Synthese und Evaluierung makrozyklischer 68 Ga-MPI-Tracer auf Pyridaben-Basis

Herz-Kreislauf-Erkrankungen zählen weltweit zu den Hauptursachen, die zu frühzeitigem Tod führen. Pathophysiologisch liegt eine Gefäßwandverdickung durch Ablagerung arteriosklerotischer Plaques (Arteriosklerose) vor. Die molekulare Bildgebung mit den nuklearmedizinischen Verfahren SPECT und PET zielt darauf ab, minderperfundierte Myokardareale zu visualisieren, um den Krankheitsverlauf durch frühzeitige Therapie abschwächen zu können. Routinemäßig eingesetzt werden die SPECT-Perfusionstracer [99mTc]Sestamibi und [99mTc]Tetrofosmin. Zum Goldstandard für die Quantifizierung der Myokardperfusion werden allerdings die PET-Tracer [13N]NH3 und [15O]H2O, da eine absolute Bestimmung des Blutflusses in mL/min/g sowohl in der Ruhe als auch bei Belastung möglich ist. 2007 wurde [18F]Flurpiridaz als neuer Myokardtracer vorgestellt, dessen Bindung an den MC I sowohl in Ratten, Hasen, Primaten als auch in ersten klinischen Humanstudien eine selektive Myokardaufnahme zeigte. Um eine Verfügbarkeit des Radionuklids über einen Radionuklidgenerator gewährleisten zu können, sollten makrozyklische 68Ga-Myokard-Perfusionstracer auf Pyridaben-Basis synthetisiert und evaluiert werden. Die neue Tracer-Klasse setzte sich aus dem makrozyklischen Chelator, einem Linker und dem Insektizid Pyridaben als Targeting-Vektor zusammen. Struktur-Affinitätsbeziehungen konnten auf Grund von Variation des Linkers (Länge und Polarität), der Komplexladung (neutral und einfach positiv geladen), des Chelators (DOTA, NODAGA, DO2A) sowie durch einen Multivalenzansatz (Monomer und Dimer) aufgestellt werden. Insgesamt wurden 16 neue Verbindungen synthetisiert. Ihre 68Ga-Markierung wurde hinsichtlich pH-Wert, Temperatur, Vorläufermenge und Reaktionszeit optimiert. Die DOTA/NODAGA-Pyridaben-Derivate ließen sich mit niedrigen Substanzmengen (6 - 25 nmol) in 0,1 M HEPES-Puffer (pH 3,4) bei 95°C innerhalb 15 min mit Ausbeuten > 95 % markieren. Für die DO2A-basierenden Verbindungen bedurfte es einer mikrowellengestützen Markierung (300 W, 1 min, 150°C), um vergleichbare Ausbeuten zu erzielen. Die in vitro-Stabilitätstests aller Verbindungen erfolgten in EtOH, NaCl und humanem Serum. Es konnten keine Instabilitäten innerhalb 80 min bei 37°C festgestellt werden. Unter Verwendung der „shake flask“-Methode wurden die Lipophilien (log D = -1,90 – 1,91) anhand des Verteilungs-quotienten in Octanol/PBS-Puffer ermittelt. Die kalten Referenzsubstanzen wurden mit GaCl3 hergestellt und zur Bestimmung der IC50-Werte (34,1 µM – 1 µM) in vitro auf ihre Affinität zum MC I getestet. In vivo-Evaluierungen erfolgten mit den zwei potentesten Verbindungen [68Ga]VN160.MZ und [68Ga]VN167.MZ durch µ-PET-Aufnahmen (n=3) in gesunden Ratten über 60 min. Um die Organverteilung ermitteln zu können, wurden ex vivo-Biodistributionsstudien (n=3) vorgenommen. Sowohl die µ-PET-Untersuchungen als auch die Biodistributionsstudien zeigten, dass es bei [68Ga]VN167.MZ zwar zu einer Herzaufnahme kam, die jedoch eher perfusionsabhängig ist. Eine Retention des Tracers im Myokard konnte in geringem Umfang festgestellt werden.

