Trends in pCO2 and sea–air CO2 flux over the global open oceans for the last two decades     

Yosuke Iida  Atsushi Kojima  Yusuke Takatani  Toshiya Nakano  Hiroyuki Sugimoto  Takashi Midorikawa  Masao Ishii 《Journal of Oceanography》2015,71(6):637-661

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Seasonal and Interannual Variation of DIC in Surface Mixed Layer in the Oyashio Region: A Climatological View     

Tsuneo?OnoEmail author  Hiromi?Kasai  Takashi?Midorikawa  Yusuke?Takatani  Kazuhiro?Saito  Masao?Ishii  Yutaka?W.?Watanabe  Katsuyuki?Sasaki 《Journal of Oceanography》2005,61(6):1075-1087

Eight-year observation results of DIC from 1996 to 2003 in the Oyashio region have been analyzed to obtain a climatological view of its seasonal variation and interannual variation. Data of DIC obtained by several institutes are synthesized to give a dataset with an uncertainty lower than 5 μmol/kg. The obtained climatology of NDIC seasonal variation in the Oyashio mixed layer shows a seasonal amplitude of 176 μmol/kg, with a maximum in January and a minimum in September. These features closely resemble those observed in the southern half of the western subarctic North Pacific (WSNP) including Station KNOT, although the timing of the NDIC maximum is slightly advanced in the case of the Oyashio. Analysis using a quasi-conservative tracer Cp0 (NDIC - 106NP) shows that among 176 μmol/kg of NDIC seasonal variation, only 16 μmol/kg is attributed to hydrographic processes while the remaining 160 μmol/kg is attributed to biological processes. The Cp0 value in the Oyashio mixed layer also resembles that of the WSNP mixed layer during the months May to November, suggesting further resemblance of the Oyashio water mass to that of WSNP in terms of carbon dynamics. The present results also suggest that a single data obtained in Oyashio mixed layer contains 30 μmol/kg of potential uncertainty for the representativity of this region, which leads to a note about a need to treat with caution results obtained by a single observation in this region.  相似文献   

Solar wind speed and its acceleration inferred using the interplanetary scintillation method in carrington rotation 1753     

Kazuyuki Hakamada  Masayoshi Kojima 《Solar physics》1994,153(1-2):419-435

Solar wind speeds (SWSs) estimated by interplanetary scintillation (IPS) observations during Carrington rotation 1753 are projected onto the so-called source-surface of 2.5 solar radii along magnetic field lines in interplanetary space. The following two working hypotheses are examined from different points of view: (1) The SWS is a weighted mean along the line of sight to a radio source; the weight for the SWS depends on the distance from theP-point, the closest approach to the Sun on the line of sight. (2) The weighting function has a very sharp peak at theP-point, so that the SWS shows a real solar wind speed at theP-point. In both the two cases, the SWSs projected onto the source surface are further projected onto the photosphere along magnetic field lines in the corona. Footpoints of these field lines are inferred as photospheric source regions of the solar wind. The intensity of the Hei (1083 nm) absorption line (HEI) in the chromosphere corresponding to these photospheric sources is interpolated from observational data. The weighted mean of the HEI is calculated in case 1. The HEI corresponding to theP-point is used in case 2. The SWS is compared with the HEI in both the two cases. It is found that the correlation between the SWS and the HEI is better in case 2 than in case 1. It is further inferred by correlation analysis between the SWS and the HEI that the solar wind is accelerated within 27 solar radii on average. Although the data examined in this paper were limited to just one solar rotation, these results suggest that the SWS estimated by the IPS technique corresponds to the solar wind speed near theP-point and the weighting function along the line of sight may have a very sharp peak near theP-point.  相似文献   

Kuroshio warm filament and the source of the warm water of the Tsushima Current   总被引：3，自引：2，他引：3  

Guo Binghuo  Xiu Shumeng  Haruo Ishii  Yasuaki Nakamura 《海洋学报(英文版)》1991,10(3):325-340

Characteristics and evolution of the Kuroshio frontal eddies and warm filaments are analyzed according to two series of satellite images (March 5 to 7, 1986 and April 14 to 16, 1988). The results show that the frontal eddies in the East China Sea are generated at the shelf break and move along the continental slope at a speed of 15 cm/s with the Kuroshio. The frontal eddies occur about every 10 d and evolve to be warm filaments a few hundred km in length and 30-40 km in width in the area west of the Yaku-shima. Meanwhile, the existence of the warm filament was also found in the area by analysing the hydrographic data in the area west of Kyushu during May 24-June 5, 1988.The Kuroshio warm filaments move westward opposite to the Kuroshio and then turn northward at the shelf break and become the main source of the warm water of the Tsushima Warm Current. A simple dynamic explanation for the process is presented in this paper.  相似文献   

Early tholeiitic and calc-alkaline arc magmatism of middle to Late Eocene Age in the southern Ogasawara (Bonin) forearc     

Satoru Haraguchi  Teruaki Ishii  Jun-Ichi Kimura 《Contributions to Mineralogy and Petrology》2008,156(2):269-272

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Preferential exchange rate effect of isotopic fractionation in a melting snowpack     

Shiqiao Zhou  Masayoshi Nakawo  Shigemasa Hashimoto  Akiko Sakai 《水文研究》2008,22(18):3734-3740

