Spectral variations of the nova V2468 Cyg at various stages of the development of its outburst

Spectral variations of the nova V2468 Cyg were studied over 1.5 years following the beginning of its outburst, during its smooth fading and the star’s rebrightenings. Following the rebrightening on March 25, 2008, the profiles of H I lines had changed, from a two-component structure with peaks at ?220 and 670 km/s to a four-component structure with peaks at ?640, ?260, 255, and 620 km/s. The profiles of [N II] 5755 Å, [O III] 5007 Å, He II 4686 Å, and [Fe VII] 6086 Å lines varied throughout the interval of our observations. During rebrightenings, the lines profiles changed and the line intensities significantly decreased. The width of the [Fe VII] 6086 Å profile varied, in addition to its shape and intensity; this profile differed from the profiles of other lines during the nebular phase. Estimates of chemical-element abundances in the nova’s envelope indicate enhanced abundances of nitrogen and oxygen, compared to the Sun, and solar abundances of neon and argon. The helium abundance was somewhat higher than the solar value. The mass of the ejected envelope is estimated to be 5 × 10^?5 M _⊙.     

Evolutionary changes in the optical spectrum of the peculiar supergiant IRC+10420

We present new spectroscopic observations of the peculiar supergiant IRC+10420. In 1997–2000, we obtained three high signal-to-noise ratio spectra of the object at 4300–8000 Å with a spectral resolution of 15 000 (20 km/ s) using the 6-m telescope of the Special Astrophysical Observatory. From our 2000 spectrum, we estimate the spectral type of IRC+10420 to be A2, corresponding to a temperature of ～9200 K. Many emission lines were detected, identified with lines of Fe I; Fe II, Ti II, Cr II, and Sc II ions; and [O I], [Fe II], and [Ca II] forbidden lines. The radial velocity derived from absorption lines without obvious emission components (He I λ5876, O I, N I, Si II) and from absorption components of the Balmer lines is 93±1 km/s. The redshift of photospheric lines relative to the star’s center-of-mass velocity is interpreted as a consequence of scattering in the expanding, optically thick dust envelope. Both emission and absorption lines show a correlation between radial velocity and oscillator strength. We found variability in the relative intensities of the H _α and H _β emission components. We conclude that IRC+10420 is rapidly evolving towards a Wolf-Rayet stage; the current rate of the photospheric temperature increase is ～120 K per year. Based on the intensity of the O I (λ7773) triplet, we estimate the star’s luminosity to be M _bol=?9.5^m. In all 1997–2000 spectra of IRC+10420, the He I λ5876 line has a significant equivalent width of at least 200 mÅ; this may be possible in the presence of such a low temperature due to the star’s high luminosity and the enhanced helium abundance in the supergiant’s atmosphere.     

Relationship between chemical composition and magnetic susceptibility in sediment cores from Central Indian Ocean Basin

Three sediment cores in a north-south transect (3°N to 13°S) from different sediment types of the Central Indian Ocean Basin (CIOB) are studied to understand the possible relationship between magnetic susceptibility (χ) and Al, Fe, Ti and Mn concentrations. The calcareous ooze core exhibit lowest χ (12.32 × 10⁻⁷ m³ kg⁻¹), Al (2.84%), Fe (1.63%) and Ti (0.14%), terrigenous clay core with moderate χ (29.93 × 10⁻⁷ m³ kg⁻¹) but highest Al (6.84%), Fe (5.20%) and Ti (0.44%), and siliceous ooze core with highest χ (38.06 × 10⁻⁷ m³ kg⁻¹) but moderate Al (4.49%), Fe (2.80%) and Ti (0.19%) contents. The distribution of χ and detrital proxy elements (Al, Fe, and Ti) are identical in both calcareous and siliceous ooze. Interestingly, in terrigenous core, the behaviour of χ is identical to only Ti content but not with Al and Fe suggesting possibility of Al and Fe having a non-detrital source. The occurrence of phillipsite in terrigenous clay is evident by the Al-K scatter plot where trend line intersects K axis at more than 50% of total K suggesting excess K in the form of phillipsite. Therefore, the presence of phillipsite might be responsible for negative correlation between χ and Al (r = −0.52). In siliceous ooze the strong positive correlations among χ, Al_exc and Fe_exc suggest the presence of authigenic Fe-rich smectite. High Mn content (0.5%) probably in the form of manganese micronodules is also contributing to χ in both calcareous and siliceous ooze but not in the terrigenous core where mean Mn content (0.1%) is similar to crustal abundance. Thus, χ systematically records the terrigenous variation in both the biogenic sediments but in terrigenous clay it indirectly suggests the presence of authigenic minerals.     

