Oxygen, hydrogen, and carbon isotopic compositions in deep sea cherts, porcellanites, and coexisting carbonates from DSDP Legs 2, 3, 6, 7, 11, 14, 16, 17, and 20

Seventy four samples of DSDP recovered cherts of Jurassic to Miocene age from varying locations, and 27 samples of on-land exposed cherts were analyzed for the isotopic composition of their oxygen and hydrogen. These studies were accompanied by mineralogical analyses and some isotopic analyses of the coexisting carbonates. d18O of chert ranges between 27 and 39%. relative to SMOW, d18O of porcellanite - between 30 and 42%. The consistent enrichment of opal-CT in porcellanites in 18O with respect to coexisting microcrystalline quartz in chert is probably a reflection of a different temperature (depth) of diagenesis of the two phases. d18O of deep sea cherts generally decrease with increasing age, indicating an overall cpoling of the ocean bottom during the last 150 m.y. A comparison of this trend with that recorded by benthonic foraminifera (Douglas and Savin, 1975; http://www.deepseadrilling.org/32/volume/dsdp32_15.pdf) indicates the possibility of d18O in deep sea cherts not being frozen in until several tens of millions of years after deposition. Cherts of any Age show a spread of d18O values, increasing diagenesis being reflected in a lowering of d18O. Drusy quartz has the lowest d18O values. On-land exposed cherts are consistently depleted in 18O in comparison to their deep sea time equivalent cherts. Water extracted from deep sea cherts ranges between 0.5 and 1.4 wt %. dD of this water ranges between -78 and -95%. and is not a function of d18O of the cherts (or the temperature of their formation).

5a-Butyl-1,3,8,10-tetra-chloro-7,13-bis-(4-nitro-benzo-yl)-5a,6a,12a,12b-tetra-hydro-7H,13H-thieno[2,3-b:4,5-b']bis-(1,4-benzoxazine)

The title compound, C(34)H(24)Cl(4)N(4)O(8)S, is a linear penta-cyclic system formed of two substituted benzoxazinyl groups fused to 2-n-butyl-tetra-hydro-thio-phene. The oxazine ring, which is fused to the n-butyl-substituted side of the thio-phene ring, is in a boat conformation. The other fused oxazine ring and the tetra-hydro-thiene ring are each in an envelope conformation. The bridgehead C atom alpha to both the S and N atoms forms the flap of each envelope. This results in a twist of the penta-cyclic system such that the dihedral angle between the terminal dichloro-benzene rings is 82.92 (8)°. In the crystal, inversion-related mol-ecules form a weakly hydrogen-bonded dimer, with two C-H⋯O inter-actions between an H atom on the oxazine ring and an amide O atom. Additionally, C-H⋯O inter-actions occur between an H atom on a screw-related nitro-benzene ring and an O atom on the nitro-benzene ring of one mol-ecule. One of the Cl atoms and the butyl group are disordered over two sets of sites with occupancy ratios of 0.94 (2):0.06 (2) and 0.624 (4):0.376 (4), respectively.

Synthesis and structural characterization of organolanthanide complexes with 1,2-dicarba-closo-dodecaborane-1,2-dichalcogenolate ligands

