论文标题
质子 - 普罗顿碰撞年龄订购太阳风类型
Proton-proton collisional age to order solar wind types
论文作者
论文摘要
太阳风流的性质取决于其源区域和运输效应。与太阳风类型无关，原位测得的太阳风总是受两者的影响。我们将质子 - 普罗顿碰撞年龄视为1AU处太阳风的订购参数，并探索了其与Xu＆Borovsky开发的太阳风风格分类方案的关系（2015年）。我们使用它来表明这种太阳风分类不需要明确的磁场信息。基于这样的观察，该分类的三种基本太阳风类型涵盖了质子 - 普罗顿碰撞年龄$ a_ {col，p-p} $的不同制度，我们提出了一种仅基于Proton-Proton colisional Age的简化太阳能风力分类方案。由此产生的所谓PAC太阳能风能分类器是完整的Xu＆Borovsky（2015）太阳能风能分类方案的替代方案，并导致与完整的Xu＆Borovsky（2015）方案非常相似的分类。质子 - 普罗顿碰撞时代井井有条。这意味着血浆特性之间的潜在固有关系，尤其是每个等离子体状态中的质子温度和磁场强度。我们认为，部门 - 反转等离子体是特别缓慢和密集的太阳风和大多数河流相互作用边界的组合。大多数太阳风参数（例如，磁场强度，B和氧电荷状态比$ n_ {o^{7+}} $ /$ n_ {o^{6+}} $）随着太阳能活动周期而变化。因此，所有基于阈值的太阳风向分类方案也需要适应太阳活动周期。
The properties of a solar wind stream are determined by its source region and by transport effects. Independently of the solar wind type, the solar wind measured in situ is always affected by both. We consider the proton-proton collisional age as an ordering parameter for the solar wind at 1AU and explore its relation to the solar wind classification scheme developed by Xu & Borovsky (2015). We use this to show that explicit magnetic field information is not required for this solar wind classification. Based on the observation that the three basic solar wind types from this categorization cover different regimes in terms of proton-proton collisional age $a_{col,p-p}$ , we propose a simplified solar wind classification scheme that is only based on the proton-proton collisional age. The resulting so-called PAC solar wind classifier is an alternative to the full Xu & Borovsky (2015) solar wind classification scheme and leads to a classification that is very similar to the full Xu & Borovsky (2015) scheme. The solar wind is well ordered by the proton-proton collisional age. This implies underlying intrinsic relationships between the plasma properties, in particular, proton temperature and magnetic field strength in each plasma regime. We argue that sector-reversal plasma is a combination of particularly slow and dense solar wind and most stream interaction boundaries. Most solar wind parameters (e.g., the magnetic field strength, B, and the oxygen charge state ratio $n_{O^{7+}}$ /$n_{O^{6+}}$) change with the solar activity cycle. Thus, all solar wind categorization schemes based on threshold values need to be adapted to the solar activity cycle as well.
