共查询到16条相似文献，搜索用时 359 毫秒
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本文采用特征线方法和激波装配法,对磁流体中间激波在行星际空间的演化过程进行数值模拟。主要结论如下:（1） 2→4型中间激波通过向下游发出后向慢压缩波使下游态磁场减幅,通过向上游发出前向快压缩波使上游态磁场增幅,以致2→4型中间激波迅速经导灭激波向慢激波转化;所发出的前向快压缩波经非线性变陡形成快激波。（2）1→3型中间激波首先通过向下游发出前向慢稀疏波而很快变成1→3=4型临界中间激波,并瞬间转变为由前向快激波和前向2→4型中间激波构成的激波系统。其中,2→4型中间激波可在其前导快激波的下游传播较远的距离,有可能为 IAU 附近的飞船观测到,但最终导灭激波转变为慢激波。 相似文献
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慢激波的演化受其上游介质性质的制约，在等离子体热压与磁压之比β值和离子、电子温度比Ｔｉ／Ｔｅ大于１的介质中不利于慢波变陡形成慢激波。由飞船ＨｅｌｉｏｓＡ，Ｂ探测资料看出，在日心距０．３-１．０ＡＵ区间只有慢速太阳风流中存在有利于慢激波形成的条件。但理论计算和飞船观测指出，在快激波下游流场中β值和Ｔｉ／Ｔｅ都增大，因而在上述区间不论何种流速的太阳风中当有快激波经过后其下游流场内很难形成慢激波。 相似文献
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从ＭＨＤＲａｎｋｉｎｅ－Ｈｕｇｏｎｉｏｔ关系出发，导出激波下游磁能、内能和动能相对上游的增长因子，它们依赖于上游的激波角、等离子体β值和激波强度．对这些因子分析得出：１．由于行星际存在大尺度螺旋磁场，使激波而不同部位能量转换率不同，导致激波面西侧为强磁场区；２．磁能、内能转换与介质流速无关，动能转换与流速呈线性关系；３．在激波驱动过程中，能量通过后向激波输入到前、后向激波间的相互作用区；４．行星际激波能量转换以法向动能为主，随着激波向外传播介质β值不断增大，法向动能增长因子不断减小，致使激波和太阳风介质的相互作用不断减弱． 相似文献
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１９９１年７月－１９９２年６月，中、美两国合作在青藏高原架设了１１个宽频带数字记录的ＰＡＳＳＣＡＬ临时地震台站，它们分布在青藏公路沿线和青藏高原东部地区．利用这些台站记录到的高质量数据，对远震的ＳＫＳ波进行分析和计算，在多数台站观测到了ＳＫＳ波分裂的现象．用ＳＣ方法计算了青藏高原所记录到的ＳＫＳ波分裂的参量，即快波偏振方向φ和快、慢波的到时差δｔ，探求台站下地幔介质的各向异性．φ从南（拉萨）往北（至格尔木）有一趋势变化，从南边的北东方向渐变至北边的近东西方向．快、慢波的到时差在高原上向北渐渐变大，在不冻泉达到最大；再往北至格尔木又迅速减小．认为在印度板块和欧亚大陆的碰撞挤压下，雅鲁藏布江以北青藏高原下面的上地幔物质在区域构造应力场的作用下，沿东西方向发生形变以至流动，它使上地幔中橄榄岩的晶格排列方向平行于物质形变或流动的方向． 相似文献
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从Ｒａｎｋｉｎｅ－Ｈｕｇｏｎｉｏｔ关系出发，以激波切向磁场ξ、上游激波角θ１和等离子体β１值为参数研究各类激波解的特性及相互关系，阐明各类激波强度随介质β值的变化规律．结果指出：（１）在ξ＜－１的Ⅰｂ型中间激波区和ξ＞４的快激波区存在双解；（２）慢激波可以直接和中间激波连接，但不能和快激波直接连接；（３）各类激波强度（用激波密度比衡量）随β１值均有变化：Ⅰｂ型中间激波上支随β１值增加而下降，下支则上升；Ⅰａ型中间激波和慢激波都随β１值增加而下降；快激波双解区上支随β１值增加而下降。下支上升；快激波在１＜ξ＜４区间的解随β１值增加而上升。 相似文献
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１９９２年１月海南省东方县发生小震群活动，本文利用在震中附近设立的５台ＤＣＳ－３０２数字磁带加速度地震仪记录的近场资料，进行了剪切波分裂的研究采用相关函数方法，通过对１８个做了精确定位的地震事件共４２条有效记录的分析，计算出了快剪切波的偏振方向为１１３°±１８Ｏ°，慢剪切波的时间延迟为（３．１±１．１）ｍｓ／ｋｍ，裂隙密度的平均值为０．００９７±０．００３３．结合该地区的地震活动性，分析了区域应力变化对时间延迟的影响，并根据ＥＤＡ理论讨论了分裂剪切波的时间延迟的变化特征，发现快、慢剪切波的到时差（时间延迟）随地震活动性及应力积累而变化，并推断出该区的主压应力场为北西西方向． 相似文献
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本文测定了2013年4月20日芦山MS7.0地震震源区及其附近台站的S波分裂参数,包括快波偏振方向和慢波延迟时间,最终得到了40个台站的S波分裂结果．结果显示:在地震主破裂区内观测到的快波优势取向为NE向,与余震分布的长轴方向一致;位于双石—大川断裂以西台站的快波偏振优势方向为NW向,与区域最大主压应力轴方向一致;位于荥经断裂附近台站的快波偏振优势方向为NW向,与该断裂走向一致．快波偏振优势方向随时间的变化结果显示:主震前位于地震破裂区附近的TQU和BAX台站的快波偏振优势方向均呈NE向;主震后TQU台站的快波偏振优势方向为近EW向,而BAX台站的快波偏振优势方向则不突出,反映出芦山地震主震前快波偏振方向受控于龙门山断裂带,而主震后受构造应力场的作用更加明显．此外,各台站的慢波延迟时间为1.25—5.40ms/km,在余震覆盖密集区域,台站的慢波延迟时间均大于3.0ms/km,反映出震源区的各向异性程度较强．芦山主震后,各台站的延迟时间随时间变化持续减小,反映出震源区地壳应力随余震活动逐渐减小． 相似文献
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It is well known that most MHD shocks observed within 1 AU are MHD fast shocks. Only a very limited number of MHD slow shocks are observed within 1 AU. In order to understand why there are only a few MHD slow shocks observed within 1 AU, we use a one-dimensional, time-dependent MHD code with an adaptive grid to study the generation and evolution of interplanetary slow shocks (ISS) in the solar wind. Results show that a negative, nearly square-wave perturbation will generate a pair of slow shocks (a forward and a reverse slow shock). In addition, the forward and the reverse slow shocks can pass through each other without destroying their characteristics, but the propagating speeds for both shocks are decreased. A positive, square-wave