排序方式： 共有135条查询结果，搜索用时 109 毫秒
41.
Y. Futaana S. Barabash M. Holmström E. Kallio H. Gunell R. Lundin M. Yamauchi J.D. Winningham J.R. Sharber A.J. Coates D.O. Kataria P. Riihelä H. Koskinen J. Luhmann D. Williams C.C. Curtis B.R. Sandel M. Carter A. Fedorov S. Orsini M. Maggi P. Bochsler J. Woch K. Asamura 《Icarus》2006,182(2):413-423
The Neutral Particle Detector (NPD), an Energetic Neutral Atom (ENA) sensor of the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) on board Mars Express, detected intense fluxes of ENAs emitted from the subsolar region of Mars. The typical ENA fluxes are (4-7) × 105 cm−2 sr−1 s−1 in the energy range 0.3-3 keV. These ENAs are likely to be generated in the subsolar region of the martian exosphere. As the satellite moved away from Mars, the ENA flux decreased while the field of view of the NPD pointed toward the subsolar region. These decreases occurred very quickly with a time scale of a few tens of seconds in two thirds of the orbits. Such a behavior can be explained by the spacecraft crossing a spatially constrained ENA jet, i.e., a highly directional ENA emission from a compact region of the subsolar exosphere. This ENA jet is highly possible to be emitted conically from the subsolar region. Such directional ENAs can result from the anisotropic solar wind flow around the subsolar region, but this can not be explained in the frame of MHD models. 相似文献
42.
E. Dubinin D. Winningham J. Woch S. Barabash R. Frahm A.J. Coates J.-A. Sauvaud H. Andersson A. Grigoriev K. Asamura K.S. Hsieh H. Koskinen P. Riihelä T. Säles J. Luhmann R. Cerulli-Irelli M. Maggi D. Williams P. Wurz C. Dierker M. Carter 《Icarus》2006,182(2):343-349
The ASPERA-3 experiment onboard the Mars Express spacecraft revealed, near the wake boundary of Mars, a spatially narrow, strip-like plasma structure composed of magnetosheath-like electrons and planetary ions. The peak electron energy often exceeds the peak energy at the bow shock that indicates a significant heating (acceleration) during the structure formation. It is shown that this structure is formed during efficient plasma penetration into the martian magnetosphere in the region near the terminator. The penetration of sheath electrons and their gradual heating (acceleration) is accompanied by a change of the ion composition from a solar wind plasma to a planetary plasma dominated by oxygen ions. A possible mechanism of plasma inflow to the magnetosphere is discussed. 相似文献
43.
K. Brinkfeldt H. Gunell P. C:son Brandt R.A. Frahm E. Kallio Y. Futaana R. Lundin M. Yamauchi J.R. Sharber A.J. Coates D.O. Kataria T. Säles W. Schmidt J. Luhmann D. Williams C.C. Curtis B.R. Sandel M. Carter A. Fedorov S. McKenna-Lawler R. Cerulli-Irelli P. Wurz N. Krupp M. Fränz C. Dierker 《Icarus》2006,182(2):439-447
We present measurements with an Energetic Neutral Atom (ENA) imager on board Mars Express when the spacecraft moves into Mars eclipse. Solar wind ions charge exchange with the extended Mars exosphere to produce ENAs that can spread into the eclipse of Mars due to the ions' thermal spread. Our measurements show a lingering signal from the Sun direction for several minutes as the spacecraft moves into the eclipse. However, our ENA imager is also sensitive to UV photons and we compare the measurements to ENA simulations and a simplified model of UV scattering in the exosphere. Simulations and further comparisons with an electron spectrometer sensitive to photoelectrons generated when UV photons interact with the spacecraft suggest that what we are seeing in Mars' eclipse are ENAs from upstream of the bow shock produced in charge exchange with solar wind ions with a non-zero temperature. The measurements are a precursor to a new technique called ENA sounding to measure solar wind and planetary exosphere properties in the future. 相似文献
44.
E. Kallio A. Fedorov T. Säles W. Schmidt P. Riihelä R. Lundin H. Gunell Y. Futaana M. Yamauchi J.-A. Sauvaud J.D. Winningham J.R. Sharber A.J. Coates D.O. Kataria J.G. Luhmann D. Williams C.C. Curtis B.R. Sandel M. Carter S. Orsini M. Maggi P. Bochsler J. Woch K. Asamura 《Icarus》2006,182(2):350-359
We have analysed ion escape at Mars by comparing ASPERA-3/Mars Express ion measurements and a 3-D quasi-neutral hybrid model. As Mars Express does not have a magnetometer onboard, the analysed IMA data are from an orbit when the IMF clock angle was possible to determine from the magnetic field measurements of Mars Global Surveyor. We found that fast escaping planetary ions were observed at the place which, according to the 3-D model, is anticipated to contain accelerated heavy ions originating from the martian ionosphere. The direction of the interplanetary magnetic field was found to affect noticeably which regions can be magnetically connected to Mars Express and to the overall 3-D Mars-solar wind interaction. 相似文献
45.
