Professor Andre Balogh

Yamauchi M, Brandt PC, Ebihara Y, Dandouras I, Nilsson H, Lundin R, Reme H, Vallat C, Lindquvist P-A, Balogh A, Daly PWet al., 2006, Source location of the wedge-like dispersed ring current in the morning sector during a substorm, JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 111, ISSN: 2169-9380

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• Citations: 22

Weygand JM, Kivelson MG, Khurana KK, Schwarzl HK, Walker RJ, Balogh A, Kistler LM, Goldstein MLet al., 2006, Non-self-similar scaling of plasma sheet and solar wind probability distribution functions of magnetic field fluctuations, JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 111, ISSN: 2169-9380

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• Citations: 15

Nakamura R, Baumjohann W, Asano Y, Runov A, Balogh A, Owen CJ, Fazakerley AN, Fujimoto M, Klecker B, Reme Het al., 2006, Dynamics of thin current sheets associated with magnetotail reconnection, JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 111, ISSN: 2169-9380

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• Citations: 101

Zhang TL, Baumjohann W, Delva M, Auster H-U, Balogh A, Barabash S, Balikhin M, Berghofer G, Biernat HK, Lammer H, Magnes W, Nakamura R, Penz T, Schwingenschuh K, Voeroes Z, Fornacon K-H, Glassmeier K-H, Richter I, Carr C, Kudela K, Shi JK, Motschmann U, Lebreton J-Pet al., 2006, Magnetic field investigation of the Venus plasma environment:: Expected new results from Venus Express, PLANETARY AND SPACE SCIENCE, Vol: 54, Pages: 1336-1343, ISSN: 0032-0633

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• Citations: 205

Rees A, Balogh A, Horbury TS, 2006, Small-scale solitary wave pulses observed by the Ulysses magnetic field experiment, JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 111, ISSN: 2169-9380

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• Citations: 9

Carr CM, Horbury TS, Balogh A, Bale SD, Baumjohann W, Bavassano B, Breen A, Burgess D, Cargill PJ, Crooker N, Erdös G, Fletcher L, Forsyth RJ, Giacalone J, Glassmeier KH, Hoeksema JT, Goldstein MX, Lockwood M, Magnes W, Maksimovic M, Marsch E, Matthaeus WH, Murphv N, Nakariakov VM, Pacheco JR, Pincon JL, Riley P, Russell CT, Schwartz SJ, Szabo A, Thompson M, Vainio R, Velli M, Vennerstrom S, Walsh R, Wimmer-Schweingruber R, Zank Get al., 2006, A magnetometer for the Solar Orbiter Mission, ISSN: 0379-6566

The magnetometer is a key instrument to the Solar Orbiter mission. The magnetic field is a fundamental parameter in any plasma: a precise and accurate measurement of the field is essential for understanding almost all aspects of plasma dynamics such as shocks and stream-stream interactions. Many of Solar Orbiter's mission goals are focussed around the links between the Sun and space. A combination of in situ measurements by the magnetometer, remote measurements of solar magnetic fields and global modelling is required to determine this link and hence how the Sun affects interplanetary space. The magnetic field is typically one of the most precisely measured plasma parameters and is therefore the most commonly used measurement for studies of waves, turbulence and other small scale phenomena. It is also related to the coronal magnetic field which cannot be measured directly. Accurate knowledge of the magnetic field is essential for the calculation of fundamental plasma parameters such as the plasma beta, Alfven speed and gyroperiod. We describe here the objectives and context of magnetic field measurements on Solar Orbiter and an instrument that fulfils those objectives as defined by the scientific requirements for the mission.

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Cattaneo MBB, Marcucci MF, Retino A, Pallocchia G, Reme H, Dandouras I, Kistler LM, Klecker B, Carlson CW, Korth A, McCarthy M, Lundin R, Balogh Aet al., 2006, Kinetic signatures during a quasi-continuous lobe reconnection event:: Cluster Ion Spectrometer (CIS) observations, JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 111, ISSN: 2169-9380

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• Citations: 14

Xiao CJ, Wang XG, Pu ZY, Zhao H, Wang JX, Ma ZW, Fu SY, Kivelson MG, Liu ZX, Zong QG, Glassmeier KH, Balogh A, Korth A, Reme H, Escoubet CPet al., 2006, <i>In situ</i> evidence for the structure of the magnetic null in a 3D reconnection event in the Earth'smagnetotail, NATURE PHYSICS, Vol: 2, Pages: 478-483, ISSN: 1745-2473

