A three-dimensional velocity of an erupting prominence prior to a coronal mass ejection-Reference-Cited by-同舟云学术

A three-dimensional velocity of an erupting prominence prior to a coronal mass ejection

Published:2021-02-27 Issue:2 Volume:73 Page:394-404
ISSN:0004-6264
Container-title:Publications of the Astronomical Society of Japan
language:en
Short-container-title:

Author:

Gutierrez Maria V¹²,Otsuji Kenichi³⁴,Asai Ayumi⁴,Terrazas Raul⁵,Ishitsuka Mutsumi²,Ishitsuka Jose²⁶,Nakamura Naoki⁴,Yoshinaga Yusuke⁷,Morita Satoshi⁸,Ishii Takako T⁴,Ueno Satoru⁴,Kitai Reizaburo⁴⁹¹⁰,Shibata Kazunari⁴¹¹

Affiliation:

1. Institute for Research in Astronomy and Astrophysics (IAFE CONICET-UBA), CC 67, Suc. 28, 1428 Buenos Aires, Argentina

2. Geophysical Institute of Peru, Calle Badajoz 169, Mayorazgo IV Etapa, Ate Vitarte, Lima, Peru

3. National Institute of Information and Communications Technology (NICT), Koganei, Tokyo, 184-8795, Japan

4. Astronomical Observatory, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, Japan

5. Ica Solar Station, Department of Physics, San Luis Gonzaga National University , Av. Los Maestros S/N, Ica, Peru

6. National University of the Center of Peru, Mariscal Castilla 3909, Huancayo 12006, Peru

7. Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, Japan

8. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan

9. Bukkyo University, 96 Kitahananobo-cho, Murasakino, Kita-ku, Kyoto, Kyoto 603-8301, Japan

10. Ritsumeikan University, 56-1 Tojiin-Kitamachi Kita-ku, Kyoto, Kyoto 603-8577, Japan

11. Doshisha University, 1-3 Tatara Miyakodani, Kyotanabe-shi, Kyoto 610-0394, Japan

Abstract

Abstract 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 Hα 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 Hα line enabled us to derive the 3D velocity field of the Hα prominence eruption. Features in extreme ultraviolet were also obtained by the Atmospheric Imager Assembly onboard the Solar Dynamic Observatory and the Extreme Ultraviolet Imager on board the 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.

Funder

Kyoto University

JSPS

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Link

http://academic.oup.com/pasj/article-pdf/73/2/394/36900199/psab006.pdf

Reference50 articles.

1. FIRST SIMULTANEOUS OBSERVATION OF AN Hα MORETON WAVE, EUV WAVE, AND FILAMENT/PROMINENCE OSCILLATIONS

2. Preflare Nonthermal Emission Observed in Microwaves and Hard X-Rays

3. Downflow Motions Associated with Impulsive Nonthermal Emissions Observed in the 2002 July 23 Solar Flare

4. The Large Angle Spectroscopic Coronagraph (LASCO)

Cited by 2 articles. 订阅此论文施引文献订阅此论文施引文献，注册后可以免费订阅5篇论文的施引文献，订阅后可以查看论文全部施引文献

1. Multiwavelength Sun-as-a-star Analysis of the M8.7 Flare on 2022 October 2 Using Hα and EUV Spectra Taken by SMART/SDDI and SDO/EVE;The Astrophysical Journal;2024-03-01

2. Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE;The Astrophysical Journal Letters;2024-01-25