The relationship between coronal fan structures and oscillations above faculae regions

The power spectra of radial-velocity and intensity oscillations are analyzed using ground-based (the Si I 10 827 Å and He I 10 830 Å lines) and Solar Dynamics Observatory (the Fe I 6173, 1700 Å, He II 304 Å, and Fe IX 171 Å lines) data, with the aim of searching for frequency modes that most efficiently penetrate into the solar corona from the lower layers of solar faculae. Analysis of the spatial distribution of the oscillation power at various heights indicates that fan structures in the corona (at the height of the 171 Å emission) are better reproduced at frequencies of 1–1.5 mHz. This means that oscillations with periods of 10–15 min dominate in coronal loops above faculae regions. The five-minute oscillations that universally dominate in radial-velocity measurements in low layers of faculae are appreciable in coronal loops only in individual compact fragments.     

Structure of the class I methanol masers OMC-2 and NGC 2264

Results of interferometric observations of the class I methanol masers OMC-2 and NGC 2264 in the 7₀-6₁ A ⁺ and 8₀-7₁ A ⁺ lines at 44 and 95 GHz, respectively, are presented. The maser spots are distributed along the arcs bent toward infrared sources, which are young stellar objects. The distributions of the maser spots at 44 and 95 GHz are virtually identical, and the fluxes from the brightest spots are similar. The measured sizes of the maser spots at 44 GHz are, on average, about 50 AU. The brightness temperature of the strongest components at 44 GHz is 1.7 × 10⁷ K and 3.9 × 10⁷ K for OMC-2 and NGC 2264, respectively. A simple model for the excitation of Class I methanol masers is proposed; it yields an estimate of the limiting brightness temperature of the emission. The model is based solely on the properties of the methanol molecule without invoking the physical parameters of the medium. Using it, we showed that the emission opening angles for NGC 2264 and OMC-2 do not exceed 3° and 4.5°, respectively. The depth of the masing region is about 1000 AU. The emission directivity is naturally realized in the model of of maser consisting of a thermalized core and a thin inverted envelope, probably, with an enhanced methanol abundance. The maser emission has the greatest intensity in the direction tangential to the envelope. The size of the masing envelope estimated from the measured depth and spot extens is ～2 × 10⁴ AU, or 0.15 pc. This size is close to the sizes of the dense molecular cores surrounding the young stellar objects IRS 4 in OMC-2 and IRS 1 in NGC 2264.     

A many-year photometric and spectroscopic variability study of planetary nebulae (1968–2008). The young planetary nebula IC 4997

We present the results of our many-year (1968–2008) photoelectric photometry and absolute spectrophotometry of the young variable planetary nebula IC 4997, performed in uniform systems. Integrated line energy fluxes in the range 3727–5007 Å are tabulated, along with the integrated (star + nebula) continuum flux at 4500 Å, and time variations investigated. We study the time behavior of fluxes in the hydrogen, HeI, [OIII], [OII], [NeIII] emission lines. Variations of the line intensity ratio R = F([OIII]4363 Å)/F(Hγ) between 1938 and 2008 are presented. We estimate the nebula’s electron density N _e and electron temperature T _e for 1972–1992: the mean nebula N _e increased by the factor of five, from ～4 × 10⁵ to ～2 × 10⁶ cm^?3, while the mean T _e increased from 12 000 to 14 000 K. The color temperature of the exciting star, measured from the 4000–4900 Å continuum, increased from 37 000–40 000 K to 47 000 K during the time interval covered by our observations, as is confirmed by the growth of ionization of HeI, NeIII, and OIII (from the 4363 Å line). V-band variations of the object’s integrated (nebula + star) light with an amplitude about 0.5 ^m can essentially be fully explained as being due to changing contributions from variable fluxes in the [OIII] 5007 and 4959 Å lines. The V magnitude in 2009 (after 40 years) happened to be the same as at the start of our observations in 1968. A period of the order of 50 years can also be noted in log R(t). This may provide evidence for binarity of the central star and be related to its orbital period.     