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• Citations: 108

Sonnerup BUO, Haaland S, Paschmann G, Dunlop MW, Reme H, Balogh Aet al., 2006, Orientation and motion of a plasma discontinuity from single-spacecraft measurements:: Generic residue analysis of Cluster data, JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 111, ISSN: 2169-9380

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• Citations: 39

Duan S-P, Liu Z-X, Cao J-B, Shi J-K, Lu L, Li Z-Y, Zong QG, Reme H, Cornilleau-Wehrlin N, Balogh A, Andre Met al., 2006, Analysis of the interaction between low-frequency waves and ions in the high-altitude cusp region observed by satellite cluster, CHINESE PHYSICS LETTERS, Vol: 23, Pages: 1351-1354, ISSN: 0256-307X

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• Citations: 6

Lavraud B, Thomsen MF, Lefebvre B, Schwartz SJ, Seki K, Phan TD, Wang YL, Fazakerley A, Rème H, Balogh Aet al., 2006, Evidence for newly closed magnetosheath field lines at the dayside magnetopause under northward IMF, Journal of Geophysical Research (Space Physics), Vol: 111, Pages: A05211-A05211

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Shi QQ, Shen C, Dunlop MW, Pu ZY, Zong QG, Liu ZX, Lucek E, Balogh Aet al., 2006, Motion of observed structures calculated from multi-point magnetic field measurements: Application to Cluster, GEOPHYSICAL RESEARCH LETTERS, Vol: 33, ISSN: 0094-8276

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• Citations: 104

Thompson SM, Kivelson MG, El-Alaoui M, Balogh A, Réme H, Kistler LMet al., 2006, Bifurcated current sheets:: Statistics from Cluster magnetometer measurements, JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 111, ISSN: 2169-9380

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• Citations: 21

Ren ZP, Lu L, Lei JG, Li ZY, Liu ZX, Balogh A, Rème Het al., 2006, Movement of the magnetic structure in the plasma sheet observed by Cluster II, CHINESE JOURNAL OF GEOPHYSICS-CHINESE EDITION, Vol: 49, Pages: 315-320, ISSN: 0001-5733

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Gazis PR, Balogh A, Dalla S, Decker R, Heber B, Horbury T, Kilchenmann A, Kota J, Kucharek H, Kunow H, Lario D, Potgieter MS, Richardson JD, Riley P, Rodriguez L, Siscoe G, Von Steiger Ret al., 2006, ICMEs at high latitudes and in the outer heliosphere, SPACE SCIENCE REVIEWS, Vol: 123, Pages: 417-451, ISSN: 0038-6308

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• Citations: 11

Wimmer-Schweingruber RF, Crooker NU, Balogh A, Bothmer V, Forsyth RJ, Gazis P, Gosling JT, Horbury T, Kilchenmann A, Richardson IG, Richardson JD, Riley P, Rodriguez L, Von Steiger R, Wurz P, Zurbuchen THet al., 2006, Understanding interplanetary coronal mass ejection signatures, SPACE SCIENCE REVIEWS, Vol: 123, Pages: 177-216, ISSN: 0038-6308

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• Citations: 100

Sahraoui F, Belmont G, Rezeau L, Cornilleau-Wehrlin N, Pinçon JL, Balogh Aet al., 2006, Anisotropic turbulent spectra in the terrestrial magnetosheath as seen by the cluster spacecraft, PHYSICAL REVIEW LETTERS, Vol: 96, ISSN: 0031-9007

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• Citations: 175

Phan TD, Gosling JT, Davis MS, Skoug RM, Oieroset M, Lin RP, Lepping RP, McComas DJ, Smith CW, Reme H, Balogh Aet al., 2006, A magnetic reconnection X-line extending more than 390 Earth radii in the solar wind, NATURE, Vol: 439, Pages: 175-178, ISSN: 0028-0836

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• Citations: 241

Liu Y, Liu R, Fraser BJ, Ables ST, Xu Z, Zhang B, Shi J, Liu Z, Huang D, Hu Z, Chen Z, Xiao W, Dunlop M, Balogh Aet al., 2006, Observation of PC 3/5 magnetic pulsations around the cusp at mid altitude, Pages: 351-356, ISSN: 0379-6566

