首页> 外文会议>SOHO-17 10 Years of SOHO and Beyond >CORONAL HOLE PROPERTIES DURING THE FIRST DECADE OF UVCS/SOHO
【24h】

CORONAL HOLE PROPERTIES DURING THE FIRST DECADE OF UVCS/SOHO

机译:UVCS / SOHO的第一个十年期间的冠孔特性

获取原文

摘要

We have measured with the SOHO Ultraviolet Coronagraph Spectrometer (UVCS) the physical properties of over 160 large coronal holes that produced a variety of high-speed solar wind conditions at 1 AU. This data set includes observations of coronal holes of different sizes and latitudinal locations present throughout solar cycle 23. Previous analyses of a subset of these UVCS observations have shown that polar and equatorial coronal holes produce different acceleration profiles and have different oxygen kinetic temperatures. These analyses also showed that a pattern is emerging, I.e., coronal holes with lower densities at a given heliocentric distance tend to exhibit faster ion outflow and higher ion temperatures. In 2005 and the beginning of 2006, the polar coronal holes have not yet evolved to the fully quiescent minimum state seen in 1996-1997, although the next solar minimum is expected to occur during 2006-2007. We present the solar cycle dependence of the derived O5+ plasma parameters from the last solar minimum in 1996 to present and compare them, where possible, with the in situ solar wind properties. This information is being used to set firm empirical constraints on coronal heating and solar wind acceleration in coronal holes.
机译:我们使用SOHO紫外线日冕仪(UVCS)测量了160多个大日冕孔的物理性质,这些大日冕孔在1 AU下产生了各种高速太阳风。该数据集包括整个太阳周期23中存在的不同大小和纬度位置的冠冕洞的观测结果。先前对这些UVCS观测结果的子集的分析表明,极地和赤道冠冕的洞会产生不同的加速度曲线,并具有不同的氧动力学温度。这些分析还表明出现了一种模式,即在给定的日向中心距离处具有较低密度的日冕孔倾向于表现出更快的离子流出和更高的离子温度。在2005年和2006年初,极地冠状孔还没有演化到1996-1997年所见的完全静止的最低状态,尽管下一个太阳极小期有望在2006-2007年发生。我们介绍了从1996年的最后一个太阳最低峰中得出的O5 +等离子体参数的太阳周期依赖性,以呈现并与原位太阳风特性进行比较。该信息被用来为日冕加热和日冕孔中的太阳风加速设置牢固的经验约束。

著录项

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱:kefu@zhangqiaokeyan.com

京公网安备:11010802029741号 ICP备案号:京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有
  • 客服微信

  • 服务号