Magnetic mineralogical variability along Deccan trap basalt borehole (KBH07), Koyna deep continental drilling program,western Maharashtra,India

A 1248 m long core (KBH 07, 17°18′07″ N; 73°47′28.2″E, 960m above msl) drilled up to basement in the Deccan traps from Koyna region was sampled at ～10m interval for magnetic mineralogical studies.Analysis of routine rock magnetic parameters (mass specific magnetic susceptibility: χ_lf, frequency dependence of susceptibility: χ_fd, susceptibility of anhysteretic remanance: χ_ARM, saturation isothermal remanance: SIRM, remanance coercivty: B_(0)CR, Soft_IRM, Hard_IRM, S-Ratio, SIRM/χ_lf, χ_ARM/χ_lf) and density (σ, gm/cc) depicted significant higher order temporal variation. The χ_lf varies between 13 and 309 x 10-8m3/kg and is independent of density variation. The χ_ARM, B_(0)CR and S-Ratios indicate majority of SD-PSD ferrimagnets with episodes of MD ferrimagnetic concentration and few hard coercivity components. The giant plagioclase lath bearing (GPB) horizons show highest variability of ferrimagnetic concentration marked by anomalous peaks. Overall the variability of rock magnetic parameters independent of lava flow units suggest that the changeover in magnetic mineral concentration, composition and domain size occur at major episodes in magma composition (e.g., primary source, crustal contamination and fractional crystallization). The studied parameters are therefore examined to mark intervals of (i) magma compositional changes, (ii) zones of oxidative conditions and (iii) rapid/slow cooling intervals demanding detailed petrologic studies. We identified one I order trend, four II order cycles and eight III order cycles for the purpose of correlation. Notable peak in χ_lf at 650–700m, the changeover in rock magnetic parameters at ～930 m and ～280 m can facilitate marker intervals while several higher order variations can be adopted for high resolution correlation to other boreholes in the region. The complex variation in rock magnetic parameters independent of flow units reflect temporal magnitudes of compositional variability, cooling and emplacement history that needs detailed petro-mineralogical attempts; and the present data is useful for high order inter-core correlations under the deep drilling program.     

贵州丹寨卡林型金矿床地球化学特征

岩石化学及微量元素研究表明,从未蚀变层纹状灰岩到强硅化灰岩,SiO₂、Au、As和Sb含量逐渐增高,CaO、CO₂和MgO含量逐步降低;在强碳酸岩化灰岩中,CaO和CO₂含量增高,SiO₂含量降低;各类蚀变与矿化岩石的稀土含量和配分模式与未蚀变层纹状灰岩总体基本一致.流体包裹体资料指示,成矿溶液为富Cl型,爆裂温度为200～338℃.同位素研究揭示,δ³⁴S_硫化物=(16.078～20.48)×10^-3,δ¹⁸O=(19.4～20.3)×10^-3,δD=(-110～-47)×10^-3,²⁰⁶Pb/²⁰⁴Pb=18.288～19.202,207Pb/²⁰⁴Pb=15.685～15.793,²⁰⁸Pb/²⁰⁴Pb=38.366～40.401.成矿流体以大气降水为主,成矿物质以壳源为主,仅有少量幔源组分的参与.     

