2,933 research outputs found
Accuracy of multi-point boundary crossing time analysis
Recent multi-spacecraft studies of solar wind discontinuity crossings
using the timing (boundary plane triangulation) method gave boundary
parameter estimates that are significantly different from those of the
well-established single-spacecraft minimum variance analysis (MVA) technique.
A large survey of directional discontinuities in Cluster data turned out
to be particularly inconsistent in the sense that multi-point timing
analyses did not identify any rotational discontinuities (RDs) whereas the
MVA results of the individual spacecraft suggested that RDs form the majority
of events. To make multi-spacecraft studies of discontinuity crossings more
conclusive, the present report addresses the accuracy of the timing approach
to boundary parameter estimation. Our error analysis is based on the reciprocal
vector formalism and takes into account uncertainties both in crossing times
and in the spacecraft positions. A rigorous error estimation scheme is
presented for the general case of correlated crossing time errors
and arbitrary spacecraft configurations. Crossing time error covariances
are determined through cross correlation analyses of the residuals.
The principal influence of the spacecraft array geometry on the accuracy of
the timing method is illustrated using error formulas for the simplified
case of mutually uncorrelated and identical errors at different spacecraft.
The full error analysis procedure is demonstrated for a solar wind
discontinuity as observed by the Cluster FGM instrument
The Hall current system revealed as a statistical significant pattern during fast flows
We have examined the dawn-dusk component of the magnetic field, <I>B<sub>Y</sub></I>, in the night side current sheet during fast flows in the neutral sheet. 237 h of Cluster data from the plasma sheet between 2 August 2002 and 2 October 2002 have been analysed. The spatial pattern of <I>B<sub>Y</sub></I> as a function of the distance from the centre of the current sheet has been estimated by using a Harris current sheet model. We have used the average slopes of these patterns to estimate earthward and tailward currents. For earthward fast flows there is a tailward current in the inner central plasma sheet and an earthward current in the outer central plasma sheet on average. For tailward fast flows the currents are oppositely directed. These observations are interpreted as signatures of Hall currents in the reconnection region or as field aligned currents which are connected with these currents. Although fast flows often are associated with a dawn-dusk current wedge, we believe that we have managed to filter out such currents from our statistical patterns
What is the best method to calculate the solar wind propagation delay?
We present a statistical study of propagation times of solar wind discontinuities between Advanced Composition Explorer (ACE) spacecraft orbiting the L1 libration point and the Cluster quartet of spacecraft near the Earth's magnetopause. The propagation times for almost 200 events are compared with the predicted times from four different models. The simplest model assumes a constant convective motion of solar wind disturbances along the Sun-Earth line, whereas more sophisticated models take the orientation of the discontinuity as well as the real positions of the solar wind monitor and target into account. The results show that taking orientation and real position of the solar wind monitor and target into account gives a more precise time delay estimation in most cases. In particular, we show that recent modifications to the minimum variance technique can improve the estimation of propagation times of solar wind discontinuities
More about arc-polarized structures in the solar wind
We report results from a Cluster-based study of the properties of 28 arc-polarized magnetic structures (also called rotational discontinuities) in the solar wind. These Alfve Ěnic events were selected from the database created and analyzed by Knetter (2005) by use of criteria chosen to elim- inate ambiguous cases. His studies showed that standard, four-spacecraft timing analysis in most cases lacks sufficient accuracy to identify the small normal magnetic field compo- nents expected to accompany such structures, leaving unan- swered the question of their existence. Our study aims to break this impasse. By careful application of minimum vari- ance analysis of the magnetic field (MVAB) from each indi- vidual spacecraft, we show that, in most cases, a small but significantly non-zero magnetic field component was present in the direction perpendicular to the discontinuity. In the very few cases where this component was found to be large, ex- amination revealed that MVAB had produced an unusual and unexplained orientation of the normal vector. On the whole, MVAB shows that many verifiable rotational discontinuities (Bn ̸= 0) exist in the solar wind and that their eigenvalue ratio (EVR=intermediate/minimum variance) can be extremely large (up to EVR = 400). Each of our events comprises four individual spacecraft crossings. The events include 17 ion- polarized cases and 11 electron-polarized ones. Fifteen of the ion events have widths ranging from 9 to 21 ion iner- tial lengths, with two outliers at 46 and 54. The electron- polarized events are generally thicker: nine cases fall in the range 20â71 ion inertial lengths, with two outliers at 9 and 13. In agreement with theoretical predictions from a one- dimensional, ideal, Hall-MHD description (Sonnerup et al., 2010), the ion-polarized events show a small depression in field magnitude, while the electron-polarized ones tend to show a small enhancement
Magnetospheric convection from Cluster EDI measurements compared with the ground-based ionospheric convection model IZMEM
Cluster/EDI electron drift observations above the Northern and Southern polar cap areas for more than seven and a half years (2001â2008) have been used to derive a statistical model of the high-latitude electric potential distribution for summer conditions. Based on potential pattern for different orientations of the interplanetary magnetic field (IMF) in the GSM y-z-plane, basic convection pattern (BCP) were derived, that represent the main characteristics of the electric potential distribution in dependence on the IMF. The BCPs comprise the IMF-independent potential distribution as well as patterns, which describe the dependence on positive and negative IMF<I>B<sub>z</sub></I> and IMF<I>B<sub>y</sub></I> variations. The full set of BCPs allows to describe the spatial and temporal variation of the high-latitude electric potential (ionospheric convection) for any solar wind IMF condition near the Earth's magnetopause within reasonable ranges. The comparison of the Cluster/EDI model with the IZMEM ionospheric convection model, which was derived from ground-based magnetometer observations, shows a good agreement of the basic patterns and its variation with the IMF. According to the statistical models, there is a two-cell antisunward convection within the polar cap for northward IMF<I>B<sub>z</sub></I>+&le;2 nT, while for increasing northward IMF<I>B<sub>z</sub></I>+ there appears a region of sunward convection within the high-latitude daytime sector, which assumes the form of two additional cells with sunward convection between them for IMF<I>B<sub>z</sub></I>+&asymp;4â5 nT. This results in a four-cell convection pattern of the high-latitude convection. In dependence of the &plusmn;IMF<I>B<sub>y</sub></I> contribution during sufficiently strong northward IMF<I>B<sub>z</sub></I> conditions, a transformation to three-cell convection patterns takes place
Discontinuities and Alfvenic Fluctuations in the Solar Wind
We examine the Alfvenicity of a set of 188 solar wind directional discontinuities (DDs) identified in the Cluster data from 2003 by Knetter (2005), with the objective of separating rotational discontinuities (RDs) from tangential ones (TDs). The DDs occurred over the full range of solar wind velocities and magnetic shear angles. By performing the Walen test in the de HoffmannâTeller (HT) frame, we show that 77 of the 127 crossings for which a good HT frame was found had plasma flow speeds exceeding 80 % of the Alfven speed at an average angular deviation of 7.7âŚ; 33 cases had speeds exceeding 90 % of the Alfven speed at an average angle of 6.4âŚ. We show that the angular deviation between flow velocity (in the HT frame) and the Alfven velocity can be obtained from a reduced form of the Walen correlation coefficient
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