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

Title: Investigating the Wave Nature of the Outer Envelope of Halo Coronal Mass Ejections

Abstract

We investigate the nature of the outer envelope of halo coronal mass ejections (H-CMEs) using multi-viewpoint observations from the Solar Terrestrial Relations Observatory-A , -B , and SOlar and Heliospheric Observatory coronagraphs. The 3D structure and kinematics of the halo envelopes and the driving CMEs are derived separately using a forward modeling method. We analyze three H-CMEs with peak speeds from 1355 to 2157 km s{sup −1}; sufficiently fast to drive shocks in the corona. We find that the angular widths of the halos range from 192° to 252°, while those of the flux ropes range between only 58° and 91°, indicating that the halos are waves propagating away from the CMEs. The halo widths are in agreement with widths of Extreme Ultraviolet (EUV) waves in the low corona further demonstrating the common origin of these structures. To further investigate the wave nature of the halos, we model their 3D kinematic properties with a linear fast magnetosonic wave model. The model is able to reproduce the position of the halo flanks with realistic coronal medium assumptions but fails closer to the CME nose. The CME halo envelope seems to arise from a driven wave (or shock) close to the CMEmore » nose, but it is gradually becoming a freely propagating fast magnetosonic wave at the flanks. This interpretation provides a simple unifying picture for CME halos, EUV waves, and the large longitudinal spread of solar energetic particles.« less

Authors:
 [1];  [2]
  1. College of Science, George Mason University, 4400 University Drive, Fairfax, VA 22030 (United States)
  2. The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 (United States)
Publication Date:
OSTI Identifier:
22663750
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 836; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; EXTREME ULTRAVIOLET RADIATION; MAGNETOACOUSTIC WAVES; MASS; SIMULATION; SOLAR CORONA; SUN; VELOCITY

Citation Formats

Kwon, Ryun-Young, and Vourlidas, Angelos, E-mail: rkwon@gmu.edu. Investigating the Wave Nature of the Outer Envelope of Halo Coronal Mass Ejections. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA5B92.
Kwon, Ryun-Young, & Vourlidas, Angelos, E-mail: rkwon@gmu.edu. Investigating the Wave Nature of the Outer Envelope of Halo Coronal Mass Ejections. United States. doi:10.3847/1538-4357/AA5B92.
Kwon, Ryun-Young, and Vourlidas, Angelos, E-mail: rkwon@gmu.edu. Mon . "Investigating the Wave Nature of the Outer Envelope of Halo Coronal Mass Ejections". United States. doi:10.3847/1538-4357/AA5B92.
@article{osti_22663750,
title = {Investigating the Wave Nature of the Outer Envelope of Halo Coronal Mass Ejections},
author = {Kwon, Ryun-Young and Vourlidas, Angelos, E-mail: rkwon@gmu.edu},
abstractNote = {We investigate the nature of the outer envelope of halo coronal mass ejections (H-CMEs) using multi-viewpoint observations from the Solar Terrestrial Relations Observatory-A , -B , and SOlar and Heliospheric Observatory coronagraphs. The 3D structure and kinematics of the halo envelopes and the driving CMEs are derived separately using a forward modeling method. We analyze three H-CMEs with peak speeds from 1355 to 2157 km s{sup −1}; sufficiently fast to drive shocks in the corona. We find that the angular widths of the halos range from 192° to 252°, while those of the flux ropes range between only 58° and 91°, indicating that the halos are waves propagating away from the CMEs. The halo widths are in agreement with widths of Extreme Ultraviolet (EUV) waves in the low corona further demonstrating the common origin of these structures. To further investigate the wave nature of the halos, we model their 3D kinematic properties with a linear fast magnetosonic wave model. The model is able to reproduce the position of the halo flanks with realistic coronal medium assumptions but fails closer to the CME nose. The CME halo envelope seems to arise from a driven wave (or shock) close to the CME nose, but it is gradually becoming a freely propagating fast magnetosonic wave at the flanks. This interpretation provides a simple unifying picture for CME halos, EUV waves, and the large longitudinal spread of solar energetic particles.},
doi = {10.3847/1538-4357/AA5B92},
journal = {Astrophysical Journal},
number = 2,
volume = 836,
place = {United States},
year = {Mon Feb 20 00:00:00 EST 2017},
month = {Mon Feb 20 00:00:00 EST 2017}
}