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Title: QUADRATURE OBSERVATIONS OF WAVE AND NON-WAVE COMPONENTS AND THEIR DECOUPLING IN AN EXTREME-ULTRAVIOLET WAVE EVENT

Abstract

We report quadrature observations of an extreme-ultraviolet (EUV) wave event on 2011 January 27 obtained by the Extreme Ultraviolet Imager on board the Solar Terrestrial Relations Observatory, and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. Two components are revealed in the EUV wave event. A primary front is launched with an initial speed of {approx}440 km s{sup -1}. It appears that significant emission enhancement occurs in the hotter channel while deep emission reduction occurs in the cooler channel. When the primary front encounters a large coronal loop system and slows down, a secondary, much fainter, front emanates from the primary front with a relatively higher starting speed of {approx}550 km s{sup -1}. Afterward, the two fronts propagate independently with increasing separation. The primary front finally stops at a magnetic separatrix, while the secondary front travels farther until it fades out. In addition, upon the arrival of the secondary front, transverse oscillations of a prominence are triggered. We suggest that the two components are of different natures. The primary front belongs to a non-wave coronal mass ejection (CME) component, which can be reasonably explained with the field-line stretching model. The multi-temperature behavior may be caused by considerable heatingmore » due to nonlinear adiabatic compression on the CME frontal loop. As for the secondary front, it is most likely a linear fast-mode magnetohydrodynamic wave that propagates through a medium of the typical coronal temperature. X-ray and radio data provide us with complementary evidence in support of the above scenario.« less

Authors:
; ;  [1];  [2]
  1. School of Astronomy and Space Science, Nanjing University, Nanjing 210093 (China)
  2. School of Physics, Astronomy, and Computational Sciences, George Mason University, Fairfax, VA 22030 (United States)
Publication Date:
OSTI Identifier:
22086434
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 759; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTRONOMY; ASTROPHYSICS; COMPRESSION; DECOUPLING; EXTREME ULTRAVIOLET RADIATION; HEATING; HOT CHANNEL; HYDROMAGNETIC WAVES; MASS; NONLINEAR PROBLEMS; OSCILLATIONS; PHOTON EMISSION; QUADRATURES; SUN; VELOCITY; X RADIATION

Citation Formats

Dai, Y., Ding, M. D., Chen, P. F., and Zhang, J., E-mail: ydai@nju.edu.cn. QUADRATURE OBSERVATIONS OF WAVE AND NON-WAVE COMPONENTS AND THEIR DECOUPLING IN AN EXTREME-ULTRAVIOLET WAVE EVENT. United States: N. p., 2012. Web. doi:10.1088/0004-637X/759/1/55.
Dai, Y., Ding, M. D., Chen, P. F., & Zhang, J., E-mail: ydai@nju.edu.cn. QUADRATURE OBSERVATIONS OF WAVE AND NON-WAVE COMPONENTS AND THEIR DECOUPLING IN AN EXTREME-ULTRAVIOLET WAVE EVENT. United States. doi:10.1088/0004-637X/759/1/55.
Dai, Y., Ding, M. D., Chen, P. F., and Zhang, J., E-mail: ydai@nju.edu.cn. Thu . "QUADRATURE OBSERVATIONS OF WAVE AND NON-WAVE COMPONENTS AND THEIR DECOUPLING IN AN EXTREME-ULTRAVIOLET WAVE EVENT". United States. doi:10.1088/0004-637X/759/1/55.
@article{osti_22086434,
title = {QUADRATURE OBSERVATIONS OF WAVE AND NON-WAVE COMPONENTS AND THEIR DECOUPLING IN AN EXTREME-ULTRAVIOLET WAVE EVENT},
author = {Dai, Y. and Ding, M. D. and Chen, P. F. and Zhang, J., E-mail: ydai@nju.edu.cn},
abstractNote = {We report quadrature observations of an extreme-ultraviolet (EUV) wave event on 2011 January 27 obtained by the Extreme Ultraviolet Imager on board the Solar Terrestrial Relations Observatory, and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. Two components are revealed in the EUV wave event. A primary front is launched with an initial speed of {approx}440 km s{sup -1}. It appears that significant emission enhancement occurs in the hotter channel while deep emission reduction occurs in the cooler channel. When the primary front encounters a large coronal loop system and slows down, a secondary, much fainter, front emanates from the primary front with a relatively higher starting speed of {approx}550 km s{sup -1}. Afterward, the two fronts propagate independently with increasing separation. The primary front finally stops at a magnetic separatrix, while the secondary front travels farther until it fades out. In addition, upon the arrival of the secondary front, transverse oscillations of a prominence are triggered. We suggest that the two components are of different natures. The primary front belongs to a non-wave coronal mass ejection (CME) component, which can be reasonably explained with the field-line stretching model. The multi-temperature behavior may be caused by considerable heating due to nonlinear adiabatic compression on the CME frontal loop. As for the secondary front, it is most likely a linear fast-mode magnetohydrodynamic wave that propagates through a medium of the typical coronal temperature. X-ray and radio data provide us with complementary evidence in support of the above scenario.},
doi = {10.1088/0004-637X/759/1/55},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 759,
place = {United States},
year = {2012},
month = {11}
}