Pub Date : 2017-03-10DOI: 10.3724/SP.J.1226.2018.00379
Yinhuan Ao, Zhaoguo Li
{"title":"Numerical simulation of the climate effect of high-altitude lakes in the Tibetan Plateau","authors":"Yinhuan Ao, Zhaoguo Li","doi":"10.3724/SP.J.1226.2018.00379","DOIUrl":"https://doi.org/10.3724/SP.J.1226.2018.00379","url":null,"abstract":"","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"76 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"90243650","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We investigated the distribution of the collapsed buildings due to the 2016 Kumamoto earthquakes in the area along the Akitsu river. A Mj6.5 foreshock and Mj7.3 mainshock occurred within 28 hours. The spatial pattern of collapsed buildings from the foreshock and mainshock were similar and the isolated areas resemble islands. Since the surface rupture occurred only during the mainshock, it is unlikely that the presence of the surface rupture generated the similar damage patterns for the foreshock and mainshock in Mashiki. The most severely damaged areas are located in the lowest river terrace. The isolated islands correspond to the locations of built areas constructed during the Meiji era. The cause of the damage islands is likely to be a combination of the subsurface soil structure and age of buildings.
{"title":"Damage Islands in Mashiki Town from the 2016 Kumamoto Earthquakes","authors":"M. Yamada","doi":"10.5610/JAEE.17.5_38","DOIUrl":"https://doi.org/10.5610/JAEE.17.5_38","url":null,"abstract":"We investigated the distribution of the collapsed buildings due to the 2016 Kumamoto earthquakes in the area along the Akitsu river. A Mj6.5 foreshock and Mj7.3 mainshock occurred within 28 hours. The spatial pattern of collapsed buildings from the foreshock and mainshock were similar and the isolated areas resemble islands. Since the surface rupture occurred only during the mainshock, it is unlikely that the presence of the surface rupture generated the similar damage patterns for the foreshock and mainshock in Mashiki. The most severely damaged areas are located in the lowest river terrace. The isolated islands correspond to the locations of built areas constructed during the Meiji era. The cause of the damage islands is likely to be a combination of the subsurface soil structure and age of buildings.","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"150 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89924423","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Rupture process of the 2016 Meinong, Taiwan, earthquake and its effects on strong ground motions","authors":"Hongqi Diao, Hiroaki Kobayashi, K. Koketsu","doi":"10.1785/0120170193","DOIUrl":"https://doi.org/10.1785/0120170193","url":null,"abstract":"","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"141 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"80126779","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2017-03-10DOI: 10.3997/2352-8265.20140222
L. Cordrie, H. Mikada, J. Takekawa
The location of the hypocenter of an earthquake as well as the determination of the source parameters have shown some limitations in the past. The actual studies often neglect the tailing of the waveform to concentrate on the first waves arrivals and the inversion methods often need a precise distribution of aftershocks to locate the fault plane. Using former models of fault slip propagation, we produce synthetic waveforms related to different fault geometries. The inversion method will be adapted to analyze the total waveform and, using a higher number of seismograms, will give back the source parameters of the studied earthquake. The different geometries of slip models give back precise waveforms and the flexibility of the code should be an advantage to future inversion processes of earthquake location. The improvements of the fault models and the inversion method are discussed through this paper.
