连接低冕和高冕:作为近太阳太阳风追踪器的传播扰动

Nathalia Alzate, Simone Di Matteo, Huw Morgan, Nicholeen Viall, Angelos Vourlidas
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引用次数: 0

摘要

我们重新审视了 2008 年 1 月为期 14 天的太阳最小静止期,并跟踪了从 STEREO/EUVI 低空到延伸日冕的子流体传播扰动(PDs),穿过 STEREO/COR1,并沿着非径向路径进入 STEREO/COR2,以追踪底层流体的结构。我们对 417 个独特的 OPD 进行了分析,发现它们分为两类:慢 OPD 和快 OPD。慢速OPDs在靠近流体边界的$\approx$1.6 $R_\odot$处优先形成,出现率不对称,在1.5 $R_\odot$处速度为$16.4_{-8.4}^{+26.6}km/s$,在7.5 $R_\odot$处加速到$200.1_{-57.9}^{+71.1}km/s$。快速OPDs优先在1.6 R_\odot$和3.0 R_\odot$时形成,这两种情况都发生在流线体的边界,而在流线体内部则更为常见。它们在1.5 $R_\odot$时的速度为$87.8_{-24.8}^{+59.1}km/s$,在7.5 $R_\odot$时的速度为$197.8_{-46.7}^{+61.8}km/s$。我们观测到 IPDs 在大约 $1.8R_\odot$时形成,速度为数十 $km/s$,大部分集中在 CME 爆发之后。我们举例说明,与OPDs有关的周期性亮度变化保持在98-128 min的范围内,低至$\approx$2.0 $R_\odot$,完全在COR1的视场之内。日心高度低于3.0 $R_\odot$的慢速OPDs的速度剖面与通过行星际闪烁获得的与太阳风体更密切相关的速度非常一致。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Connecting the Low to High Corona: Propagating Disturbances as Tracers of the Near-Sun Solar Wind
We revisit a quiet 14-day period of solar minimum during January 2008 and track sub-streamer propagating disturbances (PDs) from low heights in STEREO/EUVI to the extended corona through STEREO/COR1 and into STEREO/COR2 along nonradial paths that trace the structure of the underlying streamers. Using our recently developed method for generating nonradial Height-Time profiles of outward PDs (OPDs) and inward PDs (IPDs), we obtained their velocities along the radial and position angle directions. Our analysis of 417 unique OPDs revealed two classes: slow and fast OPDs. Slow OPDs form preferentially at $\approx$1.6 $R_\odot$ closer to the streamer boundaries, with asymmetric occurrence rates, and show speeds of $16.4_{-8.4}^{+26.6}km/s$ at 1.5 $R_\odot$ and accelerate up to $200.1_{-57.9}^{+71.1}km/s$ at 7.5 $R_\odot$. Fast OPDs form preferentially at $\approx$ 1.6 $R_\odot$ and at $\approx$3.0 $R_\odot$ both at the streamer boundaries and slightly more often within them. They show speeds of $87.8_{-24.8}^{+59.1}km/s$ at 1.5 $R_\odot$ up to $197.8_{-46.7}^{+61.8}km/s$ at 7.5 $R_\odot$. IPDs are observed forming at $\approx$1.8 $R_\odot$ with speeds of tens of $km/s$, mostly concentrated in the aftermath of a CME eruption. We present an example in which we show that periodic brightness variations related to OPDs remained in the range of 98 to 128 min, down to $\approx$2.0 $R_\odot$, well within the field of view of COR1. The velocity profiles of slow OPDs for heliocentric height below 3.0 $R_\odot$ show good agreement with speeds more closely related to the bulk solar wind obtained via interplanetary scintillation.
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