Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave. (arXiv:1905.01211v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Hu_H/0/1/0/all/0/1">Huidong Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_Y/0/1/0/all/0/1">Ying D. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_B/0/1/0/all/0/1">Bei Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peter_H/0/1/0/all/0/1">Hardi Peter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+He_W/0/1/0/all/0/1">Wen He</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_R/0/1/0/all/0/1">Rui Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_Z/0/1/0/all/0/1">Zhongwei Yang</a>
We investigate a global extreme ultraviolet (EUV) wave associated with a
coronal mass ejection (CME)-driven shock on 2017 September 10. The EUV wave is
transmitted by north and south polar coronal holes (CHs), which is observed by
SDO and STEREO A from opposite sides of the Sun. We obtain key findings on how
the EUV wave interacts with multiple coronal structures, and its connection
with the CME-driven shock: (1) the transmitted EUV wave is still connected with
the shock that is incurvated to the Sun, after the shock has reached the
opposite side of the eruption; (2) the south CH transmitted EUV wave is
accelerated inside an on-disk, low-density region with closed magnetic fields,
which implies that an EUV wave can be accelerated in both open and closed
magnetic field regions; (3) part of the primary EUV wavefront turns around a
bright point (BP) with a bipolar magnetic structure when it approaches a dim,
low-density filament channel near the BP; (4) the primary EUV wave is diffused
and apparently halted near the boundaries of remote active regions (ARs) that
are far from the eruption, and no obvious AR related secondary waves are
detected; (5) the EUV wave extends to an unprecedented scale of ~360 degrees in
latitudes, which is attributed to the polar CH transmission. These results
provide insights into the effects of coronal density and magnetic field
distributions on the evolution of an EUV wave, and into the connection between
the EUV wave and the associated CME-driven shock.
We investigate a global extreme ultraviolet (EUV) wave associated with a
coronal mass ejection (CME)-driven shock on 2017 September 10. The EUV wave is
transmitted by north and south polar coronal holes (CHs), which is observed by
SDO and STEREO A from opposite sides of the Sun. We obtain key findings on how
the EUV wave interacts with multiple coronal structures, and its connection
with the CME-driven shock: (1) the transmitted EUV wave is still connected with
the shock that is incurvated to the Sun, after the shock has reached the
opposite side of the eruption; (2) the south CH transmitted EUV wave is
accelerated inside an on-disk, low-density region with closed magnetic fields,
which implies that an EUV wave can be accelerated in both open and closed
magnetic field regions; (3) part of the primary EUV wavefront turns around a
bright point (BP) with a bipolar magnetic structure when it approaches a dim,
low-density filament channel near the BP; (4) the primary EUV wave is diffused
and apparently halted near the boundaries of remote active regions (ARs) that
are far from the eruption, and no obvious AR related secondary waves are
detected; (5) the EUV wave extends to an unprecedented scale of ~360 degrees in
latitudes, which is attributed to the polar CH transmission. These results
provide insights into the effects of coronal density and magnetic field
distributions on the evolution of an EUV wave, and into the connection between
the EUV wave and the associated CME-driven shock.
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