scholarly journals Solar wind interaction with comet 67P: Impacts of corotating interaction regions

2016 ◽  
Vol 121 (2) ◽  
pp. 949-965 ◽  
Author(s):  
N. J. T. Edberg ◽  
A. I. Eriksson ◽  
E. Odelstad ◽  
E. Vigren ◽  
D. J. Andrews ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Interaction ◽  
Corotating Interaction Regions ◽  
Interaction Regions ◽  
Comet 67P

scholarly journals Saturn's aurora in the January 2004 events

2006 ◽  
Vol 24 (6) ◽  
pp. 1649-1663 ◽  
Author(s):  
E. S. Belenkaya ◽  
S. W. H. Cowley ◽  
I. I. Alexeev
Keyword(s):  
Solar Wind ◽  
Solar Wind Plasma ◽  
Auroral Oval ◽  
Solar Wind Interaction ◽  
Corotating Interaction Regions ◽  
Plasma Sources ◽  
Interaction Regions ◽  
Magnetosphere Of Saturn ◽  
Average Angle ◽  
The Imf

Abstract. Differences in the solar wind interaction with the magnetosphere of Saturn relative to the Earth result from the decrease in the solar wind plasma density and magnetic field strength with distance from the Sun, and from the change in the average angle of the IMF at Saturn's orbit. Other reasons are related to Saturn's rapid rotation and internal magnetospheric plasma sources. Moreover, the IMF structure observed by Cassini in 2003–2004 during the approach to Saturn is consistent with corotating interaction regions (CIRs) existing during the declining phase of the solar cycle. Two cases on 16 and 26 January 2004 are considered when disturbances in the solar wind passed Cassini and then Saturn. After the solar wind shock encountered the kronian magnetosphere, the auroral oval became brighter (especially at dawn) with a reduced radius. In these cases the auroral power was anti-correlated with the radius of the oval. Possible mechanisms responsible for such unexpected behavior are presented and discussed in detail.

Solar wind flow angle and geoeffectiveness of corotating interaction regions: First results

2017 ◽  
Vol 44 (10) ◽  
pp. 4532-4539 ◽  
Author(s):  
Diptiranjan Rout ◽  
D. Chakrabarty ◽  
P. Janardhan ◽  
R. Sekar ◽  
Vrunda Maniya ◽  
...  
Keyword(s):  
Solar Wind ◽  
Wind Flow ◽  
Corotating Interaction Regions ◽  
Flow Angle ◽  
First Results ◽  
Solar Wind Flow ◽  
Interaction Regions

scholarly journals Solar Wind ∼0.15–1.5 keV Electrons around Corotating Interaction Regions at 1 au

2021 ◽  
Vol 922 (2) ◽  
pp. 198
Author(s):  
Jiawei Tao ◽  
Linghua Wang ◽  
Gang Li ◽  
Robert F. Wimmer-Schweingruber ◽  
Chadi Salem ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Speed ◽  
Kinetic Temperature ◽  
Number Density ◽  
Kappa Index ◽  
Corotating Interaction Regions ◽  
Fast Wind ◽  
Magnetic Field Magnitude ◽  
Interaction Regions ◽  
The Relationship

Abstract Here we present a statistical study of the ∼0.15–1.5 keV suprathermal electrons observed in uncompressed/compressed slow and fast solar wind around 59 corotating interaction regions (CIRs) with good measurements by Wind 3DP from 1995 through 1997. For each of these CIRs, we fit the strahl and halo energy spectra at ∼0.15–1.5 keV to a Kappa function with a Kappa index κ and kinetic temperature T eff. We find that the ∼0.15–1.5 keV strahl electrons behave similarly in both slow and fast wind: the strahl number density n s positively correlates with the solar wind electron temperature T e and interplanetary magnetic field magnitude ∣B∣, while the strahl pitch angle width Θ s decreases with the solar wind speed V sw. These suggest that the strahl electrons are generated by a similar/same process at the Sun in both slow and fast wind that produces these correlations, and the scattering efficiency of strahl in the interplanetary medium (IPM) decreases with V sw. The ∼0.15–1.5 keV halo electrons also behave similarly in both slow and fast wind: the halo parameter positively correlates with the corresponding strahl parameter, and the halo number density n h positively correlates only with T e . These indicate that the halo formation process in the IPM retains most of the strahl properties, but it erases the relationship between n s and ∣B∣. In addition, κ in compressed wind distributes similarly to that in uncompressed wind, for both the strahl and halo. It shows that CIRs at 1 au are not a significant/effective acceleration source for the strahl and halo.

