Fine structure of the interplanetary shock front according to measurements of the ion flux of the solar wind with high time resolution

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• 作者：V. G. Eselevich ; N. L. Borodkova ; M. V. Eselevich ; G. N. Zastenker…
• 刊名：Cosmic Research
• 出版年：2017
• 出版时间：January 2017
• 年：2017
• 卷：55
• 期：1
• 页码：30-45
• 全文大小：
• 刊物类别：Physics and Astronomy
• 刊物主题：Astronomy, Astrophysics and Cosmology; Astrophysics and Astroparticles; Space Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics);
• 出版者：Pleiades Publishing
• ISSN：1608-3075
• 卷排序：55

文摘

According to the data of the BMSW/SPEKTR-R instrument, which measured the density and velocity of solar wind plasma with a record time resolution, up to ~3 ×10–2 s, the structure of the front of interplanetary shocks has been investigated. The results of these first investigations were compared with the results of studying the structure of the bow shocks obtained in previous years. A comparison has shown that the quasi-stationary (averaged over the rapid oscillations) distribution of plasma behind the interplanetary shock front was significantly more inhomogeneous than that behind the bow-shock front, i.e., in the magnetosheath. It has also been shown that, to determine the size of internal structures of the fronts of quasi-perpendicular (θ_BN > 45°) shocks, one could use the magnetic field magnitude, the proton density, and the proton flux of the solar wind on almost equal terms. A comparison of low Mach (М_А < 2), low beta (β₁ < 1) fronts of interplanetary and bow shocks has shown that the dispersion of oblique magnetosonic waves plays an essential role in their formation.