scholarly journals Global hybrid simulations: Foreshock waves and cavitons under radial interplanetary magnetic field geometry

2009 ◽  
Vol 114 (A1) ◽  
pp. n/a-n/a ◽  
Author(s):  
X. Blanco-Cano ◽  
N. Omidi ◽  
C. T. Russell
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Field Geometry ◽  
Hybrid Simulations

Interplanetary magnetic field control of magnetotail magnetic field geometry: IMP 8 observations

1994 ◽  
Vol 99 (A6) ◽  
pp. 11113 ◽  
Author(s):  
Zerefsan Kaymaz ◽  
George L. Siscoe ◽  
Janet G. Luhmann ◽  
Ronald P. Lepping ◽  
Christopher T. Russell
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Field Control ◽  
Field Geometry

Effects of the Solar Wind Conditions on Mercury's Exosphere: Hybrid Simulations

2020 ◽  
Author(s):  
Pavel M. Travnicek ◽  
Dave Schriver ◽  
Thomas Orlando ◽  
James A. Slavin
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Dynamic Pressure ◽  
Energy Levels ◽  
Solar Wind Plasma ◽  
Deposited Energy ◽  
Solar Wind Parameters ◽  
Primary Focus ◽  
Hybrid Simulations

<pre class="western">We carry out a set of global hybrid simulations of the Mercury's magnetosphere with the interplanetary magnetic field oriented in the desired directions. <br />We study effects of changes of different solar wind parameters on the structure of the plasma circulation within Mercury’s magnetosphere. We focus our <br />study on the changes caused by changes in the orientation of the interplanetary magnetic field and the dynamic pressure (velocity) of the solar wind. <br />We study the structure of the of the Mercury’s magnetosphere under different solar wind conditions. Our primary focus is the assessment of the <br />precipitation levels of solar wind hydrogen on the Mercury's surface (the amount, the deposited energy, its spectra and angular distribution) and on the <br />formation of Mercury's exosphere. We examine density fluxes, energy levels and spectra of protons precipitating on Mercury’s surface as a function of <br />longitude and altitude. It has been established, that Mercury has a plasma belt formed by quasi-trapped solar wind plasma close to the Mercury’s surface. <br />Charged particles trapped in the belt mostly circle Mercury 1-2 times before they either precipitate on Mercury’s surface or escape into the Mercury’s <br />magnetospheric cavity. Lower dynamic pressure of the solar wind pushes magnetopause up above the Mercury’s surface and the plasma belt has more <br />space to develop. Its interaction with Mercury’s surface and dynamics under different solar wind conditions is essential on the precipitation of the plasma <br />on the Mercury’s surface. Higher dynamic pressure of the solar wind can push the bow shock towards Mercury’s surface and make the surface open to the <br />direct impact of the solar wind on the Mercury’s surface. Due to weak magnetic moment of the Mercury’s magnetosphere, the plasma environment at Mercury <br />is very dynamic.</pre>

H-Cmes and Ii-Type Radio Bursts Related Intense Geomagnetic Storms in Relation With Interplanetary Magnetic Field and Solar Wind Disturbances

2012 ◽  
Vol 2 (10) ◽  
pp. 1-3 ◽  
Author(s):  
Praveen Kumar Gupta ◽  
◽  
Puspraj Singh Puspraj Singh ◽  
Puspraj Singh Puspraj Singh ◽  
P. K. Chamadia P. K. Chamadia
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Geomagnetic Storms ◽  
Radio Bursts ◽  
Solar Wind Disturbances

The polarity pattern of the interplanetary magnetic field during solar rotations 1798-1808

1967 ◽  
Vol 72 (5) ◽  
pp. 1637-1643 ◽  
Author(s):  
Paul J. Coleman ◽  
Leverett Davis ◽  
Edward J. Smith ◽  
Douglas E. Jones
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field

Characteristics of the association between the interplanetary magnetic field and substorms

1977 ◽  
Vol 82 (29) ◽  
pp. 4837-4842 ◽  
Author(s):  
Michael N. Caan ◽  
Robert L. McPherron ◽  
Christopher T. Russell
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field

scholarly journals Interplanetary magnetic field control of Saturn's polar cusp aurora

2005 ◽  
Vol 23 (4) ◽  
pp. 1405-1431 ◽  
Author(s):  
E. J. Bunce ◽  
S. W. H. Cowley ◽  
S. E. Milan
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Field Line ◽  
High Latitude ◽  
Closed Field ◽  
Vortical Flows ◽  
Dayside Magnetopause ◽  
Closed Field Line ◽  
Lobe Reconnection

Abstract. Dayside UV emissions in Saturn's polar ionosphere have been suggested to be the first observational evidence of the kronian "cusp" (Gérard et al., 2004). The emission has two distinct states. The first is a bright arc-like feature located in the pre-noon sector, and the second is a more diffuse "spot" of aurora which lies poleward of the general location of the main auroral oval, which may be related to different upstream interplanetary magnetic field (IMF) orientations. Here we take up the suggestion that these emissions correspond to the cusp. However, direct precipitation of electrons in the cusp regions is not capable of producing significant UV aurora. We have therefore investigated the possibility that the observed UV emissions are associated with reconnection occurring at the dayside magnetopause, possibly pulsed, akin to flux transfer events seen at the Earth. We devise a conceptual model of pulsed reconnection at the low-latitude dayside magnetopause for the case of northwards IMF which will give rise to pulsed twin-vortical flows in the magnetosphere and ionosphere in the vicinity of the open-closed field-line boundary, and hence to bi-polar field-aligned currents centred in the vortical flows. During intervals of high-latitude lobe reconnection for southward IMF, we also expect to have pulsed twin-vortical flows and corresponding bi-polar field-aligned currents. The vortical flows in this case, however, are displaced poleward of the open-closed field line boundary, and are reversed in sense, such that the field-aligned currents are also reversed. For both cases of northward and southward IMF we have also for the first time included the effects associated with the IMF By effect. We also include the modulation introduced by the structured nature of the solar wind and IMF at Saturn's orbit by developing "slow" and "fast" flow models corresponding to intermediate and high strength IMF respectively. We then consider the conditions under which the plasma populations appropriate to either sub-solar reconnection or high-latitude lobe reconnection can carry the currents indicated. We have estimated the field-aligned voltages required, the resulting precipitating particle energy fluxes, and the consequent auroral output. Overall our model of pulsed reconnection under conditions of northwards and southwards IMF, and for varying orientations of IMF By, is found to produce a range of UV emission intensities and geometries which is in good agreement with the data presented by Gérard et al. (2004). The recent HST-Cassini solar wind campaign provides a unique opportunity to test the theoretical ideas presented here.

Sign in / Sign up

Export Citation Format

Share Document