标题： 1999-2008 年期间由先进 Composition Explorer (ACE) 采样的太阳风的冕源与原位特性 显示英文标题

标题： Coronal sources and in situ properties of the solar winds sampled by ACE during 1999-2008

摘要： 我们识别了1999-2008年期间由ACE航天器采样的太阳风的日冕源，并研究了这些太阳风的原位特性随来源的变化。 采用标准的两步映射技术来建立沿ACE太阳风流动的磁通管的日面足点。 然后将这些足点置于EIT 284~\AA 图像和光球磁图的背景下，从而使我们可以将这些源分类为四组：日冕洞（CHs）、活动区（ARs）、宁静太阳（QS）以及“未定义”。 这种方法还使我们能够确定各类太阳风所占比例、它们的速度以及原位测量到的O$^{7+}$/O$^{6+}$比值对太阳活动的响应。 我们发现，在太阳活动极大期，大多数ACE太阳风起源于活动区。 在下降阶段，日冕洞和活动区对ACE太阳风的贡献同样重要。 随着太阳活动减弱，QS的贡献增加，在最小活动期达到最大值，此时QS似乎是ACE太阳风的主要供应者。 随着活动减少，所有来源的太阳风趋于变冷，表现为O$^{7+}$/O$^{6+}$比率的逐渐降低。 另一方面，在每个活动阶段，AR太阳风往往最慢且与最高的O$^{7+}$/O$^{6+}$比率相关联，而CH太阳风则对应相反的情况，QS太阳风处于两者之间。 仅针对速度低于 500 km s$^{-1}$的慢速风应用相同的分析方法，我们发现，就各源项的贡献而言，整体行为基本相同。 这项统计研究显示， Quiet Sun 区域在太阳活动极小期是太阳风的重要源区。 显示英文摘要

摘要： We identify the coronal sources of the solar winds sampled by the ACE spacecraft during 1999-2008, and examine the in situ solar wind properties as a function of wind sources. The standard two-step mapping technique is adopted to establish the photospheric footpoints of the magnetic flux tubes along which the ACE winds flow. The footpoints are then placed in the context of EIT 284~\AA\ images and photospheric magnetograms, allowing us to categorize the sources into four groups: coronal holes (CHs), active regions (ARs), the quiet Sun (QS), and "Undefined". This practice also enables us to establish the response to solar activity of the fractions occupied by each kind of solar winds, and of their speeds and O$^{7+}$/O$^{6+}$ ratios measured in situ. We find that during the maximum phase, the majority of ACE winds originate from ARs. During the declining phase, CHs and ARs are equally important contributors to the ACE solar winds. The QS contribution increases with decreasing solar activity, and maximizes in the minimum phase when QS appear to be the primary supplier of the ACE winds. With decreasing activity, the winds from all sources tend to become cooler, as represented by the increasingly low O$^{7+}$/O$^{6+}$ ratios. On the other hand, during each activity phase, the AR winds tend to be the slowest and associated with the highest O$^{7+}$/O$^{6+}$ ratios, and the CH winds correspond to the other extreme, with the QS winds lying in between. Applying the same analysis method to the slow winds only, here defined as the winds with speeds lower than 500 km s$^{-1}$, we find basically the same overall behavior, as far as the contributions of individual groups of sources are concerned. This statistical study indicates that QS regions are an important source of the solar wind during the minimum phase.