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91.
Millennial-scale oscillations of the westerly jet path during the last glacial period 总被引:1,自引:0,他引:1
Kana Nagashima Ryuji Tada Atsushi Tani Youbin Sun Yuko Isozaki Shin Toyoda Hitoshi Hasegawa 《Journal of Asian Earth Sciences》2011,40(6):239-1220
It has been established that East Asian summer monsoon intensity varies with Dansgaard–Oeschger cycles, suggesting a connection between the climates of East Asia and the North Atlantic on a millennial timescale. However, the dynamics of such a connection are still unsolved. Here we demonstrate that temporal changes in the provenance of aeolian dust in Japan Sea sediments, which we interpret to reflect changes in the westerly jet path over East Asia, exhibit variations in harmony with Dansgaard–Oeschger cycles. The dominance of dust with a Mongolian Gobi provenance during stadials suggests a westerly jet axis located to the south of the Himalaya–Tibetan Plateau throughout most of the year, whereas the co-dominance of dust from both the Taklimakan Desert and the Mongolian Gobi during interstadials suggests that the westerly jet axis jumped to the north of the Tibetan Plateau at latest in summer. As the shift of the westerly jet axis to the north of the Tibetan Plateau is closely related to the onset of the East Asian summer monsoon, changes of the westerly jet path apparently critically affect the teleconnection between the climates of Asia and North Atlantic on a millennial timescale. 相似文献
92.
Hiroyuki Tsujino Mikitoshi Hirabara Hideyuki Nakano Tamaki Yasuda Tatsuo Motoi Goro Yamanaka 《Journal of Oceanography》2011,67(4):449-479
A long-term spin-up and a subsequent interannual simulation are conducted for the ocean–ice component of the climate model
intercomparison project (CMIP)-class earth system model of the Japan Meteorological Agency/Meteorological Research Institute.
This experiment has three purposes: first is to assess the ability of our model with the Coordinated Ocean–ice Reference Experiments
(COREs) forcing in reproducing the present ocean-climate; second is to understand the ocean-climate variability for the past
60 years; third is to present an example of evaluating an ocean–ice interannual variability simulation. The Pacific Ocean
is focused on for the last two purposes. After integrating for about 1500 years with repeated use of a detrended CORE interannual
forcing, the model reaches a quasi-steady state where the present climate is reproduced satisfactorily. Then, the interannual
variability simulation is conducted with the retrieved forcing trend and the result is analyzed. The simulation is successful
at reproducing the long-term variability in the Pacific and surrounding oceans. Brief analyses of the tropical and mid-latitude
upper layer, deep circulation, and the Arctic sea ice are presented. A caveat in treating other parts of the globe is due
to the recent intense convection in the Southern Ocean caused by a remarkably increasing trend of the Southern Hemisphere
westerly. Overall, the current simulation with our CMIP-class ocean–ice model is shown to be useful for studying the present
ocean-climate variability, specifically in the Pacific sector. It could also be used as a benchmark control experiment that
facilitates further research, model development, and intercomparison. 相似文献
93.
94.
We study the prospects for observing H2 emission during the assembly of primordial molecular cloud kernels. The primordial molecular cloud cores, which resemble those at the present epoch, can emerge around 1+ z ∼20 according to recent numerical simulations. The kernels form inside the cores, and the first stars will appear inside the kernels. A kernel typically contracts to form one of the first generation stars with an accretion rate that is as large as ∼0.01 M⊙ yr−1 . This occurs owing to the primordial abundances, which result in a kernel temperature of order 1000 K, and the collapsing kernel emits H2 line radiation at a rate ∼1035 erg s−1 . Predominantly J =5-3 ( v =0) rotational emission of H2 is expected. At redshift 1+ z ∼20 , the expected flux is ∼0.01 μJy for a single kernel. While an individual object is not observable by any facilities available in the near future, the expected assembly of primordial star clusters on subgalactic scales can result in fluxes at the sub-mJy level. This is marginally observable with ASTRO-F and ALMA. We also examine the rotational J =2-0 ( v =0) and vibrational δv =1 emission lines. The former may possibly be detectable with ALMA. 相似文献
95.
