skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: PROMINENCE ACTIVATION BY CORONAL FAST MODE SHOCK

Abstract

An X5.4 class flare occurred in active region NOAA11429 on 2012 March 7. The flare was associated with a very fast coronal mass ejection (CME) with a velocity of over 2500 km s{sup −1}. In the images taken with the Solar Terrestrial Relations Observatory-B/COR1, a dome-like disturbance was seen to detach from an expanding CME bubble and propagated further. A Type-II radio burst was also observed at the same time. On the other hand, in extreme ultraviolet images obtained by the Solar Dynamic Observatory/Atmospheric Imaging Assembly (AIA), the expanding dome-like structure and its footprint propagating to the north were observed. The footprint propagated with an average speed of about 670 km s{sup −1} and hit a prominence located at the north pole and activated it. During the activation, the prominence was strongly brightened. On the basis of some observational evidence, we concluded that the footprint in AIA images and the ones in COR1 images are the same, that is, the MHD fast mode shock front. With the help of a linear theory, the fast mode Mach number of the coronal shock is estimated to be between 1.11 and 1.29 using the initial velocity of the activated prominence. Also, the plasmamore » compression ratio of the shock is enhanced to be between 1.18 and 2.11 in the prominence material, which we consider to be the reason for the strong brightening of the activated prominence. The applicability of linear theory to the shock problem is tested with a nonlinear MHD simulation.« less

Authors:
 [1];  [2];  [3]
  1. Department of Astronomy, Kyoto University, Sakyo, Kyoto, 606-8502 (Japan)
  2. Unit of Synergetic Studies for Space, Kyoto University, Yamashina, Kyoto 607-8471 (Japan)
  3. Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471 (Japan)
Publication Date:
OSTI Identifier:
22522050
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 801; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BUBBLES; COMPRESSION RATIO; COMPUTERIZED SIMULATION; DISTURBANCES; EXTREME ULTRAVIOLET RADIATION; FILAMENTS; IMAGES; MACH NUMBER; MAGNETOHYDRODYNAMICS; MASS; NONLINEAR PROBLEMS; PLASMA; SHOCK WAVES; SOLAR FLARES; SUN

Citation Formats

Takahashi, Takuya, Asai, Ayumi, and Shibata, Kazunari, E-mail: takahashi@kwasan.kyoto-u.ac.jp. PROMINENCE ACTIVATION BY CORONAL FAST MODE SHOCK. United States: N. p., 2015. Web. doi:10.1088/0004-637X/801/1/37.
Takahashi, Takuya, Asai, Ayumi, & Shibata, Kazunari, E-mail: takahashi@kwasan.kyoto-u.ac.jp. PROMINENCE ACTIVATION BY CORONAL FAST MODE SHOCK. United States. doi:10.1088/0004-637X/801/1/37.
Takahashi, Takuya, Asai, Ayumi, and Shibata, Kazunari, E-mail: takahashi@kwasan.kyoto-u.ac.jp. Sun . "PROMINENCE ACTIVATION BY CORONAL FAST MODE SHOCK". United States. doi:10.1088/0004-637X/801/1/37.
@article{osti_22522050,
title = {PROMINENCE ACTIVATION BY CORONAL FAST MODE SHOCK},
author = {Takahashi, Takuya and Asai, Ayumi and Shibata, Kazunari, E-mail: takahashi@kwasan.kyoto-u.ac.jp},
abstractNote = {An X5.4 class flare occurred in active region NOAA11429 on 2012 March 7. The flare was associated with a very fast coronal mass ejection (CME) with a velocity of over 2500 km s{sup −1}. In the images taken with the Solar Terrestrial Relations Observatory-B/COR1, a dome-like disturbance was seen to detach from an expanding CME bubble and propagated further. A Type-II radio burst was also observed at the same time. On the other hand, in extreme ultraviolet images obtained by the Solar Dynamic Observatory/Atmospheric Imaging Assembly (AIA), the expanding dome-like structure and its footprint propagating to the north were observed. The footprint propagated with an average speed of about 670 km s{sup −1} and hit a prominence located at the north pole and activated it. During the activation, the prominence was strongly brightened. On the basis of some observational evidence, we concluded that the footprint in AIA images and the ones in COR1 images are the same, that is, the MHD fast mode shock front. With the help of a linear theory, the fast mode Mach number of the coronal shock is estimated to be between 1.11 and 1.29 using the initial velocity of the activated prominence. Also, the plasma compression ratio of the shock is enhanced to be between 1.18 and 2.11 in the prominence material, which we consider to be the reason for the strong brightening of the activated prominence. The applicability of linear theory to the shock problem is tested with a nonlinear MHD simulation.},
doi = {10.1088/0004-637X/801/1/37},
journal = {Astrophysical Journal},
number = 1,
volume = 801,
place = {United States},
year = {Sun Mar 01 00:00:00 EST 2015},
month = {Sun Mar 01 00:00:00 EST 2015}
}