Interplanetary Shock-driven Magnetopause Compressions in Gorgon Global-MHD Simulations

2021 ◽  
Author(s):  
Ravindra Desai ◽  
Jonathan Eastwood ◽  
Joseph Eggington ◽  
Mervyn Freeman ◽  
Martin Archer ◽  
...  
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Interplanetary Shock ◽  
Interplanetary Shocks ◽  
Pressure Balance ◽  
Interplanetary Coronal Mass Ejections ◽  
Corotating Interaction Regions ◽  
Mhd Simulations ◽  
Interaction Regions ◽  
Space Weather Event

<p>Fast-forward interplanetary interplanetary shocks, as occur at the forefront of interplanetary coronal mass ejections and at corotating interaction regions, can rapidly compress the magnetopause inside the drift paths of electrons and protons, and expose geosynchonous satellites directly to the solar wind.  Here, we use Gorgon Global-MHD simulations to study the response of the magnetopause to different fast-forward interplanetary shocks, with strengths extending from the median shocks observed during solar minimum up to that representing an extreme space weather event. The subsequent magnetopause response can be characterised by three distinct phases; an initial acceleration as inertial forces are overcome, a rapid compression well-represented by a power law, and large-scale damped oscillatory motion of the order of an Earth radius, prior to reaching pressure-balance equilibrium. The subsolar magnetopause is found to oscillate with notable frequencies in the range of 2–13 mHz over several periods of diminishing amplitudes.  These results provide an explanation for similar large-scale magnetopause oscillations observed previously during the extreme events of August 1972 and March 1991 and highlight why static magnetopause models break down during periods of strong solar wind driving.</p>

scholarly journals Steepening of magnetosonic waves in the inner coma of comet 67P/Churyumov–Gerasimenko

2021 ◽  
Vol 39 (4) ◽  
pp. 721-742
Author(s):  
Katharina Ostaszewski ◽  
Karl-Heinz Glassmeier ◽  
Charlotte Goetz ◽  
Philip Heinisch ◽  
Pierre Henri ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interaction Region ◽  
Occurrence Rate ◽  
Solar Wind Interaction ◽  
Background Magnetic Field ◽  
The Waves ◽  
Comet 67P ◽  
The Magnetic Field ◽  
Field Enhancements

Abstract. We present a statistical survey of large-amplitude, asymmetric plasma and magnetic field enhancements detected outside the diamagnetic cavity at comet 67P/Churyumov–Gerasimenko from December 2014 to June 2016. Based on the concurrent observations of plasma and magnetic field enhancements, we interpret them to be magnetosonic waves. The aim is to provide a general overview of these waves' properties over the mission duration. As the first mission of its kind, the ESA Rosetta mission was able to study the plasma properties of the inner coma for a prolonged time and during different stages of activity. This enables us to study the temporal evolution of these waves and their characteristics. In total, we identified ∼ 70 000 steepened waves in the magnetic field data by means of machine learning. We observe that the occurrence of these steepened waves is linked to the activity of the comet, where steepened waves are primarily observed at high outgassing rates. No clear indications of a relationship between the occurrence rate and solar wind conditions were found. The waves are found to propagate predominantly perpendicular to the background magnetic field, which indicates their compressional nature. Characteristics like amplitude, skewness, and width of the waves were extracted by fitting a skew normal distribution to the magnetic field magnitude of individual steepened waves. With increasing mass loading, the average amplitude of the waves decreases, while the skewness increases. Using a modified 1D magnetohydrodynamic (MHD) model, we investigated if the waves can be described by the combination of nonlinear and dissipative effects. By combining the model with observations of amplitude, width and skewness, we obtain an estimate of the effective plasma diffusivity in the comet–solar wind interaction region and compare it with suitable reference values as a consistency check. At 67P/Churyumov–Gerasimenko, these steepened waves are of particular importance as they dominate the innermost interaction region for intermediate to high activity.

scholarly journals Rosetta observations of solar wind interaction with the comet 67P/Churyumov-Gerasimenko

2015 ◽  
Vol 583 ◽  
pp. A21 ◽  
Author(s):  
T. W. Broiles ◽  
J. L. Burch ◽  
G. Clark ◽  
C. Koenders ◽  
E. Behar ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Interaction ◽  
Comet 67P
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