scholarly journals Suzaku detection of enigmatic geocoronal solar wind charge exchange event associated with coronal mass ejection

2019 ◽  
Vol 71 (1) ◽  
Author(s):  
Daiki Ishi ◽  
Kumi Ishikawa ◽  
Masaki Numazawa ◽  
Yoshizumi Miyoshi ◽  
Naoki Terada ◽  
...  
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Charge Exchange ◽  
Exchange Event ◽  
Solar Wind Charge Exchange ◽  
Mass Ejection

Possible Solar Wind Charge Exchange Emission from a Coronal Mass Ejection

2009 ◽  
Author(s):  
David B. Henley ◽  
Robin L. Shelton ◽  
Randall K. Smith ◽  
Steven L. Snowden ◽  
K. D. Kuntz
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Charge Exchange ◽  
Solar Wind Charge Exchange ◽  
Mass Ejection

scholarly journals Three-dimensional MHD modeling of the solar wind structures associated with 13 December 2006 coronal mass ejection

2009 ◽  
Vol 114 (A10) ◽  
pp. n/a-n/a ◽  
Author(s):  
R. Kataoka ◽  
T. Ebisuzaki ◽  
K. Kusano ◽  
D. Shiota ◽  
S. Inoue ◽  
...  
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Three Dimensional ◽  
Mhd Modeling ◽  
Mass Ejection

scholarly journals Photospheric magnetic field of an eroded-by-solar-wind coronal mass ejection

2016 ◽  
Vol 12 (S327) ◽  
pp. 67-70
Author(s):  
J. Palacios ◽  
C. Cid ◽  
E. Saiz ◽  
A. Guerrero
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Coronal Hole ◽  
Interplanetary Medium ◽  
Flux Rope ◽  
Magnetic Characteristics ◽  
Interplanetary Coronal Mass Ejection ◽  
Fast Wind ◽  
Mass Ejection

AbstractWe have investigated the case of a coronal mass ejection that was eroded by the fast wind of a coronal hole in the interplanetary medium. When a solar ejection takes place close to a coronal hole, the flux rope magnetic topology of the coronal mass ejection (CME) may become misshapen at 1 AU as a result of the interaction. Detailed analysis of this event reveals erosion of the interplanetary coronal mass ejection (ICME) magnetic field. In this communication, we study the photospheric magnetic roots of the coronal hole and the coronal mass ejection area with HMI/SDO magnetograms to define their magnetic characteristics.

scholarly journals Imaging Plasma Density Structures in the Soft X-Rays Generated by Solar Wind Charge Exchange with Neutrals

2018 ◽  
Vol 214 (4) ◽  
Author(s):  
David G. Sibeck ◽  
R. Allen ◽  
H. Aryan ◽  
D. Bodewits ◽  
P. Brandt ◽  
...  
Keyword(s):  
Solar Wind ◽  
Charge Exchange ◽  
Plasma Density ◽  
X Rays ◽  
Solar Wind Charge Exchange

OBSERVATION OF SOLAR WIND CHARGE EXCHANGE EMISSION FROM EXOSPHERIC MATERIAL IN AND OUTSIDE EARTH'S MAGNETOSHEATH 2008 SEPTEMBER 25

2009 ◽  
Vol 691 (1) ◽  
pp. 372-381 ◽  
Author(s):  
S. L. Snowden ◽  
M. R. Collier ◽  
T. Cravens ◽  
K. D. Kuntz ◽  
S. T. Lepri ◽  
...  
Keyword(s):  
Solar Wind ◽  
Charge Exchange ◽  
Solar Wind Charge Exchange

A bubblelike coronal mass ejection flux rope in the solar wind

1990 ◽  
pp. 365-371 ◽  
Author(s):  
N. U. Crooker ◽  
J. T. Gosling ◽  
E. J. Smith ◽  
C. T. Russell
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Flux Rope ◽  
Mass Ejection

scholarly journals Planar magnetic structures in coronal mass ejection-driven sheath regions

2016 ◽  
Vol 34 (2) ◽  
pp. 313-322 ◽  
Author(s):  
Erika Palmerio ◽  
Emilia K. J. Kilpua ◽  
Neel P. Savani
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Leading Edge ◽  
Formation Mechanisms ◽  
Single Plane ◽  
Magnetic Structures ◽  
Automated Method ◽  
Mass Ejection ◽  
The Magnetic Field

Abstract. Planar magnetic structures (PMSs) are periods in the solar wind during which interplanetary magnetic field vectors are nearly parallel to a single plane. One of the specific regions where PMSs have been reported are coronal mass ejection (CME)-driven sheaths. We use here an automated method to identify PMSs in 95 CME sheath regions observed in situ by the Wind and ACE spacecraft between 1997 and 2015. The occurrence and location of the PMSs are related to various shock, sheath, and CME properties. We find that PMSs are ubiquitous in CME sheaths; 85 % of the studied sheath regions had PMSs with the mean duration of 6 h. In about one-third of the cases the magnetic field vectors followed a single PMS plane that covered a significant part (at least 67 %) of the sheath region. Our analysis gives strong support for two suggested PMS formation mechanisms: the amplification and alignment of solar wind discontinuities near the CME-driven shock and the draping of the magnetic field lines around the CME ejecta. For example, we found that the shock and PMS plane normals generally coincided for the events where the PMSs occurred near the shock (68 % of the PMS plane normals near the shock were separated by less than 20° from the shock normal), while deviations were clearly larger when PMSs occurred close to the ejecta leading edge. In addition, PMSs near the shock were generally associated with lower upstream plasma beta than the cases where PMSs occurred near the leading edge of the CME. We also demonstrate that the planar parts of the sheath contain a higher amount of strong southward magnetic field than the non-planar parts, suggesting that planar sheaths are more likely to drive magnetospheric activity.

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