A Three-Dimensional Velocity of an Erupting Prominence Prior to a Coronal Mass Ejection. (arXiv:2101.08575v1 [astro-ph.SR])

A Three-Dimensional Velocity of an Erupting Prominence Prior to a Coronal Mass Ejection. (arXiv:2101.08575v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gutierrez_M/0/1/0/all/0/1">Maria V. Gutierrez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Otsuji_K/0/1/0/all/0/1">Kenichi Otsuji</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asai_A/0/1/0/all/0/1">Ayumi Asai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Terrazas_R/0/1/0/all/0/1">Raul Terrazas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishitsuka_M/0/1/0/all/0/1">Mutsumi Ishitsuka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishitsuka_J/0/1/0/all/0/1">Jose Ishitsuka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakamura_N/0/1/0/all/0/1">Naoki Nakamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshinaga_Y/0/1/0/all/0/1">Yusuke Yoshinaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morita_S/0/1/0/all/0/1">Satoshi Morita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishii_T/0/1/0/all/0/1">Takako T. Ishii</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+UeNo_S/0/1/0/all/0/1">Satoru UeNo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kitai_R/0/1/0/all/0/1">Reizaburo Kitai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shibata_K/0/1/0/all/0/1">Kazunari Shibata</a>

We present a detailed three-dimensional (3D) view of a prominence eruption,
coronal loop expansion, and coronal mass ejections (CMEs) associated with an
M4.4 flare that occurred on 2011 March 8 in the active region NOAA 11165.
Full-disk H$alpha$ images of the flare and filament ejection were successfully
obtained by the Flare Monitoring Telescope (FMT) following its relocation to
Ica University, Peru. Multiwavelength observation around the H$alpha$ line
enabled us to derive the 3D velocity field of the H$alpha$ prominence
eruption. Features in extreme ultraviolet were also obtained by the Atmospheric
Imager Assembly onboard the {it Solar Dynamic Observatory} and the Extreme
Ultraviolet Imager on board the {it Solar Terrestrial Relations Observatory –
Ahead} satellite. We found that, following collision of the erupted filament
with the coronal magnetic field, some coronal loops began to expand, leading to
the growth of a clear CME. We also discuss the succeeding activities of CME
driven by multiple interactions between the expanding loops and the surrounding
coronal magnetic field.

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