{"title":"Waveform-based Gradient method for estimating hypocenter mechanism before observing aftershocks","authors":"L. Cordrie, H. Mikada, J. Takekawa","doi":"10.3997/2352-8265.20140222","DOIUrl":"https://doi.org/10.3997/2352-8265.20140222","url":null,"abstract":"The location of the hypocenter of an earthquake as well as the determination of the source parameters have shown some limitations in the past. The actual studies often neglect the tailing of the waveform to concentrate on the first waves arrivals and the inversion methods often need a precise distribution of aftershocks to locate the fault plane. Using former models of fault slip propagation, we produce synthetic waveforms related to different fault geometries. The inversion method will be adapted to analyze the total waveform and, using a higher number of seismograms, will give back the source parameters of the studied earthquake. The different geometries of slip models give back precise waveforms and the flexibility of the code should be an advantage to future inversion processes of earthquake location. The improvements of the fault models and the inversion method are discussed through this paper.","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"38 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"86116952","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Planetesimals are small, rocky and icy planetary bodies that formed and evolved in the early solar system. Planetesimals play at least two important roles in planetary science. First, as the first generation of planetary objects, they served as the fundamental building blocks of planets. Intermediate in size between cm-sized pebbles and 1000-km-sized planetary embryos, they represent a critical and still enigmatic stage in planetary growth. Because the formation of km-sized bodies is difficult to understand given the likelihood of erosive mutual collisions and rapid orbital evolution due to gas drag, solving this problem will provide fundamental constraints on the sizes of accreting bodies, the nature of turbulence in the nebula, and the intensity of nebular magnetic fields. Additionally, planetesimals, and their modern-day relics—asteroids, comets and Kuiper belt objects—are fascinating planetary worlds in their own right. They experienced a much broader range of thermal histories than planets; these diverse conditions produced a diversity igneous end states, from unmelted bodies, to partially melted bodies to fully molten and differentiated objects. Furthermore, their geologic evolution and internal structures were fundamentally sculpted by impacts and mutual collisions. In many ways, planetesimals are like the planets they became, but in other ways they are very unfamiliar places. In 2017 Cambridge University press published an edited volume on planetesimals, summarizing the state of knowledge of this newly energized and rapidly-changing field [1]. Here we will present a review of research on planetesimals. Iron meteorites demonstrate the existence of differentiated rocky planetesimals in the first 500,000 years after solids formed in the disk [2], and Vesta has differentiated into a metal core and silicate mantle (Raymond et al., this volume). Johansen et al. [3] suggest the icy asteroids formed between 2 to 4 My after calcium-aluminum-rich inclusions (CAIs). The breakthrough discovery of pebble accretion, which shows that pebble-sized objects accrete to form larger objects extremely efficiently through gravitational perturbation of their orbits, indicates that accretion timescale could have been as short as a few thousand years for 100 km objects [4]. This extremely short timescale supports the use of simple models that assume nearly instantaneous accretion relative to the timescale of Al heating, although pebble accretion would have continued past the point of Al activity, and coated the young planetesimals with unmelted rinds over ~1 million years [3]. The meteorite collection and the asteroid belt differ in their ratios of primitive and differentiated metal and silicate fractions compared to models of differentiation, but all also differ in their ratios of metal and silicate in the completed planets Mercury, Venus, and Earth. However, the combined effects of fluid and magma mobilization and loss and impact erosion necessarily created a br
{"title":"Planetesimals: Early differentiation and consequences for planets","authors":"L. Elkins‐Tanton, B. Weiss","doi":"10.1017/9781316339794","DOIUrl":"https://doi.org/10.1017/9781316339794","url":null,"abstract":"Planetesimals are small, rocky and icy planetary bodies that formed and evolved in the early solar system. Planetesimals play at least two important roles in planetary science. First, as the first generation of planetary objects, they served as the fundamental building blocks of planets. Intermediate in size between cm-sized pebbles and 1000-km-sized planetary embryos, they represent a critical and still enigmatic stage in planetary growth. Because the formation of km-sized bodies is difficult to understand given the likelihood of erosive mutual collisions and rapid orbital evolution due to gas drag, solving this problem will provide fundamental constraints on the sizes of accreting bodies, the nature of turbulence in the nebula, and the intensity of nebular magnetic fields. Additionally, planetesimals, and their modern-day relics—asteroids, comets and Kuiper belt objects—are fascinating planetary worlds in their own right. They experienced a much broader range of thermal histories than planets; these diverse