Bio-inspired polymer-supported nitrido molybdenum(VI) complexes for ammonia synthesis − reactivity towards protons and electrons : EPR investigations on paramagnetic molybdenum(V) and copper(II) complexes

Die biologische Stickstofffixierung durch Molybdän-haltige Nitrogenasen sowie die Erforschung des zugrundeliegenden komplexen Mechanismus (N2-Aktivierung an Metall-Zentren, 6-fache Protonierung und Reduktion, N–N Bindungsspaltung unter Bildung von Ammoniak) ist von erheblichem Interesse. Insbesondere Molybdän-Komplexe wurden bereits erfolgreich als Modellverbindungen für die Untersuchung elementarer Einzelschritte der N2-Aktivierung eingesetzt. Durch die Verwendung von Triamidoamin-Liganden ist es Schrock et al. sogar gelungen mehrere Katalysezyklen zu durchlaufen und einen Mechanismus zu formulieren. Trotz der sterisch anspruchsvollen Substituenten in den Schrock-Komplexen ist die Umsatzrate dieses homogenen Katalysators, aufgrund Komplex-Deaktivierung infolge intermolekularer Reaktionen wie Dimerisierung und Disproportionierung, limitiert. In der vorliegenden Arbeit wurden einige dieser Herausforderungen angegangen und die aktiven Spezies auf einer Festphase immobilisiert, um intermolekulare Reaktionen durch räumliche Isolierung der Komplexe zu unterdrücken.rnEin Polymer-verankertes Analogon des Schrock Nitrido-Molybdän(VI)-Komplexes wurde auf einem neuen Reaktionsweg synthetisiert. Dieser beinhaltet nur einen einzigen Reaktionsschritt, um die funktionelle Gruppe „MoN“ einzuführen. Protonierung des immobilisierten Nitrido-Molybdän(VI)-Komplexes LMoVIN (L = Polymer-verankerter Triamidoamin-Ligand) mit 2,6-Lutidinium liefert den entsprechenden Imido-Molybdän(VI)-Komplex. Durch anschließende Ein-Elektronen-Reduktion mit Cobaltocen wird der Polymer-angebundene Imido-Molybdän(V)-Komplex erhalten, bewiesen durch EPR-Spektroskopie (g1,2,3 = 1.989, 1.929, 1.902). Durch die Immobilisierung und die effektive räumliche Separation der Reaktionszentren auf der Festphase werden bimolekulare Nebenreaktionen, die oft in homogenen Systemen auftreten, unterdrückt. Dies ermöglicht zum ersten Mal die Darstellung des Imido-Molybdän(V)-Intermediates des Schrock-Zyklus.rnEPR-Spektren des als Spin-Label eingeführten immobilisierten Nitrato-Kupfer(II)-Komplexes wurden unter verschiedenen Bedingungen (Lösungsmittel, Temperatur) aufgenommen, wobei sich eine starke Abhängigkeit zwischen der Zugänglichkeit und Reaktivität der immobilisierten Reaktionszentren und der Art des Lösungsmittels zeigte. Somit wurde die Reaktivität von LMoVIN gegenüber Protonen und Elektronen, welches zur Bildung von NH3 führt, unter Verwendung verschiedener Lösungsmittel untersucht und optimiert. Innerhalb des kugelförmigen Polymers verläuft die Protonierung und Reduktion von LMoVIN stufenweise. Aktive Zentren, die sich an der „äußeren Schale“ des Polymers befinden, sind gut zugänglich und reagieren schnell nach H+/e− Zugabe. Aktive Zentren im „Inneren des Polymers“ hingegen sind schlechter zugänglich und zeigen langsame diffusions-kontrollierte Reaktionen, wobei drei H+/e− Schritte gefolgt von einer Ligandenaustausch-Reaktion erforderlich sind, um NH3 freizusetzen: LMoVIN  LMoVNH  LMoIVNH2  LMoIIINH3 und anschließender Ligandenaustausch führt zur Freisetzung von NH3.rnIn einem weiteren Projekt wurde der Bis(ddpd)-Kupfer(II)-Komplex EPR-spektroskopisch in Hinblick auf Jahn−Teller-Verzerrung und -Dynamik untersucht. Dabei wurden die EPR-Spektren bei variabler Temperatur (70−293 K) aufgenommen. Im Festkörperspektrum bei T < 100 K erscheint der Kupfer(II)-Komplex als gestreckter Oktaeder, wohingegen das EPR-Spektrum bei höheren Temperaturen g-Werte aufzeigt, die einer pseudo-gestauchten oktaedrischen Kupfer(II)-Spezies zuzuordnen sind. Diese Tatsache wird einem intramolekularen dynamischen Jahn−Teller Phänomen zugeschrieben, welcher bei 100 K eingefroren wird.

