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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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ANGEO | Articles | Volume 36, issue 4
Ann. Geophys., 36, 1073-1080, 2018
https://doi.org/10.5194/angeo-36-1073-2018
© Author(s) 2018. This work is distributed under
the Creative Commons Attribution 4.0 License.
Ann. Geophys., 36, 1073-1080, 2018
https://doi.org/10.5194/angeo-36-1073-2018
© Author(s) 2018. This work is distributed under
the Creative Commons Attribution 4.0 License.

Regular paper 08 Aug 2018

Regular paper | 08 Aug 2018

Statistical survey of day-side magnetospheric current flow using Cluster observations: bow shock

Statistical survey of bow shock currents
Evelyn Liebert, Christian Nabert, and Karl-Heinz Glassmeier Evelyn Liebert et al.
  • Institut für Geophysik und extraterrestrische Physik, Technische Universtität Braunschweig, Braunschweig, Germany
Abstract
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We present the first comprehensive statistical survey of the day-side terrestrial bow shock current system based on a large number of Cluster spacecraft bow shock crossings. Calculating the 3-D current densities using fluxgate magnetometer data and the curlometer technique enables the investigation of current locations, directions, and magnitudes in dependence on arbitrary IMF orientation. In case of quasi-perpendicular shock geometries we find that the current properties are in good accordance with theory and existing simulation results. However, currents at quasi-parallel shock geometries next to the foreshock region underlie distinct variations regarding their directions.

1 Introduction
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The terrestrial bow shock slows down the solar wind velocity to subsonic Mach numbers. This is accompanied by a gain in density, temperature, and magnetic field strength. According to Ampère's law the bow shock carries electric currents which account for the jump in the magnetic field components tangential to the bow shock's surface. In contrast to the magnetopause, where the current directions are mainly determined by the geometry of the Earth's magnetic field, the direction of bow shock currents is solely determined by the orientation of the interplanetary magnetic field (IMF).

Depending on the local geometries of the shock surface and IMF orientation one distinguishes between quasi-perpendicular and quasi-parallel shocks where the IMF encounters the bow shock normal with angles above and below 45, respectively. When encountering the compressed magnetic field at the shock some solar wind particles are reflected at the shock and re-accelerated in the solar wind's electric field while gyrating along the IMF direction before they enter the shock another time. At the quasi-parallel shock the reflected particles form the foreshock region where upstream waves are generated and alter the magnetic field configuration.

To date, detailed bow shock current analysis based on in situ measurements has barely been done. Tang et al. (2012) presented a first statistical survey of bow shock currents using Cluster data from 25 crossing events when the IMF was dominated by its Bz component. They selected quasi-perpendicular shocks near the bow shock nose and calculated the current density from the magnetic gradient and the shock thickness. Recently, Hamrin et al. (2017) investigated the currents of 154 quasi-perpendicular bow shock crossings near the shock nose using data from the Magnetospheric Multiscale (MMS) mission. In this paper we extend the statistical survey of bow shock currents at larger distances to the bow shock nose to overall 369 events covering both quasi-perpendicular and quasi-parallel situations during arbitrary IMF configurations for the first time. Making use of the simultaneously collected magnetic field data supplied by the Cluster multi-spacecraft mission (Escoubet et al.2001) and applying the curlometer technique (Dunlop et al.1988) allow a direct 3-D investigation of the local current density vector.

2 Data selection and preparation
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For our investigation we use Cluster magnetic field data from the fluxgate magnetometer (FGM) (Balogh et al.2001) at spin resolution (0.25 Hz). Additionally, data from the Cluster Ion Spectrometry (CIS) instrument (Rème et al.1997) are used to support the identification of bow shock crossings. The data are retrieved from the Cluster Active Archive (Laakso et al.2010). Cluster consists of four individual spacecraft orbiting along a polar orbit with relative separations of a few kilometers up to over 10 000 km. The thickness of the Earth's bow shock is about 100 to 1000 km. In order to match these spatial dimensions we use data obtained during periods when the average inter-spacecraft distance was small at the position of the bow shock. This criterion is fulfilled in the time range from February to May 2002 and from December 2003 to May 2004 when the average inter-spacecraft distance is about 300 km or less. At these times FGM and CIS data are available at the bow shock for 162 inbound and outbound orbit segments.