Boron K-edge XANES of boron oxides: tetrahedral B–O distances and near-surface alteration

Synchrotron radiation boron K-edge XANES spectra collected in fluorescence yield mode are reported for monoclinic metaboric acid [HBO₂(II)], sinhalite (MgAlBO₄), and a selection of boron oxides in which B is exclusively in trigonal coordination (^[3]B). The anomalously high divergence of tetrahedral (^[4]B–O) bond lengths in HBO₂(II) and sinhalite is used to resolve fine structure at the ^[4]B K edge due to splitting of σ*(t₂) antibonding orbitals. For HBO₂(II), XANES peaks at 196.9 and 199.3?eV are assigned to ^[4]B–O distances of 1.564 and ～1.440 (×3) Å, respectively, and, for sinhalite, peaks at 196.8, 197.9, and 199.6?eV are assigned to distances of 1.586, 1.483 (×2), and 1.442?Å, respectively. A correlation between peak splitting at the ^[4]B K edge and divergence of tetrahedral bond length is established for borates and borosilicates using data for sinhalite, HBO₂(II), ferroaxinite, danburite, datolite, and BPO₄. B K-edge XANES spectra collected in total electron yield mode, which probes to <60?Å, show that almost all ^[4]B in HBO₂(II) and about one-third of the ^[4]B in sinhalite are converted to ^[3]B in the near-surface structure. Moreover, HBO₂(II), HBO₂(III), sassolite (boric acid; H₃BO₃), and v-B₂O₃, which have markedly different bulk structures, have a similar near-surface layer composed of a relaxed anhydrous network of BO₃ groups.     

Magnetic properties related to hydrothermal alteration processes at the Escondida porphyry copper deposit,northern Chile

Fluid–rock interaction related to the circulation of hydrothermal fluids can strongly modify the physicochemical properties of wall rocks in porphyry Cu deposits. These processes can also produce compositional and textural changes in ferromagnetic minerals, which can be quantified using magnetic methods. In the Escondida porphyry Cu deposit of northern Chile, each hydrothermally altered lithology is characterized by a discrete assemblage of Fe–Ti oxide minerals. These minerals have distinctive bulk magnetic susceptibility (K _bulk), temperature-dependent magnetic susceptibility, and magnetic hysteresis parameters. Selectively altered rocks (i.e., potassic and chloritic alteration types) exhibit the highest K _bulk values (>3.93?×?10^?3 SI units), and their hysteresis parameters indicate multidomain magnetic mineral behavior. This suggests that these rocks are composed of the coarsest magnetic grain sizes within the deposit. Optical analyses and susceptibility–temperature curves confirm that the magnetic signals in selectively altered rocks are mainly carried by secondary magnetite. In contrast, pervasively altered rocks (i.e., quartz-sericite and argillic alteration types) exhibit low K _bulk values (<1.93?×?10^?4 SI units) and contain smaller pseudo-single domain magnetic grain assemblages. This is consistent with the destruction and/or reduction in size of magnetite under acidic conditions. The results therefore demonstrate a genetic relationship between the hydrothermal alteration processes, Fe–Ti oxide minerals, and magnetic properties of the wall rock in the Escondida deposit. These magnetic methods can be considered a sensitive and efficient petrophysical tool for the identification and semi-quantification of alteration assemblages, and facilitating the recognition and mapping of discrete hydrothermal zones during exploration and operation of porphyry Cu deposits.     

Mössbauer spectroscopic study of iron in Victorian brown coal

The forms of non-pyritic Fe in a suite of Victorian brown coals have been determined by ⁵⁷Fe Mössbauer analysis. The dominant Fe phase is a poorly-ordered ferric oxyhydroxide with a magnetic ordering temperature of (530 ± 50) K and particle size of approximately 50 Å. Upon exposure of the coal to air, this phase slowly crystallises to goethite. Most of the remaining Fe occurs as a high-spin Fe(II) species attributed to dissolved and hence mobile, Fe(II) humate, which precipitates as the ferric oxyhydroxide to an extent determined by the pH. A third species, present in a much lower concentration, appears to exhibit a transition from low-spin to high-spin Fe(II) as water is removed from the coal.     

