Subduction initiation and ophiolite crust: new insights from IODP drilling

International Ocean Discovery Program (IODP) Expedition 352 recovered a high-fidelity record of volcanism related to subduction initiation in the Bonin fore-arc. Two sites (U1440 and U1441) located in deep water nearer to the trench recovered basalts and related rocks; two sites (U1439 and U1442) located in shallower water further from the trench recovered boninites and related rocks. Drilling in both areas ended in dolerites inferred to be sheeted intrusive rocks. The basalts apparently erupted immediately after subduction initiation and have compositions similar to those of the most depleted basalts generated by rapid sea-floor spreading at mid-ocean ridges, with little or no slab input. Subsequent melting to generate boninites involved more depleted mantle and hotter and deeper subducted components as subduction progressed and volcanism migrated away from the trench. This volcanic sequence is akin to that recorded by many ophiolites, supporting a direct link between subduction initiation, fore-arc spreading, and ophiolite genesis.     

Effects of Rainwater Iron and Hydrogen Peroxide on Iron Speciation and Phytoplankton Growth in Seawater near Bermuda

Rainwater is a major source of dissolved iron to much of the world's oceans, including regions where iron may be a limiting nutrient for marine phytoplankton primary production. Rainwater iron is therefore potentially important in regulating global photosynthetic uptake of CO₂, and hence climate. Two rainwater addition bioassay experiments (2% rain) conducted at the Bermuda Atlantic Time-series Station (BATS) during March 2000 using 50 or 100 nM FeCl₂ or FeCl₃ in synthetic rain (pH 4.5 H₂SO₄) showed an increase in chlorophyll a 50% greater than controls after three days. Addition of 20 μM hydrogen peroxide, a typical rainwater concentration at BATS, completely removed the chlorophyll a increase with both forms of iron additions, suggesting stimulation of phytoplankton growth by rainwater iron can be limited by rainwater H₂O₂. In laboratory experiments using Gulf Stream seawater, iron-enriched (100 nM Fe(III)) synthetic rain was mixed with seawater in a 5% rain 95% seawater ratio. Dissolved iron concentrations increased two times above concentrations predicted based on dilution alone. The increase in soluble iron probably resulted from release from seawater particles and was maintained for more than 24 hours. No increase was observed in controls that did not have iron added to the synthetic rain, or with synthetic rainwater containing both added iron and H₂O₂. The increase in iron concentration above that predicted by dilution indicates rain may have a larger effect on seawater iron concentrations than that calculated for rainwater iron addition alone.     

Resonant excitation of white dwarf oscillations in compact object binaries – I. The no back reaction approximation

We consider the evolution of white dwarfs with compact object companions (specifically black holes with masses up to  ∼10⁶  M_⊙  , neutron stars, and other white dwarfs). We suppose that the orbits are initially quite elliptical and then shrink and circularize under the action of gravitational radiation. During this evolution, the white dwarfs will pass through resonances when harmonics of the orbital frequency match the stellar oscillation eigenfrequencies. As a star passes through these resonances, the associated modes will be excited and can be driven to amplitudes that are so large that there is a back reaction on the orbit which, in turn, limits the growth of the modes. A formalism is presented for describing this dynamical interaction for a non-rotating star in the linear approximation when the orbit can be treated as non-relativistic. A semi-analytical expression is found for computing the resonant energy transfer as a function of stellar and orbital parameters for the regime where back reaction may be neglected. This is used to calculate the results of passage through a sequence of resonances for several hypothetical systems. It is found that the amplitude of the  ℓ= m = 2  f -mode can be driven into the non-linear regime for appropriate initial conditions. We also discuss where the no back reaction approximation is expected to fail, and the qualitative effects of back reaction.     