Stable isotope exchange processes between solid and liquid phases of a natural melting snowpack are investigated in detail by separating the liquid water from snow grains at different depths of the snowpack and collecting the bottom discharge using a lysimeter. In the melting–freezing mass exchange process between the two phases, the theoretical slope of the δD? δ¹⁸O line for newly refrozen ice is calculated to be nearly that of pore water. However, based on observations of the isotopic evolution and snow grain coarsening of the snowpack, it is demonstrated that the slope of the δD? δ¹⁸O line for newly refrozen ice is equal to that of the original ice. This is proved to be due to preferential water flow in the snowpack, which leads to relatively more deuterium and less oxygen‐18 in the mobile water than the immobile water because of the kinetic effect. Higher mass exchange rate in the mobile water region results in excess deuterium in the bulk refrozen ice, compared with the fractionation of uniform fractionation factors and exchange rate. This effect, which is termed the ‘preferential exchange rate effect of isotopic fractionation’, is shown to be larger in the lower part than the upper part of the snowpack. Copyright © 2008 John Wiley & Sons, Ltd.  相似文献   

Improving the scientific assessment of carbon sinks     

Atsushi Ishii 《Climate Policy》2013,13(2):217-224

Abstract

The future role of carbon sinks with reference to the Kyoto Protocol depends significantly on developing an international consensus on carbon-sink assessment and carbon accounting. A clear and practical approach is needed that allows both the scientific community and policy-makers to construct a viable operational framework. This article proposes that a new strategy be developed for carbon-sink assessment based on full carbon accounting (FCA) alongside a separate political tool for carbon accounting. This approach is derived from the experience of the European critical loads (CL) concept, which seeks to quantify levels of pollutants (such as sulfur) that can be absorbed by the environment without causing ecological harm. Crucial to the implementation of such a strategy are robust institutional settings, such as an internationally coordinated monitoring system, open and fair access to the assessment processes, and international research cooperation programs for addressing associated problems of carbon-sink activities.  相似文献   

The survivability of phyllosilicates and carbonates impacting Stardust Al foils: Facilitating the search for cometary water          下载免费PDF全文

Penelope J. Wozniakiewicz  Hope A. Ishii  Anton T. Kearsley  John P. Bradley  Mark. C. Price  Mark J. Burchell  Nick Teslich  Mike J. Cole 《Meteoritics & planetary science》2015,50(12):2003-2023

Comet 81P/Wild 2 samples returned by NASA's Stardust mission provide an unequalled opportunity to study the contents of, and hence conditions and processes operating on, comets. They can potentially validate contentious interpretations of cometary infrared spectra and in situ mass spectrometry data: specifically the identification of phyllosilicates and carbonates. However, Wild 2 dust was collected via impact into capture media at ~6 km s^?1, leading to uncertainty as to whether these minerals were captured intact, and, if subjected to alteration, whether they remain recognizable. We simulated Stardust Al foil capture conditions using a two‐stage light‐gas gun, and directly compared transmission electron microscope analyses of pre‐ and postimpact samples to investigate survivability of lizardite and cronstedtite (phyllosilicates) and calcite (carbonate). We find the phyllosilicates do not survive impact as intact crystalline materials but as moderately to highly vesiculated amorphous residues lining resultant impact craters, whose bulk cation to Si ratios remain close to that of the impacting grain. Closer inspection reveals variation in these elements on a submicron scale, where impact‐induced melting accompanied by reducing conditions (due to the production of oxygen scavenging molten Al from the target foils) has resulted in the production of native silicon and Fe‐ and Fe‐Si‐rich phases. In contrast, large areas of crystalline calcite are preserved within the calcite residue, with smaller regions of vesiculated, Al‐bearing calcic glass. Unambiguous identification of calcite impactors on Stardust Al foil is therefore possible, while phyllosilicate impactors may be inferred from vesiculated residues with appropriate bulk cation to Si ratios. Finally, we demonstrate that the characteristic textures and elemental distributions identifying phyllosilicates and carbonates by transmission electron microscopy can also be observed by state‐of‐the‐art scanning electron microscopy providing rapid, nondestructive initial mineral identifications in Stardust residues.  相似文献   

The rectilinear three-body problem using symbol sequence I. Role of triple collision     

Masaya Masayoshi Saito  Kiyotaka Tanikawa 《Celestial Mechanics and Dynamical Astronomy》2007,98(2):95-120

The dynamical structure of phase space of gravitational Newtonian three bodies which lie on a line (rectilinear three-body system) is studied. We take an initial value plane and classify the points on the plane according to the fate of the orbits starting from the points, using symbol sequences. The structure appearing on the initial value plane with this classification was well studied for the equal-mass case (Tanikawa and Mikkola 2000, Chaos 10, 649–657). In this paper, we follow and clarify the changes of this structure with the mass ratio of three particles.  相似文献   

Extinction curves expected in young galaxies     

Hiroyuki Hirashita †‡  Takaya Nozawa  Takashi Kozasa  Takako T. Ishii †  Tsutomu T. Takeuchi § 《Monthly notices of the Royal Astronomical Society》2005,357(3):1077-1087

We investigate the extinction curves of young galaxies in which dust is supplied from Type II supernovae (SNe II) and/or pair instability supernovae (PISNe). We adopt Nozawa et al. (2003) for compositions and size distribution of grains formed in SNe II and PISNe. We find that the extinction curve is quite sensitive to internal metal mixing in supernovae (SNe). The extinction curves predicted from the mixed SNe are dominated by SiO₂ and are characterized by a steep rise from infrared to ultraviolet (UV). The dust from unmixed SNe shows a shallower extinction curve, because of the contribution from large-sized (∼0.1 μm) Si grains. However, the progenitor mass is important in unmixed SNe II: if the progenitor mass is smaller than  ∼20 M_⊙  , the extinction curve is flat in UV; otherwise, the extinction curve rises towards the short wavelength. The extinction curve observed in a high-redshift quasar  ( z = 6.2)  favours the dust production by unmixed SNe II. We also provide some useful observational quantities, so that our model might be compared with future high- z extinction curves.  相似文献