Windkanalstudien zum Graupelwachstum und Bestimmung von Retentionskoeffizienten verschiedener Spurengase während der Bereifung

Am vertikalen Windkanal der Johannes Gutenberg-Universität Mainz wurden physikalische und chemische Bereifungsexperimente durchgeführt. Dabei lagen die Umgebungstemperaturen bei allen Experimenten zwischen etwa -15 und -5°C und der Flüssigwassergehalt erstreckte sich von 0,9 bis etwa 1,6g/m³, typische Bedingungen für Mischphasenwolken in denen Bereifung stattfindet. Oberflächentemperaturmessungen an wachsenden hängenden Graupelpartikeln zeigten, dass während der Experimente trockene Wachstumsbedingungen herrschten.rnZunächst wurde das Graupelwachstum an in einer laminaren Strömung frei schwebenden Eispartikeln mit Anfangsradien zwischen 290 und 380µm, die mit flüssigen unterkühlten Wolkentröpfchen bereift wurden, studiert. Ziel war es, den Kollektionskern aus der Massenzunahme des bereiften Eispartikels und dem mittleren Flüssigwassergehalt während des Wachstumsexperimentes zu bestimmen. Die ermittelten Werte für die Kollektionskerne der bereiften Eispartikel erstreckten sich von 0,9 bis 2,3cm³/s in Abhängigkeit ihres Kollektorimpulses (Masse * Fallgeschwindigkeit des bereifenden Graupels), der zwischen 0,04 und 0,10gcm/s lag. Bei den Experimenten zeigte sich, dass die hier gemessenen Kollektionskerne höher waren im Vergleich mit Kollektionskernen flüssiger Tropfen untereinander. Aus den aktuellen Ergebnissen dieser Arbeit und der vorhandenen Literaturwerte wurde ein empirischer Faktor entwickelt, der von dem Wolkentröpfchenradius abhängig ist und diesen Unterschied beschreibt. Für die untersuchten Größenbereiche von Kollektorpartikel und flüssigen Tröpfchen können die korrigierten Kollektionskernwerte in Wolkenmodelle für die entsprechenden Größen eingebunden werden.rnBei den chemischen Experimenten zu dieser Arbeit wurde die Spurenstoffaufnahme verschiedener atmosphärischer Spurengase (HNO3, HCl, H2O2, NH3 und SO2) während der Bereifung untersucht. Diese Experimente mussten aus technischen Gründen mit hängenden Eispartikeln, dendritischen Eiskristallen und Schneeflocken, bereift mit flüssigen Wolkenlösungströpfchen, durchgeführt werden.rnDie Konzentrationen der Lösung, aus der die Wolkentröpfchen mit Hilfe von Zweistoffdüsen erzeugt wurden, lagen zwischen 1 und 120mg/l. Für die Experimente mit Ammoniak und Schwefeldioxid wurden Konzentrationen zwischen 1 und 22mg/l verwendet. Das Schmelzwasser der bereiften hängenden Graupel und Schneeflocken wurden ionenchromatographisch analysiert und zusammen mit der bekannten Konzentration der bereifenden Wolkentröpfchen konnte der Retentionskoeffizient für jeden Spurenstoff bestimmt werden. Er gibt die Menge an Spurenstoff an, die bei der Phasenumwandlung von flüssig zu fest in die Eisphase übergeht. Salpetersäure und Salzsäure waren nahezu vollständig retiniert (Mittelwerte der gesamten Experimente entsprechend 99±8% und 100±9%). Für Wasserstoffperoxid wurde ein mittlerer Retentionskoeffizient von 65±17% bestimmt. rnDer mittlere Retentionskoeffizient von Ammoniak ergab sich unabhängig vom Flüssigwassergehalt zu 92±21%, während sich für Schwefeldioxid 53±10% für niedrige und 29±7% für hohe Flüssigphasenkonzentrationen ergaben. Bei einigen der untersuchten Spurenstoffe wurde eine Temperaturabhängigkeit beobachtet und wenn möglich durch Parametrisierungen beschrieben.rn

