Abstract

In the Parker model of the heliospheric magnetic field, the ratio of the azimuthal field component \({{B}_{{{\varphi }}}}\) to the radial component \({{B}_{r}}\) depends only on the radial speed V of the solar wind and coordinates of the observation point (\(r,\,\theta \)): \({{{{B}_{{{\varphi }}}}} \mathord{\left/ {\vphantom {{{{B}_{{{\varphi }}}}} {{{B}_{r}}}}} \right. \kern-0em} {{{B}_{r}}}} = {{ - \omega r\sin \theta } \mathord{\left/ {\vphantom {{ - \omega r\sin \theta } V}} \right. \kern-0em} V}\) (at a distance from the Sun r > 1 AU). We checked this relationship near the ecliptic at radial distances up to 19 AU based on data from the spacecraft VOYAGER 1, VOYAGER 2 and ULYSSES and outside the ecliptic according to ULYSSES data. It is shown that the predictions of the Parker model are in good agreement with observations outside the sector zones in time periods close to the solar activity minima. Within the sector zones and during periods of maximal solar activity, there are significant discrepancies between the observational data and the predictions of this model.

中文翻译：

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日光层磁场和帕克模型

摘要

在日球层磁场的帕克模型中，方位角场分量\({{B}_{{{\varphi }}}}\)与径向分量\({{B}_{r}} \)仅取决于太阳风的径向速度V和观测点的坐标 ( \(r,\,\theta \) )：\({{{{B}_{{{\varphi }}}} } \mathord{\left/ {\vphantom {{{{B}_{{{\varphi }}}}} {{{B}_{r}}}}} \right. \kern-0em} {{ {B}_{r}}}} = {{ - \omega r\sin \theta } \mathord{\left/ {\vphantom {{ - \omega r\sin \theta } V}} \right. \kern -0em} V}\)（距离太阳r> 1 天文单位）。我们根据来自航天器 VOYAGER 1、VOYAGER 2 和 ULYSSES 的数据以及根据 ULYSSES 数据在黄道外检查了径向距离高达 19 AU 的黄道附近的这种关系。结果表明，Parker 模型的预测与太阳活动最小值附近时间段内扇形区域外的观测结果非常吻合。在扇形区域内以及在太阳活动最大的时期，观测数据与该模型的预测之间存在显着差异。