微波消解-电感耦合等离子体质谱法测定铁矿石中铬砷镉汞铅

铁矿石中Cr、As、Cd、Hg和Pb不仅影响冶炼设备和产品性能,同时污染环境。文章以铁矿石标准物质为研究对象,对电感耦合等离子体质谱法(ICP-MS)测定铁矿石中Cd、As、Cr、Hg和Pb等5种元素进行了适用性探讨。结果表明,与常规的单元素原子吸收光谱法或多元素同步分析电感耦合等离子体发射光谱法相比,用微波消解方法处理铁矿石,具有样品消耗量少(0.1000±0.0200)g、消解用酸少(2.5 mL HCl+0.5 mL HF+1.0 mL HNO3)、排放降低、节约成本等优点,且无需配制铁底液,无需添加任何掩蔽剂,质谱干扰小,适用于分析Cr含量为5.5×10-10～2.5×10-4,As含量为7.6×10-10～1.9×10-4,Cd含量为4.5×10-11～5.5×10-6,Hg含量为1.88×10-9～1.9×10-7,Pb含量为1.2×10-10～3.2×10-5的铁矿石样品。优化后的前处理方法节约了能源、试剂和样品消耗,降低了二次污染和有效损失。     

The thermal expansion of anhydrite to 1000° C

The thermal expansion of anhydrite, CaSO₄, has been measured from 22° to 1,000° C by X-ray diffraction, using the Guinier-Lenné heating powder camera. The heating patterns were calibrated with Guinier-Hägg patterns at 25° C, using quartz as internal standard. Heating experiments were run on natural anhydrite (Bancroft, Ontario), which at room temperature has lattice constants in close agreement with those of synthetic material. The orthorhombic unit cell at 22° C (space group Amma) has a=7.003 (1) Å, b=6.996 (2) Å and c=6.242 (1) Å, V=305.9 (2) ų. At room temperature, the thermal expansion coefficients α and β (α in °C^?1×10⁴, β in °C^?2×10⁸) are for a, 0.10, ?0.69; for b, 0.08, 0.19; for c, 0.18, 1.60; for V, 0.37, 1.14. Second-order coefficients provide an excellent fit over the whole range to 1,000° C.     

A search for small-scale clumpiness in dense cores of molecular clouds

We have analyzed HCN(1-0) and CS(2-1) line profiles obtained with high signal-to-noise ratios toward distinct positions in three selected objects in order to search for small-scale structure in molecular cloud cores associated with regions of high-mass star formation. In some cases, ripples were detected in the line profiles, which could be due to the presence of a large number of unresolved small clumps in the telescope beam. The number of clumps for regions with linear scales of ～0.2–0.5 pc is determined using an analytical model and detailed calculations for a clumpy cloud model; this number varies in the range: ～2 × 10⁴–3 × 10⁵, depending on the source. The clump densities range from ～3 × 10⁵–10⁶ cm^?3, and the sizes and volume filling factors of the clumps are ～(1–3) × 10^?3 pc and ～0.03–0.12. The clumps are surrounded by inter-clump gas with densities not lower than ～(2–7) × 10⁴ cm^?3. The internal thermal energy of the gas in the model clumps is much higher than their gravitational energy. Their mean lifetimes can depend on the inter-clump collisional rates, and vary in the range ～10⁴–10⁵ yr. These structures are probably connected with density fluctuations due to turbulence in high-mass star-forming regions.     

Timing and nature of fluid flow and alteration during Mesoproterozoic shear zone formation, Olary Domain, South Australia

The development of shear zones at mid‐crustal levels in the Proterozoic Willyama Supergroup was synchronous with widespread fluid flow resulting in albitization and calcsilicate alteration. Monazite dating of shear zone fabrics reveal that they formed at 1582 ± 22 Ma, at the end of the Olarian D3 deformational event and immediately prior to the emplacement of regional S‐type granites. Two stages of fluid flow are identified in the area: first an albitizing event which involved the addition of Na and loss of Si, K and Fe; and a second phase of calcsilicate alteration with additions of Ca, Fe, Mg and Si and removal of Na. Fluid fluxes calculated for albitization and calcsilicate alteration were 5.56 × 10⁹ to 1.02 × 10¹⁰ mol m^?2 and 2.57 × 10⁸–5.20 × 10⁹ mol m^?2 respectively. These fluxes are consistent with estimates for fluid flow through mid‐crustal shear zones in other terranes. The fluids associated with shearing and alteration are calculated to have δ¹⁸O and δD values ranging between +8 and +11‰, and ?33 and ?42‰, respectively, and ?Nd values between ?2.24 and ?8.11. Our results indicate that fluids were derived from metamorphic dehydration of the Willyama Supergroup metasediments. Fluid generation occurred during prograde metamorphism of deeper crustal rocks at or near peak pressure conditions. Shear zones acted as conduits for major crustal fluid flow to shallow levels where peak metamorphic conditions had been attained earlier leading to the apparent ‘retrograde’ fluid‐flow event. Thus, the peak metamorphism conditions at upper and lower crustal levels were achieved at differing times, prior to regional granite formation, during the same orogenic cycle leading to the formation of retrograde mineral assemblages during shearing.     

