scholarly journals A statistical study of interplanetary shocks and pressure pulses internal to magnetic clouds

2007 ◽  
Vol 112 (A6) ◽  
pp. n/a-n/a ◽  
Author(s):  
Michael R. Collier ◽  
Ronald P. Lepping ◽  
Daniel B. Berdichevsky
Keyword(s):  
Statistical Study ◽  
Magnetic Clouds ◽  
Interplanetary Shocks ◽  
Pressure Pulses

scholarly journals Correction to “A statistical study of interplanetary shocks and pressure pulses internal to magnetic clouds”

2007 ◽  
Vol 112 (A9) ◽  
pp. n/a-n/a
Author(s):  
Michael R. Collier ◽  
Ronald P. Lepping ◽  
Daniel B. Berdichevsky
Keyword(s):  
Statistical Study ◽  
Magnetic Clouds ◽  
Interplanetary Shocks ◽  
Pressure Pulses

scholarly journals A summary of WIND magnetic clouds for years 1995-2003: model-fitted parameters, associated errors and classifications

2006 ◽  
Vol 24 (1) ◽  
pp. 215-245 ◽  
Author(s):  
R. P. Lepping ◽  
D. B. Berdichevsky ◽  
C.-C. Wu ◽  
A. Szabo ◽  
T. Narock ◽  
...  
Keyword(s):  
Temperature Drop ◽  
Model Fitting ◽  
Sunspot Cycle ◽  
Flux Rope ◽  
Axial Current ◽  
Model Fit ◽  
Magnetic Clouds ◽  
Symmetric Model ◽  
Large Set ◽  
Interplanetary Shocks

Abstract. Interplanetary magnetic clouds (MCs) have been identified for the first 8.6 years of the WIND mission, and their magnetic field structures have been parameter-fitted by a static, force free, cylindrically-symmetric model (Lepping et al., 1990) with various levels of success. This paper summarizes various aspects of the results of the model fitting by providing: seven estimated model fit-parameter values for each of the 82 MCs found, their objectively determined quality estimates, closest approach vectors (in two coordinate frames), fit-parameter errors for the cases of acceptable quality (50 cases, or 61%), axial magnetic fluxes, axial current densities, and total axial current - as well as some examples of MC profiles for various conditions and "categories" for each case (e.g. Bz: N→S or S→N, etc.). MC quality is estimated from a quantitative consideration of a large set of parameters, such as the chi-squared of the model fit, degree of asymmetry of the B profile, and a comparison of two means of estimating radius. This set of MCs was initially identified by visual inspection of relevant field and plasma data. Each resulting MC candidate is then tested through the use of the MC parameter model, for various adjusted durations to determine the best fit, which helps to refine the boundary-times. The resulting MC set is called Set 1. Another, larger, set (Set 2) of MCs is identified through an automated program whose criteria are based on general MC plasma and field characteristics at 1AU determined through past experience. Set 1 is almost fully contained within Set 2, whose frequency of occurrence better matches that of the sunspot cycle than Set 1. The difference-set (Set 2-Set 1) is referred to as the magnetic cloud-like (MCL) set, whose members do not very well represent good flux ropes through modeling. We present a discussion of how a MC's front boundary is specifically identified in terms of multi-parameter considerations (i.e. any one or more of: increase in B, directional discontinuity, magnetic hole in B, drop in proton plasma beta, B-fluctuation level change, proton temperature drop, etc.), as well as through the application of the flux rope model. Also presented are examples of unusual MCs, as well as some commonly occurring relationships, such as the existence and frequency (approx. 1/2 the time) of upstream interplanetary shocks, and less frequent internal shocks.

scholarly journals Statistical study of the alteration of the magnetic structure of magnetic clouds in the Earth's magnetosheath

2017 ◽  
Vol 122 (3) ◽  
pp. 2956-2972 ◽  
Author(s):  
L. Turc ◽  
D. Fontaine ◽  
C. P. Escoubet ◽  
E. K. J. Kilpua ◽  
A. P. Dimmock
Keyword(s):  
Magnetic Structure ◽  
Statistical Study ◽  
Magnetic Clouds

Fitting of expanding magnetic clouds: A statistical study

2009 ◽  
Vol 57 (12) ◽  
pp. 1375-1380 ◽  
Author(s):  
A. Lynnyk ◽  
M. Vandas
Keyword(s):  
Statistical Study ◽  
Magnetic Clouds

scholarly journals Efficiency of particle acceleration at interplanetary shocks: Statistical study of STEREO observations