沪宁高速公路一次复杂性大雾过程的数值模拟试验 总被引：4，自引：0，他引：4
为探明高速公路大雾天气的成因和演变规律,揭示雾影响交通能见度的机理,本文根据布设于我国沪宁高速公路沿线的环境气象自动监测系统(AWMS)实测资料和覆盖公路周边地区的常规气象台站观测资料,筛选出2009年11月7日发生在沪宁高速公路上的一次典型复杂性大雾天气过程.在分析天气实况的基础上,应用高时空分辨率的非静力中尺度数值预报模式WRF3.1,结合NCEP 0.5°×0.5°气象再分析资料,对该过程进行了数值模拟;利用实测资料对模拟结果进行了验证,并剖析了此次复杂性大雾过程形成的动力、水汽和热力条件.研究表明:(1)本次大雾前后的天气形势相对稳定,江苏地区主要受入海反气旋西南侧东南气流影响,整个大雾过程中地面风力始终微弱,为大雾形成提供了有利的动力条件;(2)模式模拟的由大气液态含水量条件判别的成雾区分布与实测雾区范围基本吻合;(3)模式模拟的能见度与AWMS实测能见度十分接近;(4)本次大雾过程最初是团雾雏形,在夜间辐射冷却作用下,转为辐射雾,之后,来自东南海上的暖湿空气平流进入江苏陆地后,所产生的平流雾雾体与原有辐射雾雾体结合发展为范围更大的辐射平流混合雾;(5)日出后短波辐射增温是此次复杂性大雾雾体得以快速消散的主要原因. 相似文献
46.
沪宁高速公路团雾发生规律及局地性分析 总被引：3，自引：1，他引：2
为探索高速公路团雾天气的发生规律和局地性特征,根据布设于中国沪宁高速公路沿线的AWMS系统实测资料,对2006—2009年期间该公路上发生的团雾和大雾过程进行了统计分析,探讨了团雾发生的气象和地形、地貌条件,并对临湖环境的公路东部路段和临江环境的中西部路段的团雾特征作了比较。研究表明：（1）沪宁高速公路上团雾和大雾的季节变化有着相似的季节分布,都是秋、冬、春季发生频率高,夏季发生频率低。（2）团雾和大雾因路段和站点不同而差异较大,大雾的分布是东少西多,团雾的分布趋势则是东部的临湖路段中有4个站点发生频率高,其余站点低,西部的临江路段则发生频率普遍高。（3）一般,团雾发生的气象条件是温度在-4~30℃,相对湿度在85%~95%,风速在3 m·s-1以内;团雾的主要发生时段在00—06时之间,通常在生成后的4 h内消散。（4）东部路段中的临湖环境,提供了团雾形成的有利条件,中西部的临江路段,则由于丘陵地形作用和水汽及气溶胶输送通道而成为团雾高发的区域。（5）在夏季大气对流运动频繁,城市近地层污染物易于扩散,雾和霾都不易形成;而冬季近地层大气对流不活跃,常不利于污染物扩散,这使得城市雾和霾的容易形成且不易消散。 相似文献
47.
选择地理位置和气候环境差异较大的环青海湖地区和环鄱阳湖地区,利用Penman-Monteith公式计算两地区近50年潜在蒸散,并分析其时空变化规律,提取影响潜在蒸散的主要气候因子,探讨两地区的气候特征差异。结果表明：近50年来,环鄱阳湖地区潜在蒸散年总量呈现逐年减少的趋势,倾向率达到-2.2 mm·a-1,环青海湖地区潜在蒸散年总量未呈现明显的变化特征,倾向率为-0.02 mm·a-1;两地区潜在蒸散年总量在空间分布上具有明显差异。在影响潜在蒸散的各主要气象因素中,日照时数、温度、风速与潜在蒸散呈正相关关系,水汽压与潜在蒸散表现为负相关关系,不同地区各气象要素对潜在蒸散的贡献大小不同,主要的影响因子是温度,其次是风速;但在局部可能出现其他气象因子的综合作用大于温度对潜在蒸散变化的影响的情况。 相似文献
48.
采用Boussinesq近似,研制了准三维、非线性、非静力的斜压数值模式。利用该模式做了背景流与海底地形对高频海洋内波影响的数值试验。本文得到的主要结论有:各数值试验初始1小时内,有适应过程,并最终形成垂直方向为单圈环流的海洋内波波包;以后进入海洋内波的演变过程,并在非线性作用下形成椭圆余弦波波包,并向孤立内波演变。当无背景流时,地形会激发出两支传播方向相反的海洋内波波包,水深大处波包传播较慢。当存在定常背景流时,在其与地形共同作用下,在地形处会激发出较强的内波波包,若地形足够陡峭,则内波波包截陷于该陡峭处,造成该处强烈的垂直运动。背景流随时间的变化会对在台阶地形跃阶处的内波波包产生不同的影响。 相似文献
49.
Rafael P. Fernandez Martin Kaufmann Beatriz M. Toselli 《Journal of Atmospheric and Solar》2009,71(8-9):805-815
The relative importance of different processes and transitions in the appearance of non-LTE populations for the fundamental levels of ozone was studied by quantifying the kinetic law of every process and transition that affect each level population. The vibrational temperatures and the relative contribution of every transition are presented as a function of altitude. The results show that the appearance of non-LTE populations for the fundamental levels is not produced by a direct imbalance between absorption and emission but as a consequence of imbalanced collisional transitions provoked by the overpopulation of O3(0 v2 0) levels. This fact confirms that the relaxation cascade drives through the bending mode ν2. 相似文献
50.
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