scholarly journals An improved empirical model of electron and ion fluxes at geosynchronous orbit based on upstream solar wind conditions

Space Weather ◽  
2016 ◽  
Vol 14 (7) ◽  
pp. 511-523 ◽  
Author(s):  
M. H. Denton ◽  
M. G. Henderson ◽  
V. K. Jordanova ◽  
M. F. Thomsen ◽  
J. E. Borovsky ◽  
...  
Keyword(s):  
Solar Wind ◽  
Empirical Model ◽  
Ion Fluxes ◽  
Geosynchronous Orbit ◽  
Upstream Solar Wind

scholarly journals An empirical model of electron and ion fluxes derived from observations at geosynchronous orbit

Space Weather ◽  
2015 ◽  
Vol 13 (4) ◽  
pp. 233-249 ◽  
Author(s):  
M. H. Denton ◽  
M. F. Thomsen ◽  
V. K. Jordanova ◽  
M. G. Henderson ◽  
J. E. Borovsky ◽  
...  
Keyword(s):  
Empirical Model ◽  
Ion Fluxes ◽  
Geosynchronous Orbit

scholarly journals Density holes in the upstream solar wind

2007 ◽  
Author(s):  
G. K. Parks ◽  
E. Lee ◽  
N. Lin ◽  
F. Mozer ◽  
M. Wilber ◽  
...  
Keyword(s):  
Solar Wind ◽  
Upstream Solar Wind

scholarly journals A magnetodisc model service for planetary space weather studies

2019 ◽  
Vol 9 ◽  
pp. A24
Author(s):  
Nicholas Achilleos ◽  
Patrick Guio ◽  
Nicolas André ◽  
Arianna M. Sorba
Keyword(s):  
Solar Wind ◽  
Space Weather ◽  
Theoretical Models ◽  
Plasma Pressure ◽  
Space Environment ◽  
Solar Wind Flow ◽  
Physical Response ◽  
Global Magnetic Field ◽  
Upstream Solar Wind ◽  
Azimuthal Current

Theoretical models play an important role in the Planetary Space Weather Services (PSWS) of the European Planetary Network (“Europlanet”), due to their ability to predict the physical response of magnetospheric environments to compressions or rarefactions in the upstream solar wind flow. We illustrate this aspect by presenting examples of some calculations done with the UCL Magnetodisc Model in both “Jupiter” and “Saturn” mode. Similar model outputs can now be provided via the PSWS MAGNETODISC service. For each planet’s space environment, we present example model outputs showing the effect of compressions and rarefactions on the global magnetic field, plasma pressure and azimuthal current density. As a simple illustration of the physics underlying these reference models, we quantify solar wind effects by comparing the “compressed” and “expanded” outputs to a nominal “average-state” model, reflecting more typical solar wind dynamic pressures. We also describe the implementation of the corresponding PSWS MAGNETODISC Service, through which similar outputs may be obtained by potential users.

scholarly journals MAVEN observations on a hemispheric asymmetry of precipitating ions toward the Martian upper atmosphere according to the upstream solar wind electric field

2017 ◽  
Vol 122 (1) ◽  
pp. 1083-1101 ◽  
Author(s):  
Takuya Hara ◽  
Janet G. Luhmann ◽  
François Leblanc ◽  
Shannon M. Curry ◽  
Kanako Seki ◽  
...  
Keyword(s):  
Solar Wind ◽  
Electric Field ◽  
Hemispheric Asymmetry ◽  
Upper Atmosphere ◽  
Upstream Solar Wind

Solar Wind Interaction With Jupiter's Magnetosphere: A Statistical Study of Galileo In Situ Data and Modeled Upstream Solar Wind Conditions

2019 ◽  
Vol 124 (12) ◽  
pp. 10170-10199 ◽  
Author(s):  
Marissa F. Vogt ◽  
Szilard Gyalay ◽  
Elena A. Kronberg ◽  
Emma J. Bunce ◽  
William S. Kurth ◽  
...  
Keyword(s):  
Solar Wind ◽  
Statistical Study ◽  
Solar Wind Interaction ◽  
In Situ Data ◽  
Upstream Solar Wind

Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock

Nature ◽  
2008 ◽  
Vol 454 (7200) ◽  
pp. 63-66 ◽  
Author(s):  
John D. Richardson ◽  
Justin C. Kasper ◽  
Chi Wang ◽  
John W. Belcher ◽  
Alan J. Lazarus
Keyword(s):  
Solar Wind ◽  
Termination Shock ◽  
Upstream Solar Wind
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