scholarly journals Near-Earth plasma sheet azimuthal pressure gradient and associated auroral development soon before substorm onset

2011 ◽  
Vol 116 (A7) ◽  
pp. n/a-n/a ◽  
Author(s):  
X. Xing ◽  
L. R. Lyons ◽  
Y. Nishimura ◽  
V. Angelopoulos ◽  
E. Donovan ◽  
...  
Keyword(s):  
Pressure Gradient ◽  
Plasma Sheet ◽  
Substorm Onset

scholarly journals Correlation between ground-based observations of substorm signatures and magnetotail dynamics

2005 ◽  
Vol 23 (3) ◽  
pp. 997-1011 ◽  
Author(s):  
E. Borälv ◽  
H. J. Opgenoorth ◽  
K. Kauristie ◽  
M. Lester ◽  
J.-M. Bosqued ◽  
...  
Keyword(s):  
Solar Wind ◽  
Event Study ◽  
Plasma Sheet ◽  
Sheet Thickness ◽  
Substorm Onset ◽  
Boundary Motion ◽  
Thickness Variations ◽  
Magnetotail Dynamics

Abstract. We present a substorm event study using the four Cluster spacecraft in combination with ground-based instruments, in order to perform simultaneous observations in the ionosphere and magnetotail. We show good correlation between substorm signatures on the ground and in the magnetotail, even though data from the northern-ground and southern-tail hemispheres are compared. During this event ground-based magnetometers show a substorm onset over Scandinavia in the pre-midnight sector. Within 1.5h the onset and three intensifications are apparent in the magnetograms. For all the substorm signatures seen on the ground, corresponding plasma sheet boundary motion is visible at Cluster, located at a downtail distance of 18.5 RE. As a result of the substorm onset and intensifications, Cluster moves in and out between the southern plasma sheet and lobe. Due to the lack of an apparent solar wind driver and the good correlation between substorm signatures on the ground, we conclude the substorm itself is the driver for these plasma sheet dynamics. We show that in the scales of Cluster inter-spacecraft distances (~0.5 RE) the inferred plasma sheet motion is often directed in both Ygsm- and Zgsm-directions, and discuss this finding in the context of previous studies of tail flapping and plasma sheet thickness variations.

Nonadiabatic heating of the central plasma sheet at substorm onset

1992 ◽  
Vol 97 (A2) ◽  
pp. 1481 ◽  
Author(s):  
C. Y. Huang ◽  
L. A. Frank ◽  
G. Rostoker ◽  
J. Fennell ◽  
D. G. Mitchell
Keyword(s):  
Plasma Sheet ◽  
Substorm Onset ◽  
Central Plasma ◽  
Central Plasma Sheet

scholarly journals Enhanced transport across entire length of plasma sheet boundary field lines leading to substorm onset

2010 ◽  
Vol 115 (A5) ◽  
pp. n/a-n/a ◽  
Author(s):  
L. R. Lyons ◽  
Y. Nishimura ◽  
X. Xing ◽  
V. Angelopoulos ◽  
S. Zou ◽  
...  
Keyword(s):  
Plasma Sheet ◽  
Substorm Onset ◽  
Entire Length ◽  
Boundary Field ◽  
Field Lines

The magnetic flux transport along the -Esw direction in the magnetotails on Mars and Venus

2020 ◽  
Author(s):  
Lihui Chai ◽  
James Slavin ◽  
Yong Wei ◽  
Weixing Wan ◽  
Charlie F. Bowers ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Flux ◽  
Pressure Gradient ◽  
Plasma Sheet ◽  
Magnetic Pressure ◽  
Mass Loading ◽  
Flux Transport ◽  
Loading Effect

<p>The induced magnetotails on Mars and Venus are considered to arise through the interplanetary magnetic field (IMF) draping around the planet and the solar wind deceleration due to the mass loading effect. They have very similar structures as that on Earth, two magnetic lobes of opposite radial magnetic fields and a plasma sheet in between. However, the orientation and geometry of the induced magnetotails are controlled by the IMF, not the planetary intrinsic magnetic field. In this study, we present another characteristic of the induced magnetotails on Mars and Venus with the observations of MAVEN and Venus Express. It is found that the magnetic flux in the induced magnetotails on Mars and Venus are inhomogeneous. There is more magnetic flux in the +E hemisphere than -E hemisphere. The magnetic flux is observed to transport gradually from the +E hemisphere to the -E hemisphere along the magnetotail. The magnetotail magnetic flux transport seems to be faster on Mars than that at Venus. Based on these observations, we suggest that the finite gyro-radius effect of the planetary ions that are picked up by the solar wind is responsible to the magnetic flux inhomogeneity and transport in the induced magnetotails. The role of the magnetic pressure gradient in the magnetotail will be discussed.</p>

scholarly journals Ionospheric signatures of a plasma sheet rebound flow during a substorm onset

2013 ◽  
Vol 118 (1) ◽  
pp. 350-363 ◽  
Author(s):  
L. Juusola ◽  
M. Kubyshkina ◽  
R. Nakamura ◽  
T. Pitkänen ◽  
O. Amm ◽  
...  
Keyword(s):  
Plasma Sheet ◽  
Substorm Onset

A multisatellite study of the plasma sheet dynamics at substorm onset

1984 ◽  
Vol 11 (5) ◽  
pp. 500-503 ◽  
Author(s):  
J. A. Sauvaud ◽  
A. Saint-Marc ◽  
J. Dandouras ◽  
H. Rème ◽  
A. Korth ◽  
...  
Keyword(s):  
Plasma Sheet ◽  
Substorm Onset
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