The curlometer technique estimates the local current density across the Cluster tetrahedron volume by approximating Ampère's law: ×B=μ0J. A thorough introduction to the curlometer technique and an error analysis focussing on our application can be found in our previous publication (Liebert et al.2017), where we conducted a similar study on magnetopause currents. The reliability of curlometer results depends on the Cluster tetrahedron geometry which is constantly changing along its trajectory. One possibility to characterize the shape of the tetrahedron is given by the quality factor QG, which is defined by

(1)QG=true  volumeideal   volume+true   surfaceideal   surface+1

(Glassmeier et al.2001), where the ideal volume and surface represent the volume and surface of a perfect regular tetrahedron with a side length equal to the average side length of the true tetrahedron. The quality factor equals 1 when the true tetrahedron is deformed into a linear geometry and 3 in case the true tetrahedron equals the ideal one. In this study we limit our investigation to bow shock crossings, where the quality factor takes values of 2.5 or more, leaving us 111 orbit segments. The usage of this quality factor for our investigation is discussed in detail by Liebert et al. (2017). QG≥2.5 allows us to expect accuracies of at least 2 to 10 in direction and 3 % to 15 % for the relative error in magnitude.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f01

Figure 1This sketch of the data selection process shows the shrinking number of suitable data sets. From over 2500 Cluster orbits only a few orbit segments match the spatial requirements and the quality criterion for our bow shock current investigation.

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Dunlop et al. (2001) pointed out that high-frequency fluctuations are likely to cause uncertainties within the curlometer results and suggest an appropriate averaging in time before applying the curlometer to magnetic field data. Comparing the effect of averaging windows of different sizes on the events investigated in our study proves the current directions to be quite insensitive to a window size between 20 and 40 s. Significant alteration of the directions sets in for windows below 10 s and above about 60 s as the influence of spatial scales smaller and larger than the bow shock scales rises. Current magnitudes are more sensitive to the size of the averaging window. The damping of high-frequency fluctuation and the associated spatial averaging directly lead to smaller current peak magnitudes. This effect is less intense when an average magnitude per event is calculated instead. For the statistical study presented here, we chose a 30 s averaging window, which proved to be sufficient to damp highly fluctuating current signatures with spatial dimensions far below the tetrahedron size without altering current structures having dimensions of about 50 km and more along the spacecraft trajectory to a significant extent.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f02

Figure 2Example of a bow shock crossing during an outbound orbit on 11 February 2004. The upper and middle panels show Cluster 1 magnetic field data and the curlometer results in GSE coordinates after application of a 30 s averaging window. The lower panel shows Cluster 1 CIS hot ion density n, velocity v, and temperature T. At 16:08 UT the transition from magnetosheath plasma (left-hand side) into undisturbed solar wind plasma (right-hand side) is visible within the particle data as well as within the magnetic field data. During the bow shock crossing a clear current density peak is seen.

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After the application of the curlometer tool, we look for bow shock current events by visual inspection of the curlometer results. Currents are identified as bow shock currents when the following criteria are fulfilled: (1) a clear current peak is visible, and (2) the current event coincides with particle data signatures that are consistent with a bow shock crossing (see the example event in Fig. 2). At each transition event the edges of the corresponding current feature are identified. We calculate the average current directions and magnitude for every event. There are cases where the current or the particle data or both show very fluctuating behavior, making it difficult to identify current structures at a bow shock crossing. In cases where the identification becomes presumably unreliable, the events are omitted and not included in our study.

Caused by relative movement of the bow shock with respect to Cluster, multiple crossings in a row are often recorded along an orbit segment. This enlarges our database for the statistical survey to 369 current events. Figure 3 gives an overview of the locations of all events in GSE coordinates.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f03

Figure 3Location of the investigated bow shock crossings projected onto the reference bow shock presented in a GSE coordinate system. The grey ellipsoids represent the bow shock position at x=0.2,0.5, and 0.8ΔBS with ΔBS depicting the bow shock stand-off distance.

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3 Reference bow shock
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The position and size of the bow shock vary depending on the solar wind conditions to a large extent. For representation of the bow shock crossing locations we introduce a parabolic model reference bow shock as a common frame of reference. Following Nabert et al. (2013) we use the parametrization

(2)x=ΔBS-t=y,zcBS,tt2.

