standard remote sensing techniques. Here we present new crater size frequency distributions ...(CSFDs) and model ages using craters D > 10 m for five small target units: one irregular mare patch (IMP) in Mare Nubium and four regions located on lunar wrinkle ridges in Mare Humorum. For comparison we also date another IMP found in a recent study in Mare Tranquillitatis (Braden et al. ). Absolute model age (AMA) derivation corresponds to 46 ± 5 Ma and 22 ± 1 Ma for Nubium and Sosigenes IMP, respectively. We show that for IMPs and in nearby control mare regions, similar production‐like cumulative log–log SFD slopes of −3 are observed. In contrast, control mare regions in Mare Humorum exhibit shallower equilibrium slopes from −1.83 to −2. Three out of four wrinkle ridges appear to be in equilibrium but with crater lifetimes lower than on the corresponding maria. Low crater frequencies on one wrinkle ridge result in an age of 8.6 ± 1 Ma. This study region contains 80% fresh craters, which suggests that the crater population is still in production indicative of a recent resurfacing event.
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BFBNIB, FZAB, GIS, IJS, KILJ, NLZOH, NUK, OILJ, SAZU, SBCE, SBMB, UL, UM, UPUK
The Moon’s mare volcanism predominantly occurs within the Procellarum KREEP Terrane (PKT), which is widely thought to be associated with KREEP components within the lunar interior. The Chang’e-5 ...(CE-5) mission sampled a young (2 Ga) mare basalt Em4/P58 unit of northern Oceanus Procellarum. The geochemistry of the CE-5 mare basalt enables assessment of mantle source compositions which are essential to understand the thermo-chemical mechanism for prolonged volcanism during secular cooling of the Moon. Geochemical compositions of the CE-5 bulk soil, breccias, and basalt clasts from various depths within the drill core consistently display high concentrations of incompatible trace elements (ITE: ∼ 0.3 × high-K KREEP; ∼ 5 μg/g Th) with KREEP-like inter-element ratios, for example for La/Sm, Nb/Ta, and Zr/Y. Exotic impact ejecta, extensive magma differentiation (<70 % fractional crystallization) and significant assimilation of KREEP materials during magma transit and eruption cannot account for the ITE contents and ratios or radiogenic isotope compositions (e.g., εNdinitial of + 8 to + 9 and εHfinitial of + 40 to + 46) of the CE-5 basalts; instead, partial melting of their mantle source played a dominant role. The Chang’e-5 basalt is a chemically evolved low-Ti mare basalt (Mg# of ∼ 34) with enriched KREEP-like ITE compositions but high long-term time-integrated Sm/Nd and Lu/Hf ratio, which represents a hitherto unsampled type of mare basalt. It formed by melting of an augite-rich mantle source (late-stage magma ocean cumulates containing > 30–60 % augite, and little or no ilmenite), with a small amount of late-stage interstitial melt that resembles KREEP (∼1–1.5 modal %, equivalent to 0.2–0.3 μg/g Th). The voluminous mare basalts making up the Em4/P58 unit (>1500 km3) provide compelling evidence for large-scale, ITE enriched young mare magmatism within Oceanus Procellarum. In combination with remote sensing data and with the unique Th-rich Apollo 12 basalt fragment 12032,366–18 (impact ejecta likely from Oceanus Procellarum), this implies that significant portions of the FeO- and Th-rich mare regions of the western PKT may also have formed in a similar way.
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NLZOH, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UILJ, UL, UM, UPCLJ, UPUK, ZAGLJ, ZRSKP
Mare Kõiva, the chief researcher of the Estonian Literature Museum and head of the Department of Folklore who celebrated her 70th anniversary on February 26, is interviewed on such topics as the ...free-spirited spiritual and academic atmosphere of Estonia in the 1970s, the behind-the-scenes work of folklore researchers and their connections throughout the ages, and the continuity and innovations in folklore and its research.
Extraterrestrial materials collected by sample return exploration missions have advanced our understanding of planetary formation and evolution in a profound manner. This is achieved through ...sophisticated laboratory sample analyses with very high precision and accuracy that are difficult to obtained by orbital or surface landing/roving explorations. Moreover, the well-known geographical location and geological context of returned samples enable the sample measurements to be fully interpreted and mapped into the entire planetary context (in contrast to meteorites where the geological context is missing). Planetary scientists have been endeavoring to collect and returned samples from extraterrestrial bodies, despite the significant costs involved.
In December 2020, China's Chang'e-5 mission successfully landed in and returned lunar samples from the northeastern Oceanus Procellarum in the western lunar nearside maria. The mare basalt at the landing site has been dated to be ~1–2 Ga through crater population studies, much younger than any basalts in the present lunar sample collections and among the youngest maria on the global Moon (e.g., Hiesinger et al., 2011). The Chang'e-5 sample will provide an unprecedented opportunity to characterize the late-stage lunar volcanism.
To fully explore the scientific potential of the Chang'e-5 returned samples and assist the on-going sample analyses and interpretations, we present an in-depth investigation of the geology of the specific Chang'e-5 landing site and the nearby vicinity using high-resolution remote sensing data sets. We characterize the detailed geological context, topography, morphology, morphometry, chemical and mineralogical composition of the local landing area. These geological characterizations lead us to identify a sequence of four geological events, including mare volcanism, tectonism, impact cratering and ejecta deposition, that have potentially affected and been recorded in the returned samples. Compositional and geochronological measurements of the Chang'e-5 samples would reconstruct a detailed regional geological evolution model of the landing area. Furthermore, most of the inferred ages of these geological events lie in the age gap of the Apollo/Luna samples. Precise determination of these ages through radiogenic isotope analyses would be invaluable in narrowing down the uncertainties of the lunar cratering chronology function and improve our understanding of the geological history of the entire Moon.
•Detailed geological characteristics of the local landing area have been presented•Multiple identified geological events are potentially recorded in Chang'e-5 samples•The ages of these events would help calibrate lunar cratering chronology function
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NLZOH, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UILJ, UL, UM, UPCLJ, UPUK, ZAGLJ, ZRSKP
49.
Mastitis in mare: case report M.SH. Rhaymah; Q.T. Al-Obaidi; M.A. Hamad ...
Iraqi journal of veterinary sciences,
06/2018, Volume:
32, Issue:
1
Journal Article
Peer reviewed
Open access
Mastitis is rare in mares compared with cattle, a mare suffered from mastitis was referred to the Veterinary Teaching Hospital, College of Veterinary Medicine, University of Mosul for examination ...with a history of abortion before two months and gradually loss of body weight. Clinical examination revealed, a swollen left mammary gland, painful to palpate, there was mild degree of edema in the tissue surrounding the gland, fluid with clot expressed from the gland, body temperature was 37.4ºC and heart rate was 40/ minute. Fluid (mammary secretions), milk samples were collected under sterile condition and submitted to the laboratory for bacterial culture and identification test. The results of the culture and biochemical tests showed that the Staphylococcus spp was the etiological agent. This case was treated with systemic and local antibiotic therapy (Penicillin preparation).
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IZUM, KILJ, NUK, PILJ, PNG, SAZU, UL, UM, UPUK
Secondary ion mass spectrometry (SIMS) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in ...an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207Pb/206Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane (PKT) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded.
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BFBNIB, FZAB, GIS, IJS, KILJ, NLZOH, NUK, OILJ, SAZU, SBCE, SBMB, UL, UM, UPUK
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