...
  • 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>Space Science Reviews >Kinetic-Hydrodynamic Models of the Solar Wind Interaction with the Partially Ionized Supersonic Flow of the Local Interstellar Gas: Predictions and Interpretations of the Experimental Data
【24h】

Kinetic-Hydrodynamic Models of the Solar Wind Interaction with the Partially Ionized Supersonic Flow of the Local Interstellar Gas: Predictions and Interpretations of the Experimental Data

机译：太阳风与局部星际气体部分电离的超音速流相互作用的动力学-水动力模型：实验数据的预测和解释。

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

At present there is no doubt that the local interstellar medium (LISM) is mainly partially ionized hydrogen gas moving with a supersonic flow relative to the solar system. The bulk velocity of this flow is approximately equal ∼26 km/s. Although the interaction of the solar wind with the charged component (below plasma component) of the LISM can be described in the framework of hydrodynamic approach, the interaction of H atoms with the plasma component can be correctly described only in the framework of kinetic theory because the mean free path of H atoms in the main process of the resonance charge exchange is comparable with a characteristic length of the problem considered. Results of self-consistent, kinetic-hydrodynamic models are considered in this review paper. First, such the model was constructed by Baranov and Malama (J. Geophys. Res. 98(A9):15,157–15,163, 1993). Up to now it is mainly developed by Moscow group taking into account new experimental data obtained onboard spacecraft studying outer regions of the solar system (Voyager 1 and 2, Pioneer 10 and 11, Hubble Space Telescope, Ulysses, SOHO and so on). Predictions and interpretations of experimental data obtained on the basis of these models are presented. Kinetic models for describing H atom motion were later suggested by Fahr et al. (Astron. Astrophys 298:587–600, 1995) and Lipatov et al. (J. Geophys. Res. 103(A9):20,631–20,642, 1998). However they were not self-consistent and did not incorporate sources to the plasma component. A self-consistent kinetic-hydrodynamic model suggested by Heerikhuisen et al. (J. Geophys. Res. 111:A06110, 2006, Astrophys. J. 655:L53–L56, 2007) was not tested on the results by Baranov and Malama (J. Geophys. Res. 111:A06110, 1993) although it was suggested much later. Besides authors did not describe in details their Monte Carlo method for a solution of the H atom Boltzmann equation and did not inform about an accuracy of this method. Therefore the results of Heerikhuisen et al. (J. Geophys. Res. 111:A06110, 2006) are in open to question and will not be considered in this review paper. That is why below we will mainly consider a progress of the Moscow group on heliospheric modelling endeavours in the kinetic-hydrodynamic approach. Criticism of the models that treat interstellar hydrogen in the heliosphere as several fluids is given. It is shown that the multi-fluid models give rise to unreal results especially for distributions of neutral component parameters. Magnetohydrodynamic (MHD) modelling of the solar wind interaction with the LISM gas is also reviewed. Keywords Solar wind - Interstellar medium - Heliopause - Termination shock - Bow schock - Pickup ions - Charge exchange
机译：目前，毫无疑问，局部星际介质（LISM）主要是部分离子化的氢气，以相对于太阳系的超音速流动。该流的总速度大约等于〜26 km / s。尽管可以在流体力学方法的框架中描述太阳风与LISM的带电成分（在等离子体成分以下）的相互作用，但仅在动力学理论的框架中才能正确地描述H原子与等离子体成分的相互作用。在共振电荷交换的主要过程中，H原子的平均自由程与所考虑问题的特征长度相当。这篇评论文章考虑了自洽的动力学流体动力学模型的结果。首先，这种模型是由巴拉诺夫（Baranov）和马拉马（Malama）构建的（J. Geophys。Res。98（A9）：15,157–15,163，1993）。到目前为止，它主要是由莫斯科小组开发的，其中考虑了在航天器上获得的研究太阳系外围区域的新实验数据（旅行者1和2，先锋10和11，哈勃太空望远镜，尤利西斯，SOHO等）。介绍了基于这些模型获得的实验数据的预测和解释。 Fahr等人后来提出了描述H原子运动的动力学模型。 （Astron。Astrophys 298：587-600，1995）和Lipatov等。 （J. Geophys。Res。103（A9）：20,631–20,642，1998）。然而，它们不是自洽的，并且没有将源结合到等离子体成分中。 Heerikhuisen等人提出的自洽的动力学-流体力学模型。 （J. Geophys。Res。111：A06110，2006，Astrophys。J. 655：L53-L56，2007）并未通过Baranov和Malama的测试结果进行测试（J. Geophys。Res。111：A06110，1993）被建议很晚。此外，作者没有详细描述他们的Monte Carlo方法来求解H原子Boltzmann方程，也没有告知这种方法的准确性。因此，Heerikhuisen等人的结果。 （J. Geophys。Res。111：A06110，2006）尚待商and，本评论文件中将不考虑。这就是为什么下面我们将主要考虑莫斯科小组在动力学-流体动力学方法方面的进展的原因。批评了将几种空间流体视作太阳系中星际氢的模型。结果表明，多流体模型引起了不真实的结果，特别是对于中性成分参数的分布。还审查了太阳风与LISM气体相互作用的磁流体动力学（MHD）模型。关键词太阳风-星际介质-更年期-终止电击-弓形电击-吸收离子-电荷交换

著录项

相似文献

  • 外文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号