Since launched in year 2000 the Cluster mission has passed the region around the cusp at mid-altitude (∼6Re) for many times, where ULF wave activities are rich in. From 0800 to 1300UT on October 30 2002 the Cluster spacecrafts ran along an orbit of southern cuspplasmasphere-northern cusp that provides an excellent observation of ULF waves in dayside magnetosphere. Flux gate magnetometer (FGM) data in the GSE system from the spacecrafts were transformed in a field aligned coordinated system, and the results showed that in the equatorial side of the cusp existed plenty of narrow band ULF waves in Pc3-5 range. The frequency band of the ULF waves is confined in narrow Pc5 band near the cusp and evolved into Pc3 band when the spacecrafts went to about L-5 where the plasmasphere is situated. This is consistent with the geomagnetic field line resonance (FLR) theory. However, in the cusp region only broadband waves were observed, which seem to be a magnetosheath-like turbulence due to that the cusp is located in the open field line area where the condition to excite FLR does not be satisfied but plasma disturbance from upstream solar wind is allowed to come into. By this way, a clear wave boundary of the cusp is identified, that is, the transferring position from the broadband waves to the narrow band waves is the right boundary of open field lines to the closed ones.

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Georgescu E, Vaith H, Fornacon KH, Auster U, Balogh A, Carr C, Chutter M, Dunlop M, Foerster M, Glassmeier KH, Gloag J, Paschmann G, Quinn J, Torbert Ret al., 2006, Use of EDI time-of-flight data for FGM calibration check on cluster, Pages: 535-541, ISSN: 0379-6566

The four Cluster satellites launched in summer 2000 carry flux-gate magnetometers (FGM), which measure the magnetic field vector. The satellites also carry electron drift instruments (EDI) that measure the gyration time of electrons perpendicular to the magnetic field. The gyration time is related through a universal constant to the magnetic field magnitude and is hence an absolute measure of it. The knowledge of the field magnitude can be used to verify the magnetometer calibration or to carry out a scalar calibration of FGM, similarly to near-Earth space missions where proton magnetometers provide this information. The resulting increased accuracy of the magnetic field measurement on the four spacecraft enhances the value of the multipoint measurements on Cluster by reducing the uncertainties in deriving the differential quantities such as the curl of the magnetic field. In this paper the errors in the measurements made by FGM and EDI are discussed and a comparison of the measurements is presented. The conclusion is that the absolute error of the magnetic field measurement is about 0.1 nT for fields below 100 nT and less than 0.1% for fields above.

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• Citations: 3

Wild JA, Milan SE, Davies JA, Cowley SWH, Dunlop MW, Owen CJ, Bosqued JM, Lester M, Balogh A, Carr CM, Fazakerley AN, Rème Het al., 2006, Space and ground-based investigations of dayside reconnections: Cluster, double star and superdarn observations, Pages: 199-208, ISSN: 0379-6566

In this paper, we present an overview of several investigations that have exploited Cluster, Double Star and SuperDARN radar data in order to scrutinise the coupling of the solar wind, magnetosphere and ionosphere. The studies introduced have drawn upon simultaneous space- and ground-based data in order to overcome the inherent shortcomings of the in situ (space-based) and remotely-sensed (ground-based) measurement techniques. In particular, we shall highlight the results of studies that investigate the dynamics arising from magnetic reconnection at the dayside magnetopause and the resulting ionospheric responses.

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Cornilleau-Wehrlin N, Attié D, Belraont G, Rezeau L, Robert P, Alleyne HSC, Yearby K, Balogh A, Carr Cet al., 2006, Comparison of ulf waves at magnetopause crossings at different latitudes, as seen by the cluster and double star staff experiments, Pages: 191-197, ISSN: 0379-6566

Strong ULF wave activity has been observed at magnetopause crossings since a long time. Those turbulent like waves are possibly one of the contributors to particle penetration from the Solar Wind to the Magnetosphere through the magnetopause. STAFF Wave experiments onboard Cluster and Double Star TC1 spacecraft permit the comparison of those waves during coordinated crossings, at the same local time, but at different latitude, the TC1 Double Star orbit being nearly equatorial and the Cluster one polar. From a first analysis of simultaneous Cluster and DSP data sets in the first half of year 2004, 21 coordinated magnetopause crossings have been identified, i.e. within less than 3 hours, out of which 16 are within one hour time delay. Some characteristics of the ULF wave data in the vicinity of these crossings are compared, as wave power and frequency spectra power law. Similarities and differences are discussed at the light of solar wind parameters, latitude, local time or time delay between the crossings. These results first confirm the relation between the solar wind pressure and the ULF wave power. They indicate that in most of the cases, the wave power measured by Double Star is stronger than the one measured by the Cluster spacecraft., whereas no local time dependence has been found. If those first results were to be confirmed, it could imply a predominant role of the equatorial plane in the solar wind/ magnetosphere coupling via ULF wave turbulence, with no preference for the sub-solar region.

