scholarly journals Resonant acceleration and heating of solar wind ions by dispersive ion cyclotron waves

1999 ◽  
Vol 104 (A8) ◽  
pp. 17045-17056 ◽  
Author(s):  
You Qiu Hu ◽  
Shadia Rifai Habbal
Keyword(s):  
Solar Wind ◽  
Ion Cyclotron Waves ◽  
Ion Cyclotron ◽  
Resonant Acceleration

scholarly journals Observations of ion cyclotron waves in the solar wind near 0.3 AU

2010 ◽  
Vol 115 (A12) ◽  
pp. n/a-n/a ◽  
Author(s):  
L. K. Jian ◽  
C. T. Russell ◽  
J. G. Luhmann ◽  
B. J. Anderson ◽  
S. A. Boardsen ◽  
...  
Keyword(s):  
Solar Wind ◽  
Ion Cyclotron Waves ◽  
Ion Cyclotron

scholarly journals Properties of A Supercritical Quasi-Perpendicular Interplanetary Shock Propagating in Super-Alfvénic Solar Wind: from MHD to Kinetic Scales

2021 ◽  
Author(s):  
Mingzhe Liu ◽  
Zhongwei Yang ◽  
Ying D. Liu ◽  
Bertrand Lembege ◽  
Karine Issautier ◽  
...  
Keyword(s):  
Solar Wind ◽  
Energy Dissipation ◽  
Interplanetary Shock ◽  
Particle Interactions ◽  
Temperature Anisotropy ◽  
Ion Cyclotron Waves ◽  
Proton Temperature ◽  
Ion Cyclotron ◽  
Mirror Mode

<p>We investigate the properties of an interplanetary shock (M<sub>A</sub>=3.0, θ<sub>Bn</sub>=80°) propagating in Super-Alfvénic solar wind observed on September 12<sup>th,</sup> 1999 with in situ Wind/MFI and Wind/3DP observations. Key results are obtained concerning the possible energy dissipation mechanisms across the shock and how the shock modifies the ambient solar wind at MHD and kinetic scales:  (1) Waves observed in the far upstream of the shock are incompressional and mostly shear Alfvén waves.  (2) In the downstream, the shocked solar wind shows both Alfvénic and mirror-mode features due to the coupling between the Alfvén waves and ion mirror-mode waves.  (3) Specularly reflected gyrating ions, whistler waves, and ion cyclotron waves are observed around the shock ramp, indicating that the shock may rely on both particle reflection and wave-particle interactions for energy dissipation.  (4) Both ion cyclotron and mirror mode instabilities may be excited in the downstream of the shock since the proton temperature anisotropy touches their thresholds due to the enhanced proton temperature anisotropy.  (5) Whistler heat flux instabilities excited around the shock give free energy for the whistler precursors, which help explain the isotropic electron number and energy flux together with the normal betatron acceleration of electrons across the shock.  (6) The shock may be somehow connected to the electron foreshock region of the Earth’s bow shock, since Bx > 0, By < 0, and the electron flux varies only when the electron pitch angles are less than PA = 90°, which should be further investigated. Furthermore, the interaction between Alfvén waves and the shock and how the shock modifies the properties of the Alfvén waves are also discussed.</p>

Over-reflection of magnetoacoustic ion-cyclotron plasma waves

1998 ◽  
Vol 59 (1) ◽  
pp. 1-14
Author(s):  
O. M. EL MEKKI
Keyword(s):  
Solar Wind ◽  
Vortex Sheet ◽  
Plasma Waves ◽  
Ion Cyclotron Waves ◽  
Ion Cyclotron ◽  
Hall Plasma

The over-reflection of magnetoacoustic ion-cyclotron waves in a warm Hall plasma is investigated. It is shown that the effect of the Hall term is to strongly support over-reflection, thereby destabilizing the flow. Its relevance to the current-vortex sheet of the magnetosheath resulting from the interaction of the solar wind and the Earth's magnetopause is pointed out.

scholarly journals Ion cyclotron waves during the Rosetta approach phase: a magnetic estimate of cometary outgassing

2013 ◽  
Vol 31 (12) ◽  
pp. 2201-2206 ◽  
Author(s):  
M. Volwerk ◽  
C. Koenders ◽  
M. Delva ◽  
I. Richter ◽  
K. Schwingenschuh ◽  
...  
Keyword(s):  
Solar Wind ◽  
Wave Power ◽  
Activity Levels ◽  
Water Group ◽  
Ion Cyclotron Waves ◽  
Ion Cyclotron ◽  
Wave Forms ◽  
Outgassing Rate ◽  
Insight Into ◽  
Approach Phase

Abstract. A theoretical model for the ion cyclotron wave generation during the approach phase of Rosetta to 67P/Churyumov–Gerasimenko is presented. For various activity levels of the comet, the crossing of the observational threshold is determined, whose level is derived from the wave power in the undisturbed solar wind near the comet's location during the approach phase at the appropriate frequency. The Giotto flyby at 27P/Grigg–Skjellerup is used to obtain an estimate of how often water-group ion cyclotron waves are observed, and to get insight into the wave forms. At 67P/Churyumov–Gerasimenko one can expect to observe water-group ion cyclotron waves already at a distance of 600 000 km from the nucleus for a nominal outgassing rate of Q = 350 × 1023 molecules per second. The observed first location of cyclotron waves during the Rosetta approach phase will give an indication of the actual outgassing rate of the comet.

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