Phase F,a new hydrous magnesium silicate synthesized at 1000 °C and 17 GPa: Crystal structure and estimated bulk modulus

The structure of phase F, a non-stoichiometric hydrous silicate synthesized in a uniaxial, split-sphere, multi-anvil apparatus at conditions of 17 GPa and 1000° C, has been solved and refined in space group P6₃cm, using synchrotron X-ray data for a single crystal of a size 18 × 24 × 30 μm. The composition and unit cell for phase F are Mg_3.35Si_5.51H_7.26O₁₈, a=5.073(3) Å, c=14.013(9) Å, 7= 312.3(5) ų. The structure contains layers with many similarities to superhydrous phase B. The layers of oxygen atoms are stacked in the ABCBAC-type double cubic closest packing arrangement. The bulk modulus of phase F was estimated from the structural and compositional relationship to superhydrous phase B and periclase.     

Geochemical criteria of the Upper Sinian cherts of hydrothermal origin on the southeast continental margin of the Yangtze plate

The Upper Sinian bedded cherts are widely distributed on the southeast continental margin of the Yangtze plate, with a total thickness ranging from 20 to 150 m. The cherts are very simple in chemical composition, with the contents of siliceous minerals exceeding 90% and those of other mineral species being very low. The total content of trace elements is considerably variable. The contents of most trace elements are low as compared with their crust clarke values. But these cherts are very rich in the trace elements Ba, As, Ab, Ag and U, coupled with relatively high contents of Fe, Mn and low contents of Al, Ti, and Mg. It can be identified as the cherts of hydrothermal origin in terms of the values of Fe/Ti, (Fe + Mn)/Ti, Al/ (Al + Fe + Mn) and U/Th. In the Al-Fe-Mn, and Fe-Mn-(Cu + Ni + Co) × 10 diagrams and lg [U]-lg[Th], Cr-Zr diagrams, all the samples from the area studied fall within the hydrothermal sediment field. All these characteristics show that the cherts are mainly the product of hydrothermal processes. The fact that the δ³⁰Si values of the chert range from 0.0‰ to 0.7‰ with §¹⁸O from 20.l‰ to 23.6‰ clearly manifests that the submarine hydrothermal water is the main source of silica.     

Radio-colouration of diamond: a spectroscopic study

We have undertaken a study of the common green or orange-brown spots at the surface of rough diamond specimens, which are caused by alpha particles emanating from radioactive sources outside the diamond. Richly coloured haloes represent elevated levels of structural damage, indicated by strong broadening of the main Raman band of diamond, intense strain birefringence, and up-doming of spots due to their extensive volume expansion. Green radio-colouration was analogously generated through the irradiation of diamond with 8.8 MeV helium ions. The generation of readily visible radio-colouration was observed after irradiating diamond with ≥10¹⁵ He ions per cm². The accumulation of such a high number of alpha particles requires irradiation of the diamond from a radioactive source over long periods of time, presumably hundreds of millions of years in many cases. In the samples irradiated with He ions, amorphisation was observed in volume areas where the defect density exceeded 5 × 10^?3 Å^?3 (or 0.03 dpa; displacements per target atom). In contrast, graphitisation as a direct result of the ion irradiation was not observed. The green colouration transformed to brown at moderate annealing temperatures (here 450 °C). The colour transformation is associated with only partial recovery of the radiation damage. The colour change is mainly due to the destruction of the GR1 centre, explained by trapping of vacancies at A defects to form the H3 centre. An activation energy of ~2.4 ± 0.2 eV was determined for the GR1 reduction. The H3 centre, in turn, causes intense yellowish-green photoluminescence under ultraviolet illumination. Radio-colouration and associated H3 photoluminescence are due to point defects created by the ions irradiated, whereas lattice ionisation is of minor importance. This is concluded from the depth distribution of the colouration and the photoluminescence intensity (which corresponds to the defect density but not the ionisation distribution pattern). The effect of the implanted He ions themselves on the colour and photoluminescence seems to be negligible, as radio-colouration and H3 emission were analogously produced through irradiation of diamond with C ions. The photoluminescence emission becomes observable at extremely low defect densities on the order of 10^?6 Å^?3 (or 0.000006 dpa) and is suppressed at moderate defect densities of ~5 × 10^?4 Å^?3 (or ~0.003 dpa). Intensely brown-coloured diamond hence does not show the H3 emission anymore. Anneals up to 1,600 °C has reduced considerably irradiation damage and radio-colouration, but the structural reconstitution of the diamond (and its de-colouration) was still incomplete.     