perturbation will generate both slow and fast shocks. When a forward slow shock (FSS) propagates behind a forward fast shock (FFS), the former experiences a decreasing Mach number. In addition, the FSS always disappears within a distance of 150R⊙ (where R⊙ is one solar radius) from the Sun when there is a forward fast shock (with Mach number \geq1.7) propagating in front of the FSS. In all tests that we have performed, we have not discovered that the FSS (or reverse slow shock) evolves into a FFS (or reverse fast shock). Thus, we do not confirm the FSS-FFS evolution as suggested by Whang (1987). 相似文献
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S. A. Grib 《Geomagnetism and Aeronomy》2012,52(8):1113-1116
The collision of a solar wind tangential discontinuity with the bow shock and magnetopause is considered in the scope of an MHD approximation. Using MHD methods of trial calculations and generalized shock polars, it has been indicated that a fast shock refracted into the magnetosheath originates when density increases across a tangential discontinuity and a fast rarefaction wave is generated when density decreases at this discontinuity. It has been indicated that a shock front shift under the action of collisions with a tangential discontinuity is experimentally observed and a fast bow shock can be transformed into a slow shock. Using a specific event as an example, it has been demonstrated that solar wind tangential discontinuity affects the geomagnetic field behavior. 相似文献
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采用二维理想MHD模型，分别在日球赤道面（二维二分量模型）和日球子午面（二维 三分量模型）内研究太阳风中纯速度增幅扰动的演化. 结果表明，该扰动在向外传播的过程 中逐渐演化为双重激波对，即由4个激波组成的激波系统. 该4个激波按离太阳由近及远依次 为后向快激波、后向慢激波、前向慢激波和前向快激波. 双重激波对在子午面内相对扰动源 中心法线基本对称，而在赤道面内则不对称：扰动源中心法线西侧双重激波对结构更为明显 ，所跨经度范围宽于东侧. 初步分析表明，行星际磁场的螺旋结构是产生日球赤道面内双重 激波对结构东西不对称性的主要原因. 相似文献
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In situ measurements of the solar wind largely cover more than two solar magnetic activity cycles, namely 20 and 21. This is a very appealing opportunity to study the influence of the activity cycle on the behaviour of the solar wind parameters. As a matter of fact, many authors so far have studied this topic comparing the long-term magnetic field and plasma averages. However, when the average values are evaluated on a data sample whose duration is comparable with (or even longer than) the solar rotation period we lose information about the contribution due to the fast and the slow solar wind components. Thus, discriminating in velocity plays a key role in understanding solar cycle effects on the solar wind. Based on these considerations, we performed a separate analysis for fast and slow wind, respectively. In particular, we found that: (a) fast wind carries a slightly larger momentum flux density at 1 AU, probably due to dynamic stream-stream interaction; (b) proton number density in slow wind is more cycle dependent than in fast wind and decreases remarkably across solar maximum; (c) fast wind generally carries a magnetic field intensity stronger than that carried by the slow wind; (d) we found no evidence for a positive correlation between velocity and field intensity as predicted by some theories of solar wind acceleration; (e) our results would support an approximately constant divergence of field lines associated with corotating high-velocity streams. 相似文献