Catalizzatori per la reazione di Water Gas Shift a media ed alta temperatura

L’H2 è un vettore energetico di elevato interesse, utilizzato nell’industria chimica per la produzione di NH3 e CH3OH, oltre che per le reazioni di idrogenazione ed HDS. Un importante processo nella produzione di H2 è la reazione di Water Gas Shift (WGS), usata nel trattamento delle correnti uscenti dal reattore di Steam Reforming (SR) del metano: CO + H2O  CO2 + H2 ∆H0298K = -41,2 KJ/mol. Sulla base di precedenti lavori, sono stati sviluppati nuovi catalizzatori per la reazione WGS ad alta temperatura (HTS), alternativi ai tradizionali sistemi a base di Fe/Cr, in considerazione dei vincoli economici (elevati valori del rapporto vapore/gas secco o S/DG) ed ambientali (formazione di CrVI) di questi sistemi. Partendo da sistemi Cu/Zn/Al con un basso contenuto di rame, ottenuti da precursori tipo idrotalcite (HT), stato studiato l’effetto dell’aggiunta di piccole quantità di alcuni promotori sull’attività e stabilità dei catalizzatori ottenuti, osservando un effetto positivo sulle caratteristiche fisiche, come l’aumento dell’area superficiale e della dispersione della fase attiva. I campioni contenenti i promotori erano inoltre caratterizzati da una maggiore stabilità termica e, in alcuni casi, da un’attività catalitica superiore a quella del catalizzatore di riferimento privo di promotori. L’aggiunta di piccole quantità di alcali alla formulazione con la migliore attività portava ad un ulteriore aumento di attività e di stabilità, attribuibile ad una minore formazione di coke sulla superficie. I sistemi più interessanti potevano operare anche a bassi valori del rapporto S/DG, interessanti dal punto di vista industriale. Lo studio dell’adsorbimento di CO mediante FT-IR ha permesso di ipotizzare la possibile natura della fase attiva nei sistemi. Infine, lo studio è stato esteso a sistemi per la reazione di WGS a media temperatura (MTS), osservando anche in questo caso un positivo effetto legato all’aggiunta di promotori, con un aumento dell’attività catalitica e della stabilità con il tempo di reazione.