Reactions of anhydrous LnCl(3) (Ln = Nd, Gd, Dy, Er, Yb) with 2 equiv of LiCp' in THF afford the lanthanocene complexes Of CP'(2)Ln(mu-Cl)(2)Li(THF)(2) (CP' = eta(5)-t-BuC5H4, Ln = Nd (1), Gd (2), Dy (3), Er (4), Yb (5); Cp'= 1,3-eta(5)-t-Bu2C5H3, Ln = Nd (6), Gd (7), Dy (8), Er (9), Yb (10)). The molecular structures of 7 and 8 were characterized by X-ray crystallographic analysis. In these complexes, two Cp' ring centroids and two it-bridging chloride atoms around the lanthanide atoms form a distorted tetrahedron. The insertion of elemental chalcogen E (E = S, Se) into Li-C bonds of dilithium o-carborane in THF solution afforded dimers of dilithium. dichalcogenolate carboranes, [(THF)(3)LiE2C2B10H10Li(THF)](2) (E = S (12a), Se (12b)), which were confirmed by a crystal structure analysis. Reactions Of Cp'(2)Ln(mu-Cl)(2)Li(THF)(2) (1-10) with 12a or 12b gave dinuclear complexes of the formula [Li(THF)(4)](2)[Cp'(2)LnE(2)C(2)B(10)H(10)](2) (Cp'= eta(5)-t-BuC5H4, E = S, Ln = Nd (13a), Gd (14a), Dy (15a), Er (16a), Yb (17a); E = Se, Ln = Nd (13b), Gd (14b), Dy (15b), Er (16b), Yb (17b); Cp'= 1,3-eta(5)-t-Bu2C5H3 E = S, Ln = Nd (18a), Gd (19a), Dy (20a), Er (21a), Yb (22a); E = Se, Ln = Nd (18b), Gd (19b), Dy (20b), Er (21b), Yb (22b)). According to the X-ray structure analyses, the dianions of 13a and 13b contain two o-carborane dichalcogenolate bridges, and each CP'2Ln fragment is attached to one terminal and two bridging chalcogen ligands. The central Ln(2)E(2) four-membered ring is not planar, and the direct metal-metal interaction is absent.

Metals in the Exosphere of the Highly Irradiated Planet WASP-12b

We present near-UV transmission spectroscopy of the highly irradiated transiting exoplanet WASP-12b, obtained with the Cosmic Origins Spectrograph on the Hubble Space Telescope. The spectra cover three distinct wavelength ranges: NUVA (2539-2580 Å), NUVB (2655-2696 Å), and NUVC (2770-2811 Å). Three independent methods all reveal enhanced transit depths attributable to absorption by resonance lines of metals in the exosphere of WASP-12b. Light curves of total counts in the NUVA and NUVC wavelength ranges show a detection at a 2.5s level. We detect extra absorption in the Mg II ??2800 resonance line cores at the 2.8s level. The NUVA, NUVB, and NUVC light curves imply effective radii of 2.69 ± 0.24 R J , 2.18 ± 0.18 R J , and 2.66 ± 0.22 R J respectively, suggesting the planet is surrounded by an absorbing cloud which overfills the Roche lobe. We detect enhanced transit depths at the wavelengths of resonance lines of neutral sodium, tin, and manganese, and at singly ionized ytterbium, scandium, manganese, aluminum, vanadium, and magnesium. We also find the statistically expected number of anomalous transit depths at wavelengths not associated with any known resonance line. Our data are limited by photon noise, but taken as a whole the results are strong evidence for an extended absorbing exosphere surrounding the planet. The NUVA data exhibit an early ingress, contrary to model expectations; we speculate this could be due to the presence of a disk of previously stripped material.

A high C/O ratio and weak thermal inversion in the atmosphere of exoplanet WASP-12b

The carbon-to-oxygen ratio (C/O) in a planet provides critical information about its primordial origins and subsequent evolution. A primordial C/O greater than 0.8 causes a carbide-dominated interior, as opposed to the silicate-dominated composition found on Earth; the atmosphere can also differ from those in the Solar System. The solar C/O is 0.54 (ref. 3). Here we report an analysis of dayside multi-wavelength photometry of the transiting hot-Jupiter WASP-12b (ref. 6) that reveals C/O>=1 in its atmosphere. The atmosphere is abundant in CO. It is depleted in water vapour and enhanced in methane, each by more than two orders of magnitude compared to a solar-abundance chemical-equilibrium model at the expected temperatures. We also find that the extremely irradiated atmosphere (T>2,500K) of WASP-12b lacks a prominent thermal inversion (or stratosphere) and has very efficient day-night energy circulation. The absence of a strong thermal inversion is in stark contrast to theoretical predictions for the most highly irradiated hot-Jupiter atmospheres.