Influence of housing and urban development on debris flow flooding and deposition   总被引：2，自引：2，他引：0  

Kana NAKATANI  Yuki OKUYAMA  Yuji HASEGAWA  Yoshifumi SATOFUKA  Takahisa MIZUYAMA 《山地科学学报》2013,10(2):273-280

Debris flows form deposits when they reach an alluvial fan until they eventually stop.However,houses located in the alluvial fan might affect the debris flow flooding and deposition processes.Few previous studies have considered the effects of houses on debris flow flooding and deposition.This study conducted model experiments and numerical simulations using the Kanako2D debris flow simulator to determine the influence of houses on debris flow flooding and deposition.The model experiments showed that when houses are present,the debris flow spreads widely in the cross direction immediately upstream of the houses,especially when the flow discharge is large or the grain size is small.Houses located in the alluvial fan also influence the deposition area.The presence of houses led to flooding and deposition damage in some places and reduced the damage in others.The simulation also demonstrated the influence of houses.Both the model experiment and the simulation showed that houses change the flooding and deposition areas.  相似文献   

Numerical modelling study on the flexural uplift of the Transantarctic Mountains     

Tadashi Yamasaki  Hideki Miura  Yoshifumi Nogi 《Geophysical Journal International》2008,174(1):377-390

In this study, based on a 2-D thermomechanical finite element model, the uplift of the Transantarctic Mountains (TAM) is discussed in relation to the flexural uplift of a rheologically layered lithosphere, which is described by Vening-Meinesz's cantilever kinematics. The general model behaviour shows that the thickness of the crust and the geothermal gradient in the lithosphere are the principal factors in controlling the effective elastic thickness ( T _e). Although T _e is also significantly dependent on the magnitude of the uplift and the wet or dry rheological condition of rocks, these two factors do not have a dominant influence on the half-wavelength of the TAM. The model with a plausible crustal structure beneath Antarctica shows that the thermal structure beneath East Antarctica is the critical factor, controlling the half-wavelength of the TAM. If there is a significant radiogenic heat source in the Antarctic lithosphere, T _e beneath East Antarctica is estimated to be 50 km, at most, and the lithosphere has no potential to explain an exceptionally large-scale half-wavelength of the TAM. Even for the model without a heat source, if East Antarctica is significantly thermally influenced by West Antarctica, T _e is estimated to be about 60 km, and it is difficult to reproduce the half-wavelength of the TAM. Contrarily, when a radiogenic heat source is absent and the thermal structure beneath East Antarctica is not significantly affected by that beneath West Antarctica, the rheological structure beneath East Antarctica has the potential to reproduce the half-wavelength of the TAM ( T _e∼ 100 km). Thus, the presence of a radiogenic heat source in the crust and mantle and the thermal influence of West Antarctica on East Antarctica are crucial factors in the reproduction of the half-wavelength found in the TAM.  相似文献   

Fifteen years progress of the TRITON array in the Western Pacific and Eastern Indian Oceans     

Kentaro Ando  Yoshifumi Kuroda  Yosuke Fujii  Tatsuya Fukuda  Takuya Hasegawa  Takanori Horii  Yasuhisa Ishihara  Yuji Kashino  Yukio Masumoto  Keisuke Mizuno  Motoki Nagura  Iwao Ueki 《Journal of Oceanography》2017,73(4):403-426

The Triangle Trans‐Ocean Buoy Network (TRITON) project by the Japan Agency for Marine-Earth Science and Technology began with deployment in the western tropical Pacific Ocean in 1998 and has shifted to steady, long-term observations since 1999. After on-site inter-comparison with the Autonomous Temperature Line Acquisition System mooring system of the Tropical Atmosphere and Ocean (TAO) array by the National Oceanic and Atmospheric Administration, the TRITON array became the international TAO/TRITON array in 2000 as a key component of the Global Ocean and Climate Observing Systems. The TAO/TRITON array took over from the TAO array, which was developed during the Tropical Ocean and Global Atmosphere program (1985–1994), and replaced the western part of TAO with new additional real-time measurements of salinity and ocean currents. In 2001, two TRITON moorings were deployed in the eastern Indian Ocean for capturing the eastern pole of the Indian Ocean Dipole. From this initiative, the Indian Ocean Observing System (IndOOS) was designed, and the Indian Ocean mooring array (Research Moored Array for Africa–Asian–Australian Monsoon Analysis and Prediction) was developed as a key component of IndOOS. In this paper, 15 years of progress in the TRITON project in the western Pacific and eastern Indian Oceans is reviewed with regards to scientific outcomes, technological development, and collaborations with international and domestic partners. Future directions for sustainable observation in the Pacific and Indian Oceans are also discussed.  相似文献   