Comparison of Model Chemistry and Density Functional Theory Thermochemical Predictions with Experiment for Formation of Ionic Clusters of the Ammonium Cation Complexed with Water and Ammonia; Atmospheric Implications

The G2, G3, CBS-QB3, and CBS-APNO model chemistry methods and the B3LYP, B3P86, mPW1PW, and PBE1PBE density functional theory (DFT) methods have been used to calculate ΔH° and ΔG° values for ionic clusters of the ammonium ion complexed with water and ammonia. Results for the clusters NH4+(NH3)n and NH4+(H2O)n, where n = 1−4, are reported in this paper and compared against experimental values. Agreement with the experimental values for ΔH° and ΔG° for formation of NH4+(NH3)n clusters is excellent. Comparison between experiment and theory for formation of the NH4+(H2O)n clusters is quite good considering the uncertainty in the experimental values. The four DFT methods yield excellent agreement with experiment and the model chemistry methods when the aug-cc-pVTZ basis set is used for energetic calculations and the 6-31G* basis set is used for geometries and frequencies. On the basis of these results, we predict that all ions in the lower troposphere will be saturated with at least one complete first hydration shell of water molecules.

Hydration of the Sulfuric Acid−Methylamine Complex and Implications for Aerosol Formation

The binary H2SO4−H2O nucleation is one of the most important pathways by which aerosols form in the atmosphere, and the presence of ternary species like amines increases aerosol formation rates. In this study, we focus on the hydration of a ternary system of sulfuric acid (H2SO4), methylamine (NH2CH3), and up to six waters to evaluate its implications for aerosol formation. By combining molecular dynamics (MD) sampling with high-level ab initio calculations, we determine the thermodynamics of forming H2SO4(NH2CH3)(H2O)n, where n = 0−6. Because it is a strong acid−base system, H2SO4−NH2CH3 quickly forms a tightly bound HSO4−−NH3CH3+ complex that condenses water more readily than H2SO4 alone. The electronic binding energy of H2SO4−NH2CH3 is −21.8 kcal mol−1 compared with −16.8 kcal mol−1 for H2SO4−NH3 and −12.8 kcal mol−1 for H2SO4−H2O. Adding one to two water molecules to the H2SO4−NH2CH3 complex is more favorable than adding to H2SO4 alone, yet there is no systematic difference for n ≥ 3. However, the average number of water molecules around H2SO4−NH2CH3 is consistently higher than that of H2SO4, and it is fairly independent of temperature and relative humidity.

Hydration of the Sulfuric Acid-Methylamine Complex and Implications for Aerosol Formation

The binary H2SO4-H2O nucleation is one of the most important pathways by which aerosols form in the atmosphere, and the presence of ternary species like amines increases aerosol formation rates. In this study, we focus on the hydration of a ternary system of sulfuric acid (H2SO4), methylamine (NH2CH3), and up to six waters to evaluate its implications for aerosol formation. By combining molecular dynamics (MD) sampling with high-level ab initio calculations, we determine the thermodynamics of forming H2SO4(NH2CH3)(H2O)n, where n = 0-6. Because it is a strong acid-base system, H2SO4-NH2CH3 quickly forms a tightly bound HSO4(-)-NH3CH3(+) complex that condenses water more readily than H2SO4 alone. The electronic binding energy of H2SO4-NH2CH3 is -21.8 kcal mol(-1) compared with -16.8 kcal mol(-1) for H2SO4-NH3 and -12.8 kcal mol(-1) for H2SO4-H2O. Adding one to two water molecules to the H2SO4-NH2CH3 complex is more favorable than adding to H2SO4 alone, yet there is no systematic difference for n ≥ 3. However, the average number of water molecules around H2SO4-NH2CH3 is consistently higher than that of H2SO4, and it is fairly independent of temperature and relative humidity.

Parameter identification of a copper-zeolite SCR catalyst model using reactor data

The selective catalytic reduction system is a well established technology for NOx emissions control in diesel engines. A one dimensional, single channel selective catalytic reduction (SCR) model was previously developed using Oak Ridge National Laboratory (ORNL) generated reactor data for an iron-zeolite catalyst system. Calibration of this model to fit the experimental reactor data collected at ORNL for a copper-zeolite SCR catalyst is presented. Initially a test protocol was developed in order to investigate the different phenomena responsible for the SCR system response. A SCR model with two distinct types of storage sites was used. The calibration process was started with storage capacity calculations for the catalyst sample. Then the chemical kinetics occurring at each segment of the protocol was investigated. The reactions included in this model were adsorption, desorption, standard SCR, fast SCR, slow SCR, NH3 Oxidation, NO oxidation and N2O formation. The reaction rates were identified for each temperature using a time domain optimization approach. Assuming an Arrhenius form of the reaction rates, activation energies and pre-exponential parameters were fit to the reaction rates. The results indicate that the Arrhenius form is appropriate and the reaction scheme used allows the model to fit to the experimental data and also for use in real world engine studies.