ΔBS depicts the sub-solar bow shock stand-off distance with respect to the center of the Earth (see Fig. 4). The geometric parameters cBS,t represent the bow shock curvature in the t=y and t=z directions. Nabert et al. (2013) deduce values of

(3)cBS,y=0.41ΔBS,cBS,z=0.51ΔBS,

from an analytical zeroth-order approach to solve the MHD equations in the magnetosheath.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f04

Figure 4Sketch of the model bow shock used as a reference bow shock for data presentation. The dotted lines show example projections of two different currents from their true location to the location at the reference bow shock.

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For each identified current the mean value of the tetrahedron barycenter’s position vector is calculated. By radial projection along the Earth-spacecraft line the intersection of this vector with the reference bow shock is calculated (cf. Fig. 4). Figure 3 gives an overview of the location of all events after projection onto the reference bow shock within GSE coordinates.

Current directions at the bow shock are directly controlled by the IMF orientation via Amperè's law. As we do not confine our study to mainly north–south orientated IMF, the presentation of the resulting current directions in a GSE system like in Fig. 3 would lead to a quite chaotic looking distribution and would make it almost impossible to extract useful information from it as the required information about the IMF orientation would not be included in such a picture. In order to account for the varying IMF orientations we conduct a second step of transformation by rotating the coordinate system around the GSE x axis in such a way that the IMFyz,GSE component is orientated in the positive z direction within the new IMF-aligned coordinate system. The IMF is calculated by averaging the magnetic field data obtained during 5 min ahead of each bow shock current event.

4 Results
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4.1 Directions of bow shock currents

Depending on the angle Φ between local shock normal and IMF, current events are categorized into quasi-perpendicular (Φ>45) and quasi-parallel shocks (Φ<45). The majority of 274 of the investigated currents represent quasi-perpendicular geometries. It is likely that this imbalance is caused by our event selection procedure. Within the foreshock region of a quasi-parallel shock oscillations are triggered and develop while the plasma is convected towards the shock surface. This causes fluctuations within the particle and the magnetic field data, leading to less clear plasma transition and current signatures. As described in Sect. 2, events are omitted, when a reliable bow shock current identification is not possible.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f05

Figure 5Frequency distribution of the angle difference between the current directions and the local bow shock normal (a) and the IMF tangential component (b). The angles are binned with 10 intervals.

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Figure 5 shows the orientation of the current flow with respect to the model bow shock normal and the IMF. Most of the observed bow shock currents during quasi-perpendicular geometries lie nearly perpendicular to both the shock normal, which means that the currents flow parallel to the bow shock surface, and the IMF tangential component, as expected from theory. The deviation from perpendicularity with respect to IMFt is much larger in the case of quasi-parallel shock situations (95 events), which reflects more turbulent and fluctuating conditions of the plasma flow adjacent to the foreshock region in contrast to the quasi-perpendicular shock. The broad distribution of the angle between current direction and reference bow shock normal indicates that the current flow direction at the quasi-parallel bow shock deviates extremely from the shape of a simplified bow shock surface.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f06

Figure 6Bow shock current directions in the xy plane (a) and yz plane (b). Jx direction is represented by the colour code. The z axis of the coordinate system is aligned to the IMFyz component. The grey paraboloid and ellipsoids represent the bow shock position at z=0 and x=0.2,0.5, and 0.8ΔBS, respectively. Polar histograms (c) show the occurrence rates of current angles within the yz plane with respect to the positive y axis.

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The global current direction distribution of the quasi-perpendicular and quasi-parallel bow shock currents is displayed in Fig. 6 in the IMF-aligned coordinate systems. The current directions are represented by arrows of normalized length and the color code indicates the direction of currents with respect to the x axis with red arrows pointing towards Earth and green arrows pointing towards the Sun. From theory, within this coordinate system the currents are expected to possess positive y components, independently of their locations. As visible in the yz projections the flow directions are prescribed by the IMF orientation very clearly as they are collectively pointing along the positive y axis in the IMF-aligned coordinate system. The histograms of the Jyz direction in the bottom panel of Fig. 6 illustrate this in a quantitative manner. It shows a very clear peak around 0 in the quasi-perpendicular case. The peak is also visible in the quasi-parallel case, but it is much broader and currents with negative y components are observed frequently.

