Abstract
We report radial-speed evolution of interplanetary coronal mass ejections (ICMEs) detected by the Large Angle and Spectrometric Coronagraph onboard the Solar and Heliospheric Observatory (SOHO/LASCO), interplanetary scintillation (IPS) at 327 MHz, and in-situ observations. We analyze solar-wind disturbance factor (g-value) data derived from IPS observations during 1997 – 2009 covering nearly the whole period of Solar Cycle 23. By comparing observations from SOHO/LASCO, IPS, and in situ, we identify 39 ICMEs that could be analyzed carefully. Here, we define two speeds [V SOHO and V bg], which are the initial speed of the ICME and the speed of the background solar wind, respectively. Examinations of these speeds yield the following results: i) Fast ICMEs (with V SOHO−V bg>500 km s−1) rapidly decelerate, moderate ICMEs (with 0 km s−1≤V SOHO−V bg≤500 km s−1) show either gradually decelerating or uniform motion, and slow ICMEs (with V SOHO−V bg<0 km s−1) accelerate. The radial speeds converge on the speed of the background solar wind during their outward propagation. We subsequently find; ii) both the acceleration and the deceleration are nearly complete by 0.79±0.04 AU, and those are ended when the ICMEs reach a 480±21 km s−1. iii) For ICMEs with (V SOHO−V bg)≥0 km s−1, i.e. fast and moderate ICMEs, a linear equation a=−γ 1(V−V bg) with γ 1=6.58±0.23×10−6 s−1 is more appropriate than a quadratic equation a=−γ 2(V−V bg)|V−V bg| to describe their kinematics, where γ 1 and γ 2 are coefficients, and a and V are the acceleration and speed of ICMEs, respectively, because the χ 2 for the linear equation satisfies the statistical significance level of 0.05, while the quadratic one does not. These results support the assumption that the radial motion of ICMEs is governed by a drag force due to interaction with the background solar wind. These findings also suggest that ICMEs propagating faster than the background solar wind are controlled mainly by the hydrodynamic Stokes drag.
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Abbreviations
- ACE:
-
Advanced Composition Explorer
- AU:
-
Astronomical unit
- CC:
-
Correlation coefficient
- CDAW:
-
Coordinated Data Analysis Workshop
- CME:
-
Coronal mass ejection
- CPI:
-
Comprehensive Plasma Instrumentation
- ESA:
-
European Space Agency
- FOV:
-
Field-of-view
- GSFC:
-
Goddard Space Flight Center
- ICME:
-
Interplanetary coronal mass ejection
- IDED:
-
IPS disturbance event day
- IDEDs:
-
IPS disturbance event days
- IMP:
-
Interplanetary Monitoring Platform
- IPS:
-
Interplanetary Scintillation
- LASCO:
-
Large Angle and Spectrometric Coronagraph
- LOS:
-
Line-of-sight
- MIT:
-
Massachusetts Institute of Technology Faraday Cup Experiment
- NASA:
-
National Aeronautics and Space Administration
- OMNI:
-
Operating Missions as Nodes on the Internet
- SOHO:
-
Solar and Heliospheric Observatory
- STEL:
-
Solar-Terrestrial Environment Laboratory
- STEREO:
-
Solar-Terrestrial Relations Observatory
- SWE:
-
Solar Wind Experiment
- SWEPAM:
-
Solar Wind Electron, Proton, and Alpha Monitor
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Acknowledgements
The IPS observations were carried out under the solar-wind program of the Solar-Terrestrial Environment Laboratory (STEL) of Nagoya University. We acknowledge use of the SOHO/LASCO CME catalog; this CME catalog is generated and maintained at the CDAW Data Center by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between ESA and NASA. We thank NASA/GSFC’s Space Physics Data Facility for use of the OMNIWeb service and OMNI data. We thank the IDL Astronomy User’s Library for the use of IDL software. We acknowledge use of the comprehensive ICME catalog compiled by I.G. Richardson and H.V. Cane. We also thank B.V. Jackson for useful help and comments.
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Iju, T., Tokumaru, M. & Fujiki, K. Radial Speed Evolution of Interplanetary Coronal Mass Ejections During Solar Cycle 23. Sol Phys 288, 331–353 (2013). https://doi.org/10.1007/s11207-013-0297-5
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DOI: https://doi.org/10.1007/s11207-013-0297-5