PROPERTIES AND STRUCTURES OF Li-N BASED HYDROGEN STORAGE MATERIALS

Traditional transportation fuel, petroleum, is limited and nonrenewable, and it also causes pollutions. Hydrogen is considered one of the best alternative fuels for transportation. The key issue for using hydrogen as fuel for transportation is hydrogen storage. Lithium nitride (Li3N) is an important material which can be used for hydrogen storage. The decompositions of lithium amide (LiNH2) and lithium imide (Li2NH) are important steps for hydrogen storage in Li3N. The effect of anions (e.g. Cl-) on the decomposition of LiNH2 has never been studied. Li3N can react with LiBr to form lithium nitride bromide Li13N4Br which has been proposed as solid electrolyte for batteries. The decompositions of LiNH2 and Li2NH with and without promoter were investigated by using temperature programmed decomposition (TPD) and X-ray diffraction (XRD) techniques. It was found that the decomposition of LiNH2 produced Li2NH and NH3 via two steps: LiNH2 into a stable intermediate species (Li1.5NH1.5) and then into Li2NH. The decomposition of Li2NH produced Li, N2 and H2 via two steps: Li2NH into an intermediate species --- Li4NH and then into Li. The kinetic analysis of Li2NH decomposition showed that the activation energies are 533.6 kJ/mol for the first step and 754.2 kJ/mol for the second step. Furthermore, XRD demonstrated that the Li4NH, which was generated in the decomposition of Li2NH, formed a solid solution with Li2NH. In the solid solution, Li4NH possesses a similar cubic structure as Li2NH. The lattice parameter of the cubic Li4NH is 0.5033nm. The decompositions of LiNH2 and Li2NH can be promoted by chloride ion (Cl-). The introduction of Cl- into LiNH2 resulted in the generation of a new NH3 peak at low temperature of 250 °C besides the original NH3 peak at 330 °C in TPD profiles. Furthermore, Cl- can decrease the decomposition temperature of Li2NH by about 110 °C. The degradation of Li3N was systematically investigated with techniques of XRD, Fourier transform infrared (FT-IR) spectroscopy, and UV-visible spectroscopy. It was found that O2 could not affect Li3N at room temperature. However, H2O in air can cause the degradation of Li3N due to the reaction between H2O and Li3N to LiOH. The produced LiOH can further react with CO2 in air to Li2CO3 at room temperature. Furthermore, it was revealed that Alfa-Li3N is more stable in air than Beta-Li3N. The chemical stability of Li13N4Br in air has been investigated by XRD, TPD-MS, and UV-vis absorption as a function of time. The aging process finally leads to the degradation of the Li13N4Br into Li2CO3, lithium bromite (LiBrO2) and the release of gaseous NH3. The reaction order n = 2.43 is the best fitting for the Li13N4Br degradation in air reaction. Li13N4Br energy gap was calculated to be 2.61 eV.

Two-Dimensional Supramolecular Electron Spin Arrays

A bottom-up approach is introduced to fabricate two-dimensional self-assembled layers of molecular spin-systems containing Mn and Fe ions arranged in a chessboard lattice. We demonstrate that the Mn and Fe spin states can be reversibly operated by their selective response to coordination/decoordination of volatile ligands like ammonia (NH3).

