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Kinematic Properties of Slow ICMEs and an Interpretation of a Modified Drag Equation for Fast and Moderate ICMEs
by
Tokumaru, M.
, Fujiki, K.
, Iju, T.
in
Astrophysics and Astroparticles
/ Atmospheric Sciences
/ Fluid dynamics
/ Hydrodynamics
/ Kinematics
/ Physics
/ Physics and Astronomy
/ Propagation
/ Solar physics
/ Space Exploration and Astronautics
/ Space Sciences (including Extraterrestrial Physics
2014
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Kinematic Properties of Slow ICMEs and an Interpretation of a Modified Drag Equation for Fast and Moderate ICMEs
by
Tokumaru, M.
, Fujiki, K.
, Iju, T.
in
Astrophysics and Astroparticles
/ Atmospheric Sciences
/ Fluid dynamics
/ Hydrodynamics
/ Kinematics
/ Physics
/ Physics and Astronomy
/ Propagation
/ Solar physics
/ Space Exploration and Astronautics
/ Space Sciences (including Extraterrestrial Physics
2014
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Kinematic Properties of Slow ICMEs and an Interpretation of a Modified Drag Equation for Fast and Moderate ICMEs
by
Tokumaru, M.
, Fujiki, K.
, Iju, T.
in
Astrophysics and Astroparticles
/ Atmospheric Sciences
/ Fluid dynamics
/ Hydrodynamics
/ Kinematics
/ Physics
/ Physics and Astronomy
/ Propagation
/ Solar physics
/ Space Exploration and Astronautics
/ Space Sciences (including Extraterrestrial Physics
2014
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Kinematic Properties of Slow ICMEs and an Interpretation of a Modified Drag Equation for Fast and Moderate ICMEs
Journal Article
Kinematic Properties of Slow ICMEs and an Interpretation of a Modified Drag Equation for Fast and Moderate ICMEs
2014
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Overview
We report kinematic properties of slow interplanetary coronal mass ejections (ICMEs) identified by SOHO/LASCO, interplanetary scintillation, and
in situ
observations and propose a modified equation for the ICME motion. We identified seven ICMEs between 2010 and 2011 and compared them with 39 events reported in our previous work. We examined 15 fast (
V
SOHO
−
V
bg
>500 km s
−1
), 25 moderate (0 km s
−1
≤
V
SOHO
−
V
bg
≤500 km s
−1
), and 6 slow (
V
SOHO
−
V
bg
<0 km s
−1
) ICMEs, where
V
SOHO
and
V
bg
are the initial speed of ICMEs and the speed of the background solar wind. For slow ICMEs, we found the following results: i) They accelerate toward the speed of the background solar wind during their propagation and reach their final speed by 0.34±0.03 AU. ii) The acceleration ends when they reach 479±126 km s
−1
; this is close to the typical speed of the solar wind during the period of this study. iii) When
γ
1
and
γ
2
are assumed to be constants, a quadratic equation for the acceleration
a
=−
γ
2
(
V
−
V
bg
)|
V
−
V
bg
| is more appropriate than a linear one
a
=−
γ
1
(
V
−
V
bg
), where
V
is the propagation speed of ICMEs, while the latter gives a smaller
χ
2
value than the former. For the motion of the fast and moderate ICMEs, we found a modified drag equation
a
=−2.07×10
−12
(
V
−
V
bg
)|
V
−
V
bg
|−4.84×10
−6
(
V
−
V
bg
). From the viewpoint of fluid dynamics, we interpret this equation as indicating that ICMEs with 0 km s
−1
≤
V
−
V
bg
≤2300 km s
−1
are controlled mainly by the hydrodynamic Stokes drag force, while the aerodynamic drag force is a predominant factor for the propagation of ICME with
V
−
V
bg
>2300 km s
−1
.
Publisher
Springer Netherlands,Springer Nature B.V
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