Iodine diagenesis in pelagic deep-sea sediments

Nineteen sediment cores from the Madeira, Seine, Tagus and Nares Abyssal Plains and the Alboran Sea have been used to evaluate the speciation, fluxes and diagenesis of iodine in the deep sea. The sediments have surficial molar I/C ratios of 10–30 × 10⁻⁴ in excess of previous reported values for planktonic material (~1 × 10⁻⁴). Solid phase I contents decrease exponentially with depth corresponding to decomposition rate constants of 5–260 × 10⁻⁶ yr⁻¹ which vary with the carbon accumulation rate.Iodine species in the pore waters follow a vertical sequence of four zones: 1. a zone of I⁻ production where total dissolved iodine (∑I) concentrations initially increase at the seawater-sediment interface; 2. a zone of I⁻ oxidation where interconversion of I⁻ to IO⁻₃ occurs; 3. a zone of IO⁻₃ reduction where interconversion of IO⁻₃ back to I⁻ occurs which corresponds to the suboxic part of the sediment column; and 4. a further zone of I⁻ production which is confined to the lower anoxic part of the sediment column. Benthic ∑I fluxes in the Madeira Abyssal Plain measured from shipboard incubation experiments and calculated from porewater gradients are similar, averaging 0.55 and 0.36 × 10⁻⁸ μmol cm⁻² sec⁻, respectively.In the surface sediment the observed I enrichment results from a quasi-closed cycle for iodine initially involving release of I⁻ from decomposing marine organic matter followed by rapid removal onto organic matter at the sediment-seawater interface where I/C regeneration ratios of up to 200 × 10⁻⁴ are found, lodate reduction occurs during suboxic diagenesis, after denitrification and before MnO₂ reduction, consistent with the sequence of reactions predicted from the free energy yields for organic matter oxidation. There is some further I⁻ production in the anoxic section of sediments but at much smaller rates than occur during the interfacial diagenetic cycling.     

Titanium,Ti, A New Mineral Species from Luobusha,Tibet, China

We describe the new mineral species titanium,ideally Ti,found in the podiform chromitites of the Luobusha ophiolite in Tibet,People’s Republic of China.The irregular crystals range from 0.1 to 0.6 mm in diameter and form an intergrowth with coesite and kyanite.Titanium is silver grey in colour,the luster is metallic,it is opaque,the streak is grayish black,and it is non-fluorescent.The mineral is malleable,has a rough to hackly fracture and has no apparent cleavage.The estimated Mohs hardness is 4,and the calculated density is 4.503 g/cm3.The composition is Ti 99.23-100.00 wt%.The mineral is hexagonal,space group P63 /mmc.Unit-cell parameters are a 2.950(2),c 4.686(1),V 35.32(5) 3,Z = 2.The five strongest powder diffraction lines [d in(hkl)(I/I0)] are: 2.569(010)(32),2.254(011)(100),1.730(012)(16),1.478(110)(21),and 0.9464(121)(8).The species and name were approved by the CNMNC(IMA 2010–044).