conditions produced a diversity igneous end states, from unmelted bodies, to partially melted bodies to fully molten and differentiated objects. Furthermore, their geologic evolution and internal structures were fundamentally sculpted by impacts and mutual collisions. In many ways, planetesimals are like the planets they became, but in other ways they are very unfamiliar places. In 2017 Cambridge University press published an edited volume on planetesimals, summarizing the state of knowledge of this newly energized and rapidly-changing field [1]. Here we will present a review of research on planetesimals. Iron meteorites demonstrate the existence of differentiated rocky planetesimals in the first 500,000 years after solids formed in the disk [2], and Vesta has differentiated into a metal core and silicate mantle (Raymond et al., this volume). Johansen et al. [3] suggest the icy asteroids formed between 2 to 4 My after calcium-aluminum-rich inclusions (CAIs). The breakthrough discovery of pebble accretion, which shows that pebble-sized objects accrete to form larger objects extremely efficiently through gravitational perturbation of their orbits, indicates that accretion timescale could have been as short as a few thousand years for 100 km objects [4]. This extremely short timescale supports the use of simple models that assume nearly instantaneous accretion relative to the timescale of Al heating, although pebble accretion would have continued past the point of Al activity, and coated the young planetesimals with unmelted rinds over ~1 million years [3]. The meteorite collection and the asteroid belt differ in their ratios of primitive and differentiated metal and silicate fractions compared to models of differentiation, but all also differ in their ratios of metal and silicate in the completed planets Mercury, Venus, and Earth. However, the combined effects of fluid and magma mobilization and loss and impact erosion necessarily created a br","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"84 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87803740","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2017-03-10DOI: 10.1002/essoar.10500002.1
N. Tsutsumida, J. Kaduk
Land surface phenology (LSP) characterizes the vegetated land surface and is practical to understand terrestrial environmentals at a global scale. Regularly observed remotely sensed data such as Landsat, MODIS, and AVHRR contributes to analyze LSP spatially. However, at least two main challenges should be addressed such that (i) the spatial resolution which attributes to the data source may significantly impact to LSP estimation, and (ii) the estimated LSP may not represent the vegetated land surface well due to the mixed land cover. Previous studies have shown that the estimation of LSP from different data is not consistent due to the spatial scale of data but yet fully linked with the mixed land cover problem. Thus, in this study, we attempt to analyze the impact of spatial scale issue to the estimated LSP in homogenous land cover areas. We use freely available remotely sensed data with different spatial resolution such as Landsat (30m), MODIS (250m, 500m, 1km), and GIMMS3g (8km) and estimate phenological indices for each. As land cover description differs among data products, land cover classes are aggregated into 12 classes globally from major global land cover producs (GLCC, GLC2000, and globcover), then spatially homogenuous land cover are only picked up. Phenological indices such as the magnitude and the peak of DOY are calculated by harmonic analysis to compare results among different spatial scales. The variability of phenological indices is explored according to the different spatial scale under the condition of homogenuous land cover. It is expected to model such variability to overcome the spatial scale impact and such characteristics depending on the spatial scale should be taken into account when considering LSP from satellite.
{"title":"Impact of spatial scale for phenological indices derived from remotely sensed data","authors":"N. Tsutsumida, J. Kaduk","doi":"10.1002/essoar.10500002.1","DOIUrl":"https://doi.org/10.1002/essoar.10500002.1","url":null,"abstract":"Land surface phenology (LSP) characterizes the vegetated land surface and is practical to understand terrestrial environmentals at a global scale. Regularly observed remotely sensed data such as Landsat, MODIS, and AVHRR contributes to analyze LSP spatially. However, at least two main challenges should be addressed such that (i) the spatial resolution which attributes to the data source may significantly impact to LSP estimation, and (ii) the estimated LSP may not represent the vegetated land surface well due to the mixed land cover. Previous studies have shown that the estimation of LSP from different data is not consistent due to the spatial scale of data but yet fully linked with the mixed land cover problem. Thus, in this study, we attempt to analyze the impact of spatial scale issue to the estimated LSP in homogenous land cover areas. We use freely available remotely sensed data with different spatial resolution such as Landsat (30m), MODIS (250m, 500m, 1km), and GIMMS3g (8km) and estimate phenological indices for each. As land cover description differs among data products, land cover classes are aggregated into 12 classes globally from major global land cover producs (GLCC, GLC2000, and globcover), then spatially homogenuous land cover are only picked up. Phenological indices such as the magnitude and the peak of DOY are calculated by harmonic analysis to compare results among different spatial scales. The variability of phenological indices is explored according to the different spatial scale under the condition of homogenuous land cover. It is expected to model such variability to overcome the spatial scale impact and such characteristics depending on the spatial scale should be taken into account when considering LSP from satellite.","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"49 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"91045378","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