To achieve the maximum detection range for active sonars, it is desirable to maximize their acoustic power. In attempting to do so, there are two limitations which are caused by cavitation on the face of the transducer and an interaction effect between transducer elements of the array. To avoid these limitations, a method is proposed for driving the array elements in phase with a uniform velocity to yield the desired radiation. For this purpose, a sonar transducer array which has internal accelerometers for monitoring the motion of the transducer element is being developed. This paper presents an outline of this sonar array and a method of high-speed numerical calculation which was developed for the prediction of the radiation characteristics of the array using the fractional Fourier transform algorithm 相似文献
96.
97.
Kaori Nagashima Björn Löptien Laurent Gizon Aaron C. Birch Robert Cameron Sebastien Couvidat Sanja Danilovic Bernhard Fleck Robert Stein 《Solar physics》2014,289(9):3457-3481
The Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI) filtergrams, taken at six wavelengths around the Fe i 6173.3 Å line, contain information about the line-of-sight velocity over a range of heights in the solar atmosphere. Multi-height velocity inferences from these observations can be exploited to study wave motions and energy transport in the atmosphere. Using realistic convection-simulation datasets provided by the STAGGER and MURaM codes, we generate synthetic filtergrams and explore several methods for estimating Dopplergrams. We investigate at which height each synthetic Dopplergram correlates most strongly with the vertical velocity in the model atmospheres. On the basis of the investigation, we propose two Dopplergrams other than the standard HMI-algorithm Dopplergram produced from HMI filtergrams: a line-center Dopplergram and an average-wing Dopplergram. These two Dopplergrams correlate most strongly with vertical velocities at the heights of 30?–?40 km above (line center) and 30?–?40 km below (average wing) the effective height of the HMI-algorithm Dopplergram. Therefore, we can obtain velocity information from two layers separated by about a half of a scale height in the atmosphere, at best. The phase shifts between these multi-height Dopplergrams from observational data as well as those from the simulated data are also consistent with the height-difference estimates in the frequency range above the photospheric acoustic-cutoff frequency. 相似文献
98.
Christine E. Jilly Gary R. Huss Alexander N. Krot Kazuhide Nagashima Qing‐Zhu Yin Naoji Sugiura 《Meteoritics & planetary science》2014,49(11):2104-2117
Radiometric dating of secondary minerals can be used to constrain the timing of aqueous alteration on meteoritic parent bodies. Dolomite is a well‐documented secondary mineral in CM chondrites, and is thought to have formed by precipitation from an aqueous fluid on the CM parent body within several million years of accretion. The petrographic context of crosscutting dolomite veins indicates that aqueous alteration occurred in situ, rather than in the nebular setting. Here, we present 53Mn‐53Cr systematics for dolomite grains in Sutter's Mill section SM51‐1. The Mn‐Cr isotope data show well‐resolved excesses of 53Cr correlated with 55Mn/52Cr ratio, which we interpret as evidence for the in situ decay of radioactive 53Mn. After correcting for the relative sensitivities of Mn and Cr using a synthetic Mn‐ and Cr‐bearing calcite standard, the data yield an isochron with slope corresponding to an initial 53Mn/55Mn ratio of 3.42 ± 0.86 × 10?6. The reported error includes systematic uncertainty from the relative sensitivity factor. When calculated relative to the U‐corrected Pb‐Pb absolute age of the D'Orbigny angrite, Sutter's Mill dolomites give a formation age between 4564.8 and 4562.2 Ma (2.4–5.0 Myr after the birth of the solar system). This age is contemporaneous with previously reported ages for secondary carbonates in CM and CI chondrites. Consistent carbonate precipitation ages between the carbonaceous chondrite groups suggest that aqueous alteration was a common process during the early stages of parent body formation, probably occurring via heating from internal 26Al decay. The high‐precision isochron for Sutter's Mill dolomite indicates that late‐stage processing did not reach temperatures that were high enough to further disturb the Mn‐Cr isochron. 相似文献
99.
100.