First observation of energetic neutral atoms in the Venus environment     

A. Galli  P. Wurz  S. Barabash  Y. Futaana  H. Gunell  R. Lundin  K. Brinkfeldt  N. Krupp  W. Baumjohann  T.L. Zhang  A.J. Coates  D.O. Kataria  K.C. Hsieh  J.A. Sauvaud  C. Mazelle  M. Grande  T. Sales  P. Riihela  J. Kozyra  S. McKenna-Lawlor  R. Cerulli-Irelli  A. Milillo  E. Roelof  C.T. Russell  D. Winningham  J. Scherrer 《Planetary and Space Science》2008,56(6):807-811

The ASPERA-4 instrument on board the Venus Express spacecraft offers for the first time the possibility to directly measure the emission of energetic neutral atoms (ENAs) in the vicinity of Venus. When the spacecraft is inside the Venus shadow a distinct signal of hydrogen ENAs usually is detected. It is observed as a narrow tailward stream, coming from the dayside exosphere around the Sun direction. The intensity of the signal reaches several , which is consistent with present theories of the plasma and neutral particle distributions around Venus.  相似文献   

Heavy ion escape from Mars, influence from solar wind conditions and crustal magnetic fields     

Hans Nilsson  Niklas J.T. Edberg  Stas Barabash  Yoshifumi Futaana  Andrei Fedorov 《Icarus》2011,215(2):475-484

We have used more than 4 years of Mars Express ion data to estimate the escape of heavy ions ( and ) from Mars. To take the limited field of view of the instrument into account, the data has been binned into spatial bins and angular bins to create average distribution functions for different positions in the near Mars space. The net escape flux for the studied low solar activity period, between May 2007 and May 2011, is 2.0 ± 0.2 × 10²⁴ s⁻¹. The escape has been calculated independently for four different quadrants in the Y_MSO − Z_MSO plane, south, dusk, north and dawn. Escape is highest from the northern and dusk quadrants, 0.6 ± 0.1 × 10²⁴ s⁻¹, and smallest from the south and dawn quadrants, 0.4 ± 0.1 × 10²⁴ s⁻¹. The flux ratio of molecular ( and ) to O⁺ ions is 0.9 ± 0.1, averaged over all quadrants. The flux difference between the north and south quadrants is statistically significant, and is presumed to be due to the presence of significant crustal magnetic fields in the southern hemisphere, reducing the outflow. The difference between the dawn and dusk quadrants is likely due to the magnetic tension associated with the nominal Parker angle spiral, which should lead to higher average magnetic tension on the dusk side. The escape increases during periods of high solar wind flux and during times when co-rotating interaction regions (CIR) affect Mars. In the latter case the increase is a factor 2.4-2.9 as compared to average conditions.  相似文献   

First ENA observations at Mars: Charge exchange ENAs produced in the magnetosheath     

H. Gunell  K. Brinkfeldt  P. C:son Brandt  E. Kallio  Y. Futaana  H. Andersson  A. Grigoriev  R.A. Frahm  J.R. Scherrer  D.R. Linder  T. Säles  W. Schmidt  J. Kozyra  E. Roelof  S. Livi  K.C. Hsieh  M. Grande  J.-A. Sauvaud  J.-J. Thocaven  S. Orsini  M. Maggi  P. Bochsler  J. Woch  K. Asamura 《Icarus》2006,182(2):431-438

Measurements of energetic neutral atoms (ENA) generated in the magnetosheath at Mars are reported. These ENAs are the result of charge exchange collisions between solar wind protons and neutral oxygen and hydrogen in the exosphere of Mars. The peak of the observed ENA flux is . For the case studied here, i.e., the passage of Mars Express through the martian magnetosheath around 20:15 UT on 3 May 2004, the measurements agree with an analytical model of the ENA production at the planet. It is possible to find parameter values in the model such that the observed peak in the ENA count rate during the spacecraft passage through the magnetosheath is reproduced.  相似文献   

Suzaku observations of charge exchange emission from solar system objects     

Y. Ezoe  R. Fujimoto  N.Y. Yamasaki  K. Mitsuda  T. Ohashi  K. Ishikawa  S. Oishi  Y. Miyoshi  N. Terada  Y. Futaana  F.S. Porter  G.V. Brown 《Astronomische Nachrichten》2012,333(4):319-323

Recent results of charge exchange emission from solar system objects observed with the Japanese Suzaku satellite are reviewed. Suzaku is of great importance to investigate diffuse X‐ray emission like the charge exchange from planetary exospheres and comets. The Suzaku studies of Earth's exosphere, Martian exosphere, Jupiter's aurorae, and comets are overviewed (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Advanced method to derive the IMF direction near Mars from cycloidal proton distributions     

M. Yamauchi  Y. Futaana  E. Kallio  R. Lundin  J.D. Winningham  M. Holmström 《Planetary and Space Science》2008,56(8):1145-1154