From planetesimals to planets: volatile molecules

Context. Solar and extrasolar planets are the subject of numerous studies aiming to determine their chemical composition and internal structure. In the case of extrasolar planets, the composition is important as it partly governs their potential habitability. Moreover, observational determination of chemical composition of planetary atmospheres are becoming available, especially for transiting planets. Aims. The present works aims at determining the chemical composition of planets formed in stellar systems of solar chemical composition. The main objective of this work is to provide valuable theoretical data for models of planet formation and evolution, and future interpretation of chemical composition of solar and extrasolar planets. Methods. We have developed a model that computes the composition of ices in planets in different stellar systems with the use of models of ice and planetary formation. Results. We provide the chemical composition, ice/rock mass ratio and C:O molar ratio for planets in stellar systems of solar chemical composition. From an initial homogeneous composition of the nebula, we produce a wide variety of planetary chemical compositions as a function of the mass of the disk and distance to the star. The volatile species incorporated in planets are mainly composed of H2O, CO, CO2, CH3OH, and NH3. Icy or ocean planets have systematically higher values of molecular abundances compared to giant and rocky planets. Gas giant planets are depleted in highly volatile molecules such as CH4, CO, and N2 compared to icy or ocean planets. The ice/rock mass ratio in icy or ocean and gas giant planets is, respectively, equal at maximum to 1.01 ± 0.33 and 0.8 ± 0.5, and is different from the usual assumptions made in planet formation models, which suggested this ratio to be 2–3. The C:O molar ratio in the atmosphere of gas giant planets is depleted by at least 30% compared to solar value.

From stellar nebula to planetesimals

Context. Solar and extrasolar comets and extrasolar planets are the subject of numerous studies in order to determine their chemical composition and internal structure. In the case of planetesimals, their compositions are important as they govern in part the composition of future planets. Aims. The present works aims at determining the chemical composition of icy planetesimals, believed to be similar to present day comets, formed in stellar systems of solar chemical composition. The main objective of this work is to provide valuable theoretical data on chemical composition for models of planetesimals and comets, and models of planet formation and evolution. Methods. We have developed a model that calculates the composition of ices formed during the cooling of the stellar nebula. Coupled with a model of refractory element formation, it allows us to determine the chemical composition and mass ratio of ices to rocks in icy planetesimals throughout in the protoplanetary disc. Results. We provide relationships for ice line positions (for different volatile species) in the disc, and chemical compositions and mass ratios of ice relative to rock for icy planetesimals in stellar systems of solar chemical composition. From an initial homogeneous composition of the nebula, a wide variety of chemical compositions of planetesimals were produced as a function of the mass of the disc and distance to the star. Ices incorporated in planetesimals are mainly composed of H2O, CO, CO2, CH3OH, and NH3. The ice/rock mass ratio is equal to 1 ± 0.5 in icy planetesimals following assumptions. This last value is in good agreement with observations of solar system comets, but remains lower than usual assumptions made in planet formation models, taking this ratio to be of 2–3.

Metamagnetic Copper(II) Diphosphonates with Layered Structures

Compounds [NH3(CH2)4NH3]Cu3(hedp)2·2H2O (1) and [NH3(CH2)3NH3]Cu3(hedp)2·3.5H2O (2), where hedp represents 1-hydroxyethylidenediphosphonate, exhibit two-dimensional structures closely related to each other. The anionic layers with composition {Cu3(hedp)2}n2n- contain four- and eight-membered rings assembled from vertex-sharing {CuO4} units and {CPO3} tetrahedra. The protonated diamines and lattice water fill the interlayer spaces. Crystal data for 2:  space group P1̄, a = 8.0315(4), b = 11.3713(6), c = 13.3117(7) Å, α = 97.122(1), β = 103.187(1), γ = 108.668(1)°, V = 1095.5(1) Å3, Z = 2. Magnetic properties of the two compounds have been investigated. Both show typical metamagnetic behaviors at low temperature. The critical field at which the antiferromagnetic ground-state switches to a ferrimagnetic state is ∼48 Oe for 1 and 185 Oe for 2 at about 2 K.