M. Araki, S. Takano, N. Sakai, S. Yamamoto, T. Oyama, N. Kuze, K. Tsukiyama
the two states. In the present observations, the Ka = 0 line of para species of l-C6H2 was detected, although the detection was limited for the Ka = 1 line of ortho species so far except for IRC+10216. The column densities of the ortho and para species of l-C6H2 were independently obtained to be 1.3 × 10 11 and 0.6 × 10 11 cm −2 , respectively. C7H was detected for the first time except for IRC+10216. The column density of C7H was estimated to be 6.2 × 10 10 cm −2 from the J = 24.5‒23.5 and 25.5‒24.5 lines. These results of detections would
{"title":"Detections of Long Carbon Chains CH 3 CCCCH, C 6 H, linear -C 6 H 2 and C 7 H in the Low-Mass Star Forming Region L1527","authors":"M. Araki, S. Takano, N. Sakai, S. Yamamoto, T. Oyama, N. Kuze, K. Tsukiyama","doi":"10.15278/ISMS.2017.TA06","DOIUrl":"https://doi.org/10.15278/ISMS.2017.TA06","url":null,"abstract":"the two states. In the present observations, the Ka = 0 line of para species of l-C6H2 was detected, although the detection was limited for the Ka = 1 line of ortho species so far except for IRC+10216. The column densities of the ortho and para species of l-C6H2 were independently obtained to be 1.3 × 10 11 and 0.6 × 10 11 cm −2 , respectively. C7H was detected for the first time except for IRC+10216. The column density of C7H was estimated to be 6.2 × 10 10 cm −2 from the J = 24.5‒23.5 and 25.5‒24.5 lines. These results of detections would","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"22 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84688399","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
M. Nakano, A. Wada, M. Sawada, Hiromasa Yoshimura, R. Onishi, Shintaro Kawahara, W. Sasaki, T. Nasuno, M. Yamaguchi, Takeshi Iriguchi, M. Sugi, Yoshiaki Takeuchi
Recent advances in high-performance computers facilitate operational numerical weather prediction by global hydrostatic atmospheric models with horizontal resolutions of ∼ 10 km. Given further advances in such computers and the fact that the hydrostatic balance approximation becomes invalid for spatial scales < 10 km, the development of global nonhydrostatic models with high accuracy is urgently required. The Global 7 km mesh nonhydrostatic Model Intercomparison Project for improving TYphoon forecast (TYMIPG7) is designed to understand and statistically quantify the advantages of high-resolution nonhydrostatic global atmospheric models to improve tropical cyclone (TC) prediction. A total of 137 sets of 5-day simulations using three next-generation nonhydrostatic global models with horizontal resolutions of 7 km and a conventional hydrostatic global model with a horizontal resolution of 20 km were run on the Earth Simulator. The three 7 km mesh nonhydrostatic models are the nonhydrostatic global spectral atmospheric Double Fourier Series Model (DFSM), the Multi-Scale Simulator for the Geoenvironment (MSSG) and the Nonhydrostatic ICosahedral Atmospheric Model (NICAM). The 20 km mesh hydrostatic model is the operational Global Spectral Model (GSM) of the Japan Meteorological Agency. Compared with the 20 km mesh GSM, the 7 km mesh models reduce systematic errors in the TC track, intensity and wind radii predictions. The benefits of the multi-model ensemble method were confirmed for the 7 km mesh nonhydrostatic global models. While the three 7 km mesh models reproduce the typical axisymmetric mean inner-core structure, including the primary and secondary circulations, the simulated TC structures and their intensities in each case are very different for each model. In addition, the simulated track is not consistently better than that of the 20 km mesh GSM. These results suggest that the development of more sophisticated initialization techniques and model physics is needed to further improve the TC prediction.
{"title":"Global 7-km mesh nonhydrostatic Model Intercomparison Project for improving TYphoon forecast (TYMIP-G7)","authors":"M. Nakano, A. Wada, M. Sawada, Hiromasa Yoshimura, R. Onishi, Shintaro Kawahara, W. Sasaki, T. Nasuno, M. Yamaguchi, Takeshi Iriguchi, M. Sugi, Yoshiaki Takeuchi","doi":"10.5194/gmd-2016-184","DOIUrl":"https://doi.org/10.5194/gmd-2016-184","url":null,"abstract":"Recent advances in high-performance computers facilitate operational numerical weather prediction by global hydrostatic atmospheric models with horizontal resolutions of ∼ 10 km. Given further advances in such computers and the fact that the hydrostatic balance approximation becomes invalid for spatial scales < 10 km, the development of global nonhydrostatic models with high accuracy is urgently required. The Global 7 km mesh nonhydrostatic Model Intercomparison Project for improving TYphoon forecast (TYMIPG7) is designed to understand and statistically quantify the advantages of high-resolution nonhydrostatic global atmospheric models to improve tropical cyclone (TC) prediction. A total of 137 sets of 5-day simulations using three next-generation nonhydrostatic