Simultaneous Observations of Solar-Flare Electron Spectra in Interplanetary Space and Within Earth's Magnetosphere

1971 ◽  
Vol 26 (8) ◽  
pp. 458-463 ◽  
Author(s):  
H. I. West ◽  
A. L. Vampola
Keyword(s):  
Solar Flare ◽  
Interplanetary Space ◽  
Earth’S Magnetosphere ◽  
Electron Spectra ◽  
Earth's Magnetosphere

scholarly journals Space Weather, SuperDARN and the Tasmanian Tiger

1997 ◽  
Vol 50 (4) ◽  
pp. 773 ◽  
Author(s):  
Raymond A. Greenwald
Keyword(s):  
Solar Wind ◽  
Electric Fields ◽  
Space Weather ◽  
Interplanetary Space ◽  
Rapid Evolution ◽  
Upper Atmosphere ◽  
Global Network ◽  
Pressure Gradients ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

The plasma environment extending from the solar surface through interplanetary space to the outermost reaches of the Earth’s atmosphere and magnetic field is dynamic, often disturbed, and capable of harming humans and damaging manmade systems. Disturbances in this environment have been identified as space weather disturbances. At the present time there is growing interest in monitoring and predicting space weather disturbances. In this paper we present some of the difficulties involved in achieving this goal by comparing the processes that drive tropospheric-weather systems with those that drive space-weather systems in the upper atmosphere and ionosphere. The former are driven by pressure gradients which result from processes that heat and cool the atmosphere. The latter are driven by electric fields that result from interactions between the streams of ionised gases emerging from the Sun (solar wind) and the Earth’s magnetosphere. Although the dimensions of the Earth’s magnetosphere are vastly greater than those of tropospheric weather systems, the global space-weather response to changes in the solar wind is much more rapid than the response of tropospheric-weather systems to changing conditions. We shall demonstrate the rapid evolution of space-weather systems in the upper atmosphere through measurements with a global network of radars known as SuperDARN. We shall also describe how the SuperDARN network is evolving, including a newly funded Australian component known as the Tasman International Geospace Environmental Radar (TIGER).

Solar flare effects in the Earth’s magnetosphere

2021 ◽  
Author(s):  
Jing Liu ◽  
Wenbin Wang ◽  
Liying Qian ◽  
William Lotko ◽  
Alan G. Burns ◽  
...  
Keyword(s):  
Solar Flare ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere ◽  
Solar Flare Effects

A model of radiation conditions during spacecraft flights in the interplanetary space and in the earth's magnetosphere

1992 ◽  
Vol 12 (2-3) ◽  
pp. 441-444 ◽  
Author(s):  
I.V. Getselev ◽  
P.P. Ignatiev ◽  
N.A. Kabashova ◽  
N.N. Kontor ◽  
A.R. Moszhukhina ◽  
...  
Keyword(s):  
Interplanetary Space ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere ◽  
Radiation Conditions

scholarly journals The physics of space weather/solar-terrestrial physics (STP): what we know now and what the current and future challenges are

2020 ◽  
Vol 27 (1) ◽  
pp. 75-119 ◽  
Author(s):  
Bruce T. Tsurutani ◽  
Gurbax S. Lakhina ◽  
Rajkumar Hajra
Keyword(s):  
Solar Wind ◽  
Space Weather ◽  
Energetic Particle ◽  
High Speed ◽  
Geomagnetic Storms ◽  
Interplanetary Space ◽  
Magnetic Clouds ◽  
Slow Solar Wind ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

Abstract. Major geomagnetic storms are caused by unusually intense solar wind southward magnetic fields that impinge upon the Earth's magnetosphere (Dungey, 1961). How can we predict the occurrence of future interplanetary events? Do we currently know enough of the underlying physics and do we have sufficient observations of solar wind phenomena that will impinge upon the Earth's magnetosphere? We view this as the most important challenge in space weather. We discuss the case for magnetic clouds (MCs), interplanetary sheaths upstream of interplanetary coronal mass ejections (ICMEs), corotating interaction regions (CIRs) and solar wind high-speed streams (HSSs). The sheath- and CIR-related magnetic storms will be difficult to predict and will require better knowledge of the slow solar wind and modeling to solve. For interplanetary space weather, there are challenges for understanding the fluences and spectra of solar energetic particles (SEPs). This will require better knowledge of interplanetary shock properties as they propagate and evolve going from the Sun to 1 AU (and beyond), the upstream slow solar wind and energetic “seed” particles. Dayside aurora, triggering of nightside substorms, and formation of new radiation belts can all be caused by shock and interplanetary ram pressure impingements onto the Earth's magnetosphere. The acceleration and loss of relativistic magnetospheric “killer” electrons and prompt penetrating electric fields in terms of causing positive and negative ionospheric storms are reasonably well understood, but refinements are still needed. The forecasting of extreme events (extreme shocks, extreme solar energetic particle events, and extreme geomagnetic storms (Carrington events or greater)) are also discussed. Energetic particle precipitation into the atmosphere and ozone destruction are briefly discussed. For many of the studies, the Parker Solar Probe, Solar Orbiter, Magnetospheric Multiscale Mission (MMS), Arase, and SWARM data will be useful.

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