Gas composition of the main volatile elements in protoplanetary discs and its implication for planet formation

Context. Direct observations of gaseous exoplanets reveal that their gas envelope has a higher C/O ratio than that of the host star (e.g., Wasp 12-b). This has been explained by considering that the gas phase of the disc could be inhomogeneous, exceeding the stellar C/O ratio in regions where these planets formed; but few studies have considered the drift of the gas and planet migration. Aims. We aim to derive the gas composition in planets through planet formation to evaluate if the formation of giant planets with an enriched C/O ratio is possible. The study focusses on the effects of different processes on the C/O ratio, such as the disc evolution, the drift of gas, and planet migration. Methods. We used our previous models for computing the chemical composition, together with a planet formation model, to which we added the composition and drift of the gas phase of the disc, which is composed of the main volatile species H2O, CO, CO2, NH3, N2, CH3OH, CH4, and H2S, H2 and He. The study focusses on the region where ice lines are present and influence the C/O ratio of the planets. Results. Modelling shows that the condensation of volatile species as a function of radial distance allows for C/O enrichment in specific parts of the protoplanetary disc of up to four times the solar value. This leads to the formation of planets that can be enriched in C/O in their envelope up to three times the solar value. Planet migration, gas phase evolution and disc irradiation enables the evolution of the initial C/O ratio that decreases in the outer part of the disc and increases in the inner part of the disc. The total C/O ratio of the planets is governed by the contribution of ices accreted, suggesting that high C/O ratios measured in planetary atmospheres are indicative of a lack of exchange of material between the core of a planet and its envelope or an observational bias. It also suggests that the observed C/O ratio is not representative of the total C/O ratio of the planet.

Chemistry of hot waters sampled from basaltic basement at DSDP Hole 83-504B

Seawater that has been altered by reaction with basaltic basement has been sampled from Deep Sea Drilling Project Hole 504B, located on 5.9-m.y.-old crust on the southern flank of the Costa Rica Rift. Fourteen water samples have been collected on Legs 69, 70, and 83, both before and after renewed drilling on the latter two legs, at temperatures from 69 to 133°C and pressures from 390 to 425 bars. The water sampled prior to renewed drilling on Leg 83 had occupied the hole for nearly 2 yr. since it was last flushed with surface seawater at the end of Leg 70. Despite some contamination by seawater during sampling, the composition of two of these waters has been determined by using nitrate as a tag for the contaminant. Both the 80 and 115°C waters have seawater chlorinity, but have lost considerable Mg, Na, K, sulfate, and 02, and have gained Ca, alkalinity, Si, NH3 and H2S. The loss of sulfate is due to anhydrite precipitation, as indicated by the d34S value of the remaining dissolved sulfate. The 87Sr/86Sr ratio has been lowered to 0.7086 for the 80°C water and 0.7078 for the 115°C water, whereas the Sr concentration is nearly unchanged. The changes in major element composition relative to seawater are also larger for the 115°C water, indicating that the basement formation water at this site probably varies in composition with depth. Based on their direction relative to seawater, the compositional changes for the 80 and 115°C waters do not complement the changes inferred for the altered rocks from Hole 504B, suggesting that the bulk composition of the altered rocks, like their mineralogy, is largely unrelated to the present thermal and alteration regime in the hole. The exact nature of the reacted seawaters cannot be determined yet, however. During its 2 yr. residence in the hole, the surface seawater remaining at the end of Leg 70 would have reacted with the wall rocks and exchanged with their interstitial formation waters by diffusion and possibly convection. How far these processes have proceeded is not yet certain, although calculations suggest that diffusion alone could have largely exchanged the surface seawater for interstitial water. The d18O of the samples is indistinguishable from seawater, however, and the d14C of the 80°C sample is similar to that of ocean bottom water. Although the interpretation of these species is ambiguous, that of tritium should not be. Tritium analyses, which are in progress, should clarify the nature of the reacted seawaters obtained from the hole.