global models with horizontal resolutions of 7 km and a conventional hydrostatic global model with a horizontal resolution of 20 km were run on the Earth Simulator. The three 7 km mesh nonhydrostatic models are the nonhydrostatic global spectral atmospheric Double Fourier Series Model (DFSM), the Multi-Scale Simulator for the Geoenvironment (MSSG) and the Nonhydrostatic ICosahedral Atmospheric Model (NICAM). The 20 km mesh hydrostatic model is the operational Global Spectral Model (GSM) of the Japan Meteorological Agency. Compared with the 20 km mesh GSM, the 7 km mesh models reduce systematic errors in the TC track, intensity and wind radii predictions. The benefits of the multi-model ensemble method were confirmed for the 7 km mesh nonhydrostatic global models. While the three 7 km mesh models reproduce the typical axisymmetric mean inner-core structure, including the primary and secondary circulations, the simulated TC structures and their intensities in each case are very different for each model. In addition, the simulated track is not consistently better than that of the 20 km mesh GSM. These results suggest that the development of more sophisticated initialization techniques and model physics is needed to further improve the TC prediction.","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"37 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"91502193","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
AbstractIn this study, the 2D and 3D cloud-resolving model simulations of the Tropical Rainfall Measuring Mission (TRMM) Kwajalein Experiment (KWAJEX) are compared to study the impact of dimensionality on barotropic processes during tropical convective development. Barotropic conversion of perturbation kinetic energy is associated with vertical transport of horizontal momentum under vertical shear of background horizontal winds. The similarities in both 2D and 3D model simulations show that 1) vertical wind shear is a necessary condition for barotropic conversion, but it does not control the barotropic conversion; 2) the evolution of barotropic conversion is related to that of the vertical transport of horizontal momentum; and 3) the tendency of vertical transport of horizontal momentum is mainly determined by the covariance between horizontal wind and the cloud hydrometeor component of buoyancy. The differences between the 2D and 3D model simulations reveal that 1) the barotropic conversion has shorter t...
{"title":"The Impact of Dimensionality on Barotropic Processes during KWAJEX","authors":"Xiaofan Li","doi":"10.1175/JAS-D-16-0184.1","DOIUrl":"https://doi.org/10.1175/JAS-D-16-0184.1","url":null,"abstract":"AbstractIn this study, the 2D and 3D cloud-resolving model simulations of the Tropical Rainfall Measuring Mission (TRMM) Kwajalein Experiment (KWAJEX) are compared to study the impact of dimensionality on barotropic processes during tropical convective development. Barotropic conversion of perturbation kinetic energy is associated with vertical transport of horizontal momentum under vertical shear of background horizontal winds. The similarities in both 2D and 3D model simulations show that 1) vertical wind shear is a necessary condition for barotropic conversion, but it does not control the barotropic conversion; 2) the evolution of barotropic conversion is related to that of the vertical transport of horizontal momentum; and 3) the tendency of vertical transport of horizontal momentum is mainly determined by the covariance between horizontal wind and the cloud hydrometeor component of buoyancy. The differences between the 2D and 3D model simulations reveal that 1) the barotropic conversion has shorter t...","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"153 10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"91525929","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The measurement of the H/H2 brightness ratio of giant planets’ far-ultraviolet (FUV) aurora is a proxy for precipitating soft (a few 10s keV) electrons. We investigate the relevance of this H/H2 indicator with the Jupiter auroral observations obtained by the Hubble Space Telescope. The H/H2 ratio does not show any clear relationship with the FUV color ratio which is sensitive to more energetic electrons. Compared to the same analysis applied for Saturn’s aurora, the relationship for Jupiter mainly shows decreasing flux with increasing energy without acceleration features.
{"title":"Auroral electron energy estimation using the H/H2 brightness ratio applied to Jupiter","authors":"C. Tao, L. Lamy, R. Prangé, N. André, S. Badman","doi":"10.1553/pre8s139","DOIUrl":"https://doi.org/10.1553/pre8s139","url":null,"abstract":"The measurement of the H/H2 brightness ratio of giant planets’ far-ultraviolet (FUV) aurora is a proxy for precipitating soft (a few 10s keV) electrons. We investigate the relevance of this H/H2 indicator with the Jupiter auroral observations obtained by the Hubble Space Telescope. The H/H2 ratio does not show any clear relationship with the FUV color ratio which is sensitive to more energetic electrons. Compared to the same analysis applied for Saturn’s aurora, the relationship for Jupiter mainly shows decreasing flux with increasing energy without acceleration features.","PeriodicalId":14836,"journal":{"name":"Japan Geoscience Union","volume":"32 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2017-03-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82038375","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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