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Interaction of interplanetary shocks with the heliospheric termination shock: Two-dimensional magnetohydrodynamic modelстатья
Информация о цитировании статьи получена из
Web of Science
Статья опубликована в журнале из списка Web of Science и/или Scopus
Дата последнего поиска статьи во внешних источниках: 27 мая 2015 г.
- Авторы: Baranov V.B., Barmin A.A., Pushkar E.A.
- Журнал: Journal of Geophysical Research: Space Physics
- Том: 101
- Номер: A12
- Год издания: 1996
- Издательство: AGU Publications
- Местоположение издательства: Вашингтон
- Первая страница: 27465
- Последняя страница: 27481
- DOI: 10.1029/96JA02459
- Аннотация: The two-dimensional problem of the oblique interaction between an interplanetary shock (IPS) and the termination shock (TS) with allowance for the effect of the interplanetary magnetic field is studied within the framework of the ideal magnetohydrodynamic model and a steady model of the solar wind interaction with the local interstellar medium. The self-consistent axisymmetric model proposed by Baranov and Malama which takes into account the processes of resonant charge exchange between H atoms and protons is used. The electron number density and the solar wind velocity V-SW ahead of TS depends on the parameters of this model. The postinteraction configuration consists of a new moving TS', a transmitted IPS', a set of Alfven and slow magnetohydrodynamic waves, and a contact discontinuity which can change as functions of five dimensionless governing parameters and the specific heat ratio gamma. The maximum electron number density n(e) is usually reached behind the new. termination shock TS' for an oblique (theta not equal 0) impingement of IPS on TS rather than for the head-on collision (theta=0). Nevertheless, the maximum calculated values of n, are lower than those corresponding to plasma frequencies omega(p) congruent to 2 kHz observed by-the Voyager spacecraft. It is found that all the quantities Is considered depends radically on the angle psi(TS) between the front of TS and the vector of the interplanetary magnetic field strength B-SW.
- Добавил в систему: Баранов Владимир Борисович