scholarly journals Interaction between an interplanetary magnetic cloud and the Earth's magnetosphere: Motions of the bow shock

2000 ◽  
Vol 105 (A6) ◽  
pp. 12627-12638 ◽  
Author(s):  
D. J. Wu ◽  
J. K. Chao ◽  
R. P. Lepping
Keyword(s):  
Magnetic Cloud ◽  
Bow Shock ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

The Earth's magnetosphere under continued forcing: Substorm activity during the passage of an interplanetary magnetic cloud

1993 ◽  
Vol 98 (A5) ◽  
pp. 7657-7671 ◽  
Author(s):  
C. J. Farrugia ◽  
M. P. Freeman ◽  
L. F. Burlaga ◽  
R. P. Lepping ◽  
K. Takahashi
Keyword(s):  
Magnetic Cloud ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere ◽  
Substorm Activity

A study of an expanding interplanetary magnetic cloud and its interaction with the Earth's magnetosphere: The interplanetary aspect

1993 ◽  
Vol 98 (A5) ◽  
pp. 7621-7632 ◽  
Author(s):  
C. J. Farrugia ◽  
L. F. Burlaga ◽  
V. A. Osherovich ◽  
I. G. Richardson ◽  
M. P. Freeman ◽  
...  
Keyword(s):  
Magnetic Cloud ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

scholarly journals The evolution of Earth’s magnetosphere during the solar main sequence

2019 ◽  
Vol 489 (4) ◽  
pp. 5784-5801 ◽  
Author(s):  
S Carolan ◽  
A A Vidotto ◽  
C Loesch ◽  
P Coogan
Keyword(s):  
Solar Wind ◽  
Main Sequence ◽  
Solar Rotation ◽  
Strong Shock ◽  
Bow Shock ◽  
Base Temperature ◽  
The Sun ◽  
Earth’S Magnetosphere ◽  
Rotation Rates ◽  
Earth's Magnetosphere

ABSTRACT As a star spins-down during the main sequence, its wind properties are affected. In this work, we investigate how Earth’s magnetosphere has responded to the change in the solar wind. Earth’s magnetosphere is simulated using 3D magnetohydrodynamic models that incorporate the evolving local properties of the solar wind. The solar wind, on the other hand, is modelled in 1.5D for a range of rotation rates Ω from 50 to 0.8 times the present-day solar rotation (Ω⊙). Our solar wind model uses empirical values for magnetic field strengths, base temperature, and density, which are derived from observations of solar-like stars. We find that for rotation rates ≃10 Ω⊙, Earth’s magnetosphere was substantially smaller than it is today, exhibiting a strong bow shock. As the Sun spins-down, the magnetopause standoff distance varies with Ω−0.27 for higher rotation rates (early ages, ≥1.4 Ω⊙) and with Ω−2.04 for lower rotation rates (older ages, <1.4 Ω⊙). This break is a result of the empirical properties adopted for the solar wind evolution. We also see a linear relationship between the magnetopause distance and the thickness of the shock on the subsolar line for the majority of the evolution (≤10 Ω⊙). It is possible that a young fast rotating Sun would have had rotation rates as high as 30–50 Ω⊙. In these speculative scenarios, at 30 Ω⊙, a weak shock would have been formed, but for 50 Ω⊙, we find that no bow shock could be present around Earth’s magnetosphere. This implies that with the Sun continuing to spin-down, a strong shock would have developed around our planet and remained for most of the duration of the solar main sequence.

scholarly journals Current Systems in the Earth's Magnetosphere

2018 ◽  
Vol 56 (2) ◽  
pp. 309-332 ◽  
Author(s):  
N. Yu. Ganushkina ◽  
M. W. Liemohn ◽  
S. Dubyagin
Keyword(s):  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere ◽  
Current Systems
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