Having a closer look at the color code and the xy projection reveals that the currents are following the draped shape of the bow shock pointing towards the Sun and Earth at the flanks. Again, more deviations are visible during quasi-parallel bow shock crossings (Fig. 6b). Hamrin et al. (2017) investigated Jx in a similar way. As their events are located near the bow shock nose because of the MMS orbit, they introduced the approximation JxJn, where Jn depicts the portion of the current that flows normal to the shock surface. Their events lie within a range of about 7 Earth radii distance from the Earth–Sun line which approximately corresponds to a distance of about 0.5 ΔBS in our coordinate system. Near the bow shock nose they find that Jx points towards the Sun at y<0 (GSM) and towards Earth at y>0 (GSM) for northward IMF. In the case of southward IMF the current directions are reversed. The distribution of the colors in Fig. 6 shows that the results of the orientation of the Jx component from the study conducted by Hamrin et al. (2017) and from our study are qualitatively identical and are also valid for larger distances from the bow shock nose.

In order to investigate the current normal component in our study, we calculate Jn via the local normal direction of the model bow shock surface for all quasi-perpendicular events. We analyze the orientation of the normal component in dependence on the y coordinate within the IMF-aligned coordinate system. Table 1 gives the occurrence rate of outward and inward orientation of Jn in a region close to the bow shock nose, approximately corresponding to the location of events within the study by Hamrin et al. (2017) as well as a region further away from the nose at the flanks of the bow shock. Based on our results, we can not identify a general dependence of the Jn orientation from the location of the events. Overall, the currents are slightly more often pointing outwards.

Table 1Occurrence rate of outward- and inward-pointing directions of the current normal component at the quasi-perpendicular bow shock depending on the y coordinate within the IMF-aligned coordinate system.

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4.2 Current magnitudes

Figure 7 shows the occurrence distribution of investigated current magnitudes. The majority (about 80 %) do not exceed 30 nA m−2 and the average current magnitude of all events is 19.4 nA m−2. As the current magnitudes calculated by the curlometer are influenced by the averaging in time and space (averaging window, spacecraft separation, average current density along event trajectory), it is more likely that current magnitudes tend to be underestimated than overestimated. A direct comparison of some events which were analyzed in the study by Tang et al. (2012) as well as in our study show that the current density magnitudes calculated with the curlometer technique are factors between 2.7 and 4.5 smaller than those calculated by determination of the layer thickness and the jump in the magnetic field.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f07

Figure 7Occurrence rate of bow shock current magnitudes with a 10 nA m−2 binning interval.

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MHD simulations (Lopez et al.2011) predict a relatively broad region around the bow shock nose where the current magnitudes are constantly high, while the magnitudes are decreasing at the high-latitude bow shock. Investigating the spatial dependence of the event's current magnitudes results in a roughly homogeneous distribution in case of the quasi-parallel shock events which are all located at low latitudes (cf. Fig. 6). In case of quasi-perpendicular events current magnitudes near the bow shock nose are slightly larger than those at the flanks. The average magnitude of all quasi-perpendicular currents below 60 latitude is 22.3 nA m−2, while the average value of currents at higher latitudes is 16.1 nA m−2.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f08

Figure 8Current magnitude in dependence of the IMF tangential component. The IMFt component is calculated via the shock normal direction and is binned into intervals of 1 nT. The current magnitude <JBS> is calculated by averaging over all quasi-perpendicular and all quasi-parallel current events that are ascribed to the corresponding interval.

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The IMF magnitude is another controller of the bow shock current magnitude. Based on Ampère's law and the Rankine–Hugoniot conditions one can expect a linear correlation between the current magnitude and the magnetic field strength of the IMF tangential component with respect to the shock surface

(4)J[Bt]IMFt,

where the brackets denote the jump of the magnetic field across the discontinuity.

Tang et al. (2012) found this linear relation between bow shock current and IMFz component at quasi-perpendicular bow shock events during northward- and southward-orientated IMF. Our survey shows that the linear correlation also applies to arbitrary IMF orientation and shock geometry. Figure 8 displays the average current magnitudes that are calculated for 1 nT intervals of the IMF component tangential to the bow shock surface. For quasi-perpendicular and quasi-parallel cases magnetic field values up to 15 and 8 nT are observed, respectively. Within the range from 0 to 8 nT there are no distinct qualitative differences between quasi-perpendicular and quasi-parallel situations visible.

