Erratum: “Solar wind interaction with the stationary dust can produce drift waves to form nonlinear structures” [Phys. Plasmas 13, 012903 (2006)]

2011 ◽  
Vol 18 (4) ◽  
pp. 049903 ◽  
Author(s):  
H. Saleem
Keyword(s):  
Solar Wind ◽  
Drift Waves ◽  
Nonlinear Structures ◽  
Solar Wind Interaction ◽  
Stationary Dust

The solar wind interaction with Venus through the eyes of the Pioneer Venus Orbiter

2006 ◽  
Vol 54 (13-14) ◽  
pp. 1482-1495 ◽  
Author(s):  
C.T. Russell ◽  
J.G. Luhmann ◽  
R.J. Strangeway
Keyword(s):  
Solar Wind ◽  
Solar Wind Interaction

Solar wind interaction with the Earth's magnetic field: 1. Magnetosheath

1973 ◽  
Vol 78 (19) ◽  
pp. 3714-3730 ◽  
Author(s):  
V. Formisano ◽  
G. Moreno ◽  
F. Palmiotto ◽  
P. C. Hedgecock
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Earth’S Magnetic Field ◽  
Solar Wind Interaction ◽  
Earth's Magnetic Field

Solar Wind Interaction and Pressure Balance at the Dayside Ionopause of Mars

2021 ◽  
Author(s):  
Feng Chu ◽  
Firdevs Duru ◽  
Zachary Girazian ◽  
Robin Ramstad ◽  
Jasper S. Halekas ◽  
...  
Keyword(s):  
Solar Wind ◽  
Pressure Balance ◽  
Solar Wind Interaction

The solar wind interaction with Mars: Consideration of Phobos 2 mission observations of an ion composition boundary on the dayside

1991 ◽  
Vol 96 (A7) ◽  
pp. 11165 ◽  
Author(s):  
T. K. Breus ◽  
A. M. Krymskii ◽  
R. Lundin ◽  
E. M. Dubinin ◽  
J. G. Luhmann ◽  
...  
Keyword(s):  
Solar Wind ◽  
Ion Composition ◽  
Solar Wind Interaction

Selenology: Solar Wind Interaction

Nature ◽  
1971 ◽  
Vol 230 (5290) ◽  
pp. 146-146
Author(s):  
Keyword(s):  
Solar Wind ◽  
Solar Wind Interaction

scholarly journals Magnetosheath-cusp interface

2004 ◽  
Vol 22 (1) ◽  
pp. 183-212 ◽  
Author(s):  
S. Savin ◽  
L. Zelenyi ◽  
S. Romanov ◽  
I. Sandahl ◽  
J. Pickett ◽  
...  
Keyword(s):  
Boundary Layer ◽  
Solar Wind ◽  
Magnetic Fields ◽  
Large Scale ◽  
Traditional Approach ◽  
Qualitative Difference ◽  
Small Scale ◽  
Nonlinear Phenomena ◽  
Solar Wind Interaction ◽  
Linear Superposition

Abstract. We advance the achievements of Interball-1 and other contemporary missions in exploration of the magnetosheath-cusp interface. Extensive discussion of published results is accompanied by presentation of new data from a case study and a comparison of those data within the broader context of three-year magnetopause (MP) crossings by Interball-1. Multi-spacecraft boundary layer studies reveal that in ∼80% of the cases the interaction of the magnetosheath (MSH) flow with the high latitude MP produces a layer containing strong nonlinear turbulence, called the turbulent boundary layer (TBL). The TBL contains wave trains with flows at approximately the Alfvén speed along field lines and "diamagnetic bubbles" with small magnetic fields inside. A comparison of the multi-point measurements obtained on 29 May 1996 with a global MHD model indicates that three types of populating processes should be operative: large-scale (∼few RE) anti-parallel merging at sites remote from the cusp; medium-scale (few thousandkm) local TBL-merging of fields that are anti-parallel on average; small-scale (few hundredkm) bursty reconnection of fluctuating magnetic fields, representing a continuous mechanism for MSH plasma inflow into the magnetosphere, which could dominate in quasi-steady cases. The lowest frequency (∼1–2mHz) TBL fluctuations are traced throughout the magnetosheath from the post-bow shock region up to the inner magnetopause border. The resonance of these fluctuations with dayside flux tubes might provide an effective correlative link for the entire dayside region of the solar wind interaction with the magnetopause and cusp ionosphere. The TBL disturbances are characterized by kinked, double-sloped wave power spectra and, most probably, three-wave cascading. Both elliptical polarization and nearly Alfvénic phase velocities with characteristic dispersion indicate the kinetic Alfvénic nature of the TBL waves. The three-wave phase coupling could effectively support the self-organization of the TBL plasma by means of coherent resonant-like structures. The estimated characteristic scale of the "resonator" is of the order of the TBL dimension over the cusps. Inverse cascades of kinetic Alfvén waves are proposed for forming the larger scale "organizing" structures, which in turn synchronize all nonlinear cascades within the TBL in a self-consistent manner. This infers a qualitative difference from the traditional approach, wherein the MSH/cusp interaction is regarded as a linear superposition of magnetospheric responses on the solar wind or MSH disturbances. Key words. Magnetospheric physics (magnetopause, cusp, and boundary layers) – Space plasma physics (turbulence; nonlinear phenomena)

The solar wind interaction with the geomagnetic field

1970 ◽  
Vol 10 (4) ◽  
Author(s):  
JohnH. Wolfe ◽  
DevrieS. Intriligator
Keyword(s):  
Solar Wind ◽  
Geomagnetic Field ◽  
Solar Wind Interaction
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