In a previous paper, we showed a method for deriving the interplanetary magnetic field (IMF) orientation from the velocity distribution of ring-like distributed ions as measured by the Ion Mass Analyser (IMA) on board Mars Express (MEX). This method has been improved so that one can derive the IMF orientation from a very limited portion of the ring distributions, i.e., only the highest energy portion of the ring distribution. This method uses the maximum variance direction L instead of the minimum variance direction N, which are derived from manually selected ring data. Because IMA's count rate for a semi-persistent ring distribution is nearly proportional to energy squire, L is most likely aligned to the tangential direction of the ring distribution at its highest energy, and this tangential direction is parallel or anti-parallel to the electric field. A vector product of L and the solar wind direction (X) gives the IMF orientation projected to the Y-Z plane. The tilt angle of IMF toward the X direction from the Y-Z plane is the same as the angle between the X direction and the ring plane, and is obtained from two methods when the initial speed of the ring ions is estimated to be much smaller than the solar wind speed: (1) angle between the velocity of ring's maximum energy portion and the solar wind vector, and (2) energy ratio between the solar wind and the maximum energy of the ring. The present method is applied to the IMA data from 3 June 2005 (0605-0640 UT) when the Mars Global Surveyor (MGS) magnetometer data are available. Using these data, we also tried to determine the sign of the IMF direction by estimating the evolution direction of the ring ions.  相似文献   

Mars Express and Venus Express multi-point observations of geoeffective solar flare events in December 2006     

Y. Futaana  S. Barabash  S. McKenna-Lawlor  J.G. Luhmann  E. Carlsson  J.D. Winningham  P. Wurz  H. Gunell  W. Baumjohann  J.R. Sharber  H. Andersson  K. Brinkfeldt  K. Asamura  A.J. Coates  D.O. Kataria  B.R. Sandel  C. Mazelle  M. Grande  T. Sales  P. Riihela  N. Krupp  M. Fränz  S. Orsini  A. Mura  M. Maggi  P. Brandt  J. Scherrer 《Planetary and Space Science》2008,56(6):873-880

In December 2006, a single active region produced a series of proton solar flares, with X-ray class up to the X9.0 level, starting on 5 December 2006 at 10:35 UT. A feature of this X9.0 flare is that associated MeV particles were observed at Venus and Mars by Venus Express (VEX) and Mars Express (MEX), which were ∼80° and ∼125° east of the flare site, respectively, in addition to the Earth, which was ∼79° west of the flare site. On December 5, 2006, the plasma instruments ASPERA-3 and ASPERA-4 on board MEX and VEX detected a large enhancement in their respective background count levels. This is a typical signature of solar energetic particle (SEP) events, i.e., intensive MeV particle fluxes. The timings of these enhancements were consistent with the estimated field-aligned travel time of particles associated with the X9.0 flare that followed the Parker spiral to reach Venus and Mars. Coronal mass ejection (CME) signatures that might be related to the proton flare were twice identified at Venus within <43 and <67 h after the flare. Although these CMEs did not necessarily originate from the X9.0 flare on December 5, 2006, they most likely originated from the same active region because these characteristics are very similar to flare-associated CMEs observed on the Earth. These observations indicate that CME and flare activities on the invisible side of the Sun may affect terrestrial space weather as a result of traveling more than 90° in both azimuthal directions in the heliosphere. We would also like to emphasize that during the SEP activity, MEX data indicate an approximately one-order of magnitude enhancement in the heavy ion outflow flux from the Martian atmosphere. This is the first observation of the increase of escaping ion flux from Martian atmosphere during an intensive SEP event. This suggests that the solar EUV flux levels significantly affect the atmospheric loss from unmagnetized planets.  相似文献   

Horizontal structure of planetary-scale waves at the cloud top of Venus deduced from Galileo SSI images with an improved cloud-tracking technique     

Toru Kouyama  Takeshi Imamura  Masato Nakamura  Takehiko Satoh  Yoshihumi Futaana 《Planetary and Space Science》2012,60(1):207-216

An improved cloud tracking method for deriving wind velocities from successive planetary images was developed. The new method incorporates into the traditional cross-correlation method an algorithm that corrects for erroneous cloud motion vectors by re-determining the most plausible correlation peak among all of the local maxima on the correlation surface by comparing each vector with its neighboring vectors. The newly developed method was applied to the Venusian violet images obtained by the Solid State Imaging system (SSI) onboard the Galileo spacecraft during its Venus flyby. Although the results may be biased by the choice of spatial scale of atmospheric features, the cloud tracking is the most practical mean of estimating the wind velocities with extensive spatial and temporal coverage. The two-dimensional distribution of the horizontal wind vector field over 5 days was obtained. It was found from these wind maps that the solar-fixed component in 1990 was similar to that in 1982 obtained by the Pioneer Venus orbiter. The deviation of the instantaneous zonal wind field from the solar-fixed component shows a distinct wavenumber-1 structure in the equatorial region. On the assumption that this structure is a manifestation of an equatorial Kelvin wave, the phase relationship between the zonal wind and the cloud brightness suggests a short photochemical lifetime of the violet absorber. The momentum deposition by this Kelvin wave, which is subject to radiative damping, would induce a westward mean-wind acceleration of ～0.3 m s^?1 per Earth day.  相似文献