What is the best method to calculate the solar wind propagation delay?

Mailyan, B.; Munteanu, Costel; Haaland, Stein

doi:10.5194/angeo-26-2383-2008

Cited by 69 publications

(117 citation statements)

References 48 publications

Supporting

Mentioning

113

Contrasting

Order By: Relevance

“…The time shift of the solar wind measurements in the OMNI data set is done according to the phase front propagation technique, first described in Weimer et al (2003). The validity of this method has been demonstrated recently by Mailyan et al (2008); Weimer and King (2008).…”

Section: Solar Wind and Auxiliary Datamentioning

confidence: 99%

Plasma transport in the magnetotail lobes

et al. 2009

Self Cite

View full text Add to dashboard Cite

Abstract. The Earth's magnetosphere is populated by particles originating from the solar wind and the terrestrial ionosphere. A substantial fraction of the plasma from these sources are convected through the magnetotail lobes. In this paper, we present a statistical study of convective plasma transport through the Earth's magnetotail lobes for various geomagnetic conditions. The results are based on a combination of density measurements from the Electric Field and Waves Experiment (EFW) and convection velocities from the Electron Drift Instrument (EDI) on board the Cluster spacecraft. The results show that variations in the plasma flow is primarily attributed to changes in the convection velocity, whereas the plasma density remains fairly constant and shows little correlation with geomagnetic activity. During disturbed conditions there is also an increased abundance of heavier ions, which combined with enhanced convection, cause an accentuation of the mass flow. The convective transport is much slower than the field aligned transport. A substantial amount of plasma therefore escape downtail without ever reaching the central plasma sheet.

show abstract

Section: Solar Wind and Auxiliary Datamentioning

confidence: 99%

Plasma transport in the magnetotail lobes

et al. 2009

Self Cite

View full text Add to dashboard Cite

show abstract

“…This method applies the so-called phase front propagation technique proposed by Weimer et al (2003) in the modification of the constrained minimum variance calculation MVAB-0 of Haaland et al (2006). Some refinement of this technique was recently presented by Weimer and King (2008) and it is also thoroughly discussed in this issue by Mailyan et al (2008).…”

Section: Ace Solar Wind and Imf Datamentioning

confidence: 99%

High-latitude plasma convection during Northward IMF as derived from in-situ magnetospheric Cluster EDI measurements

et al. 2008

View full text Add to dashboard Cite

Abstract. In this study, we investigate statistical, systematic variations of the high-latitude convection cell structure during northward IMF. Using 1-min-averages of Cluster/EDI electron drift observations above the Northern and Southern polar cap areas for six and a half years (February 2001 till July 2007, and mapping the spatially distributed measurements to a common reference plane at ionospheric level in a magnetic latitude/MLT grid, we obtained regular drift patterns according to the various IMF conditions. We focus on the particular conditions during northward IMF, where lobe cells at magnetic latitudes >80 • with opposite (sunward) convection over the central polar cap are a permanent feature in addition to the main convection cells at lower latitudes. They are due to reconnection processes at the magnetopause boundary poleward of the cusp regions. Mapped EDI data have a particular good coverage within the central part of the polar cap, so that these patterns and their dependence on various solar wind conditions are well verified in a statistical sense. On average, 4-cell convection pattern are shown as regular structures during periods of nearly northward IMF with the tendency of a small shift toward negative clock angles. The positions of these high-latitude convection foci are within 79 • to 85 • magnetic latitude and 09:00-15:00 MLT. The MLT positions are approximately symmetric ±2 h about 11:30 MLT, i.e. slightly offset from midday toward prenoon hours, while the maximum (minimum) potential of the high-latitude cells is at higher magnetic latitudes near their maximum potential difference at ≈−10 • to −15 • clock angle for the North (South) Hemisphere. With increasing clock angle distances from ≈IMFB z +, a gradual transition occurs from the 4-cell pattern via a 3-cell to the Correspondence to: M. Förster (mfo@gfz-potsdam.de) common 2-cell convection pattern, in the course of which one of the medium-scale high-latitude dayside cells diminishes and disappears while the other intensifies and merges with the opposite main cell of the same polarity to form the large "round-shaped" convection cell when approaching a well-known IMFB y -dominated configuration. Opposite scenarios with interchanged roles of the respective cells occur for the opposite turning of the clock angle and at the Southern Hemisphere. The high-latitude dayside cells become more pronounced with increasing magnitude of the IMF vector.

show abstract

“…This simple method has been shown to be adequate when using ACE data since this spacecraft is located fairly close to the Sun-Earth line (see Mailyan et al, 2008). However, in order to account for residual uncertainties in solar wind delay time as well as the response time of the magnetosphere to changes in the external conditions, an instability criterion for the interplanetary field conditions has been utilized.…”

Section: Data Selectionmentioning

confidence: 99%

Cluster observations of near-Earth magnetospheric lobe plasma densities – a statistical study

et al. 2008

Self Cite

View full text Add to dashboard Cite

Abstract. The Cluster-mission has enabled a study of the near-Earth magnetospheric lobes throughout the waning part of solar cycle 23. During the first seven years of the mission the satellites crossed this region of space regularly from about July to October. We have obtained new and more accurate plasma densities in this region based on spacecraft potential measurements from the EFW-instrument. The plasma density measurements are found by converting the potential measurements using a functional relationship between these two parameters. Our observations have shown that throughout this period a full two thirds of the measurements were contained in the range 0.007-0.092 cm −3 irrespective of solar wind conditions or geomagnetic activity. In fact, the most probable density encountered was 0.047 cm −3 , staying roughly constant throughout the entire observation period. The plasma population in this region seems to reflect an equilibrium situation in which the density is independent of the solar wind condition or geomagnetic activity. However, the high density tail of the population (n e >0.2 cm −3 ) seemed to decrease with the waning solar cycle. This points to a source region influenced by the diminishing solar UV/EUVintensity. Noting that the quiet time polar wind has just such a development and that it is magnetically coupled to the lobes, it seems likely to assume that this is a prominent source for the lobe plasma.

show abstract

What is the best method to calculate the solar wind propagation delay?

Cited by 69 publications

References 48 publications

Plasma transport in the magnetotail lobes

Plasma transport in the magnetotail lobes

High-latitude plasma convection during Northward IMF as derived from in-situ magnetospheric Cluster EDI measurements

Cluster observations of near-Earth magnetospheric lobe plasma densities – a statistical study

Contact Info

Product

Resources

About