In the limit of a high Mach number one can derive

(5)J=3IMFt/(μ0L),

where L is the bow shock thickness. The correlation coefficient of the linear fit within Fig. 8 is 0.84. The slope of the fit provides an estimate of the average bow shock thickness of about 1600 km. As mentioned above, it is likely that the magnitudes tend to be underestimated by the curlometer technique. The value of 1600 km therefore represents an upper estimate of the shock thickness. Bale et al. (2003) performed an extensive study of the bow shock thickness which gives a typical scale of a few hundreds of kilometers.

5 Conclusions
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The usage of the curlometer technique allows us a direct investigation of 369 current events recorded within the magnetic field data obtained by Cluster during 111 bow shock crossings in 2002, 2003, and 2004. In 274 cases the bow shock represented a quasi-perpendicular shock (Φ>45). In 95 events a quasi-parallel (Φ<45) shock was observed. It lies adjacent to the foreshock region where solar wind particles are reflected back into the solar wind along the IMF direction and cause upstream and downstream perturbations of the magnetic field configuration.

At quasi-perpendicular shocks the bow shock currents are very clearly described by the IMF direction fulfilling the equation ×B=μ0J. The angle distribution between the bow shock current and IMFt shows a sharp peak at 90. When displayed in an IMFyz-aligned coordinate system the current directions' arrows arrange themselves parallel to each other in the yz plane. As the currents flow parallel to the shock surface, the draped shape of the bow shock becomes visible within the current direction in the xy plane. Current magnitudes are larger near the bow shock nose than at the flanks. Figure 9 is a schematic summary of our results for the currents observed at the day-side quasi-perpendicular bow shock.

https://www.ann-geophys.net/36/1073/2018/angeo-36-1073-2018-f09

Figure 93-D scheme of day-side bow shock current magnitude and orientation with respect to the IMF yz component (GSM) in case of a quasi-perpendicular bow shock. Greater and darker arrows represent higher values of current magnitude.

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The angle distribution between currents and the normal of the reference bow shock peaks at 90 as well, but it is broadened to some extent as the reference bow shock naturally deviates from the true bow shock geometry. The magnitudes of currents at the quasi-perpendicular shock generally increase with an increasing tangential component of the IMF. Typical values of the averaged current magnitudes obtained by the curlometer technique are in the range of 5 to 40 nA m−2 with an average of about 20 nA m−2. Those results are on the same order of magnitude but smaller than the ones determined in former studies by calculating the current density via the jump in the magnetic field and a derived current sheet thickness.

The quasi-parallel shocks that we have found are all located at relatively low latitudes. In this region, we were not able to observe a spatial dependence of the current magnitude. Additionally, the IMF tangential components possess lower values only up to 8 nT. In this range we find that the dependence on the IMF magnitude seems to be qualitatively equal to that observed for quasi-perpendicular situations. In particular the current magnitudes of the quasi-perpendicular and quasi-parallel bow shocks are of a similar size for a given IMF, which is an interesting finding as the ideally (in reality never realized) parallel shock would be accompanied by no jump in the magnetic field and therefore no current at all (Narita2006).

The direction of currents of the quasi-parallel bow shock are less described by the IMF orientation compared to the quasi-perpendicular shock. Overall, the main characteristics are maintained, but far more and larger deviations are visible. In addition, the currents no longer lie perpendicular to the normal direction of the reference bow shock, which indicates that the simplified model bow shock geometry does not hold at the quasi-parallel bow shock.

Data availability
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Data availability. 

All Cluster data used in this study can be retrieved from the Cluster Active Archive (Laakso et al., 2010).

Competing interests
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Competing interests. 

The authors declare that they have no conflict of interest.

Acknowledgements
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Acknowledgements. 

This work was financially supported by the Deutsches Zentrum für Luft- und Raumfahrt under contract 50OC1402. The author thanks the Cluster FGM and CIS teams and the Cluster Science Archive for processing and providing the Cluster data.

The topical editor, Minna Palmroth, thanks two anonymous referees for help in evaluating this paper.

References
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Short summary
At the bow shock the solar wind is slowed down in front of Earth's magnetosphere. This is accompanied by a gain in strength of the magnetic field, which implies that the bow shock carries electric currents. We present the a comprehensive statistical study of bow shock currents making use of multi-point data collected by Cluster spacecraft. We find that the currents depend on the shock geometry and the interplanetary magnetic field and are in good accordance with theory and simulation results.
At the bow shock the solar wind is slowed down in front of Earth's magnetosphere. This is...
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