2016 ◽  
Vol 588 ◽  
pp. A17 ◽  
Author(s):  
N. Dresing ◽  
S. Theesen ◽  
A. Klassen ◽  
B. Heber
Keyword(s):  
Particle Acceleration ◽  
Statistical Study ◽  
Interplanetary Shocks

scholarly journals From the Sun to the Earth: impact of the 27-28 May 2003 solar events on the magnetosphere, ionosphere and thermosphere

2006 ◽  
Vol 24 (1) ◽  
pp. 129-151 ◽  
Author(s):  
C. Hanuise ◽  
J. C. Cerisier ◽  
F. Auchère ◽  
K. Bocchialini ◽  
S. Bruinsma ◽  
...  
Keyword(s):  
Solar Wind ◽  
High Latitude ◽  
Current System ◽  
Auroral Oval ◽  
Wind Pressure ◽  
Electron Content ◽  
Interplanetary Shocks ◽  
Total Electron ◽  
Pressure Pulses ◽  
Solar Wind Pressure

Abstract. During the last week of May 2003, the solar active region AR 10365 produced a large number of flares, several of which were accompanied by Coronal Mass Ejections (CME). Specifically on 27 and 28 May three halo CMEs were observed which had a significant impact on geospace. On 29 May, upon their arrival at the L1 point, in front of the Earth's magnetosphere, two interplanetary shocks and two additional solar wind pressure pulses were recorded by the ACE spacecraft. The interplanetary magnetic field data showed the clear signature of a magnetic cloud passing ACE. In the wake of the successive increases in solar wind pressure, the magnetosphere became strongly compressed and the sub-solar magnetopause moved inside five Earth radii. At low altitudes the increased energy input to the magnetosphere was responsible for a substantial enhancement of Region-1 field-aligned currents. The ionospheric Hall currents also intensified and the entire high-latitude current system moved equatorward by about 10°. Several substorms occurred during this period, some of them - but not all - apparently triggered by the solar wind pressure pulses. The storm's most notable consequences on geospace, including space weather effects, were (1) the expansion of the auroral oval, and aurorae seen at mid latitudes, (2) the significant modification of the total electron content in the sunlight high-latitude ionosphere, (3) the perturbation of radio-wave propagation manifested by HF blackouts and increased GPS signal scintillation, and (4) the heating of the thermosphere, causing increased satellite drag. We discuss the reasons why the May 2003 storm is less intense than the October-November 2003 storms, although several indicators reach similar intensities.

scholarly journals Multisatellite observations of the magnetosphere response to changes in the solar wind and interplanetary magnetic field

2018 ◽  
Author(s):  
Galina Korotova ◽  
David Sibeck ◽  
Scott Thaller ◽  
John Wygant ◽  
Harlan Spence ◽  
...  
Keyword(s):  
Electric Field ◽  
Statistical Study ◽  
Azimuthal Velocity ◽  
Local Times ◽  
Interplanetary Shocks ◽  
Electrical Field ◽  
Normal Orientation ◽  
Statistical Studies ◽  
The Given

Abstract. We employ multipoint observations of the magnetosphere to present case and statistical studies of the electromagnetic field and plasma response to interplanetary (IP) shocks. On February 27, 2014 the initial encounter of an IP shock with the magnetopause occurred on the early postnoon magnetosphere, consistent with the observed alignment of the shock with the spiral IMF. The dayside equatorial magnetosphere exhibited a dusk-dawn oscillatory electrical field with a period of ~ 330 s and peak to peak amplitudes of ~ 15 mV/m for a period of 30 min. The intensity of electrons in the energy range from 31.5 to 342 KeV responded with periods corresponding to the shock induced ULF electric field waves. The initial electric field perturbation was directed dawnward for this case study. We then perform a statistical study of Ey variations of the electric field and associated plasma drift Vx and Vy flow velocities for 30 magnetospheric events during the passage of interplanetary shocks. The direction of the initial Vx component of plasma flow is tailward at all local times except the nightside magnetosphere, where flows are sunward near the sun-Earth line but antisunward towards dawn and dusk. The observed directions of the azimuthal velocity Vy predominately agree with those expected for the given spiral or orthospiral shock normal orientation.

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