The distribution and abundance of pelagic gammarid amphipods on Georges Bank and Nantucket Shoals

In this study, long-term, broad-scale zooplankton survey data were used to estimate the temporal and spatial distribution and abundance of gammarid amphipods present in the water column on Georges Bank. Delta-mean abundances computed from 10 years of data showed that gammarid amphipod abundances peaked in summer and again in fall. The amphipods were also most numerous in water less than 50 m deep. The statistical tests employed revealed no conclusive evidence for diurnal vertical migration. Interannual delta-mean abundances fluctuated approximately 5-fold between 1977 and 1986, ranging from 217 to 1181 amphipods 100 m⁻³. Peak amphipod biomass occurred in July and was estimated to be 2.8 kcal m⁻². Using production-to-biomass ratios from the literature, mean annual production of amphipods in these samples was estimated to be between 1.6 and 9.8 kcal m⁻². Production in shallow areas was especially high, 22 kcal m⁻² year⁻¹.     

The detection of interstellar methylcyanoacetylene

A new interstellar molecule, methylcyanoacetylene (CH3C3N), has been detected in the molecular cloud TMC-1. The J = 8 --> 7, J = 7 --> 6, J = 6 --> 5, and J = 5 --> 4 transitions have been observed. For the first three of these, both the K = 0 and K = 1 components are present, while for J = 5 --> 4, only the K = 0 line has been detected. The observed frequencies were calculated by assuming a value of radial velocity VLSR = 5.8 km s-1 for TMC-1, typical of other molecules in the cloud. All observed frequencies are within 10 kHz of the calculated frequencies, which are based on the 1982 laboratory constants of Moises et al., so the identification is secure. The lines are broadened by hyperfine splitting, and the J = 5 --> 4, K = 0 transition shows incipient resolution into three hyperfine components. The rotational temperature determined for these observations is quite low, with 2.7 K < or = Trot < or = 4 K. the total column density is approximately 5 x 10(12) cm-2.     

A multidimensional, adiabatic hydrodynamics code for studying tidal excitation

We have developed a massively parallel, simple and fast hydrodynamics code for multidimensional, self-gravitating and adiabatic flows. Our primary motivation is the study of the non-linear development of white dwarf oscillations excited via tidal resonances, typically over hundreds of stellar dynamical times. Consequently, we require long-term stability, low diffusivity and high-numerical efficiency. This is accomplished by an Eulerian finite-difference scheme on a regular Cartesian grid. This choice of coordinates provides uniform resolution throughout the flow as well as simplifying the computation of the self-gravitational potential, which is done via spectral methods. In this paper, we describe the numerical scheme and present the results of some common diagnostic problems. We also demonstrate the stability of a cold white dwarf in three dimensions over hundreds of dynamical times. Finally, we compare the results of the numerical scheme to the linear theory of adiabatic oscillations, finding numerical quality factors on the order of 6000 and excellent agreement with the oscillation frequency obtained by the linear analysis.     

Imaging bright-spots in the accretion flow near the black hole horizon of Sgr A*

Solar active regions are distinguished by their strong magnetic fields. Modern local helioseismology seeks to probe them by observing waves which emerge at the solar surface having passed through their interiors. We address the question of how an acoustic wave from below is partially converted to magnetic waves as it passes through a vertical magnetic field layer where the sound and Alfvén speeds coincide (the equipartition level), and find that (i) there is no associated reflection at this depth, either acoustic or magnetic, only transmission and conversion to an ongoing magnetic wave; and (ii) conversion in active regions is likely to be strong, though not total, at frequencies typically used in local helioseismology, with lower frequencies less strongly converted. A simple analytical formula is presented for the acoustic-to-magnetic conversion coefficient.     

Colour corrections for high-redshift objects due to intergalactic attenuation

Corrections to the magnitudes of high-redshift objects due to intergalactic attenuation are computed using current estimates of the properties of the intergalactic medium (IGM). The results of numerical simulations are used to estimate the contributions to resonant scattering from the higher-order Lyman transitions. Differences of 0.5–1 mag from the previous estimate of Madau are found. Intergalactic k _IGM-corrections and colours are provided for high-redshift starburst galaxies and Type I and Type II quasi-stellar objects for several filter systems used in current and planned deep optical and infrared surveys.