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Shi JK, Zhang TL, Cheng ZW, Liu ZX, Nakamura R, Carr C, Balogh Aet al., 2006, Field aligned current observed by cluster, Pages: 417-420, ISSN: 0379-6566

In this study, features of the Field Aligned Currents (FACs) distribution in the plasma sheet boundary layer are investigated. The current is calculated with the 4-point measurement of FluxGate Magnetometer (FGM) on board the Cluster in the period of July to October 2001. There are 172 FAC cases/events chosen for statistics. The results show that spatial distribution of the FAC has asymmetry in several aspects. The FACs occurrence is mainly Earthward in dawn side and is mainly tailward in dusk side. The FACs occurrence also has south-north hemisphere asymmetry.

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Zong QG, Fritz TA, Zhang H, Fu SY, Zhou XZ, Goldstein ML, Daly PW, Reme H, Balogh A, Fazakerley ANet al., 2006, The magnetospheric cusp: Structure and dynamics, Advances in Geosciences: Volume 2: Solar Terrestrial (ST), Pages: 173-189, ISBN: 9789812569844

Understanding the polar cusps is essential for a thorough understanding of the entire physics of the magnetosphere, and of the dynamical interaction between the solar wind and any planetary magnetosphere. Energetic electrons are unique to fully assess magnetic Field-Line topology and thus should be able to clearly delineate regions of open and closed magnetic field lines in the High-Latitude regions and contributed crucially to understanding and resolving an internal debate going on between groups measuring only the lower energy (<20 keV) plasma. Energetic electrons with high and stable flux were observed in the high latitude boundary/cusp region when the Interplanetary Magnetic Field (IMF) had a predominate positive Bz component. With measurements at larger separations and more coordination of multiple satellite measurements for particular cusp crossings it will become more evident what the true nature of the cusp is and what roles the cusp plays. The boundary normal, velocity and timing analysis obtained by all four Cluster spacecraft indicates that the multiple cusp phenomena are most likely caused by the oscillation of a single northern cusp which was shifted back and forth. Cusp oscillations with a period of ˜20min are observed by Cluster in the High-Latitude region, whilst the Cold-Dense plasma with fluctuations (20-Min period) are observed in the Dusk-Side of the tail plasma sheet by Geotail. This is consistent with the idea that the high latitude reconnection during northward IMF is the responsible mechanism for the formation of the Cold-Dense plasma sheet.

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• Citations: 2

Eastwood JP, Sibeck DG, Slavin JA, Lavraud B, Lucek EA, Balogh A, Dandouras Iet al., 2006, Observations of flux ropes and X-lines in the near earth magnetotail, European Space Agency, (Special Publication) ESA SP, Pages: 59-66, ISSN: 0379-6566

Magnetic reconnection in the Earth's magnetotail plays a key role in controlling the dynamics of the Earth's magnetosphere. Recent results based on Cluster multi-spacecraft analysis have raised important questions about the traditional interpretation of reconnection-associated phenomena observed by single spacecraft. Cluster has shown that observations conventionally interpreted as a single X-line can correspond to multiple X-line structure [1]. Single point observations cannot distinguish between these two possibilities, and previous interpretations have invoked the simpler picture. This case study is put into a wider context by examining the plasma dynamics following this particular event. Within this picture, one can make the hypothesis that further loop-like structures - small flux ropes - ought to be observed in conjunction with this event. We present such evidence here, and in particular use the curlometer technique to analyse the observations.

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Marchaudon A, Owen CJ, Bosqued JM, Fear RC, Fazakerley AN, Dunlop MW, Lahiff AD, Carr C, Balogh A, Lindqvist PA, Rème Het al., 2006, Simultaneous double star and cluster ftes observations on the dawnside flank of the magnetosphere, Pages: 163-170, ISSN: 0379-6566

We present Cluster and Double Star-1 (TC-1) observations from a close magnetic conjunction on May 8, 2004. The five spacecraft were on the dawnside flank of the magnetosphere, with TC-1 located near the equatorial plane and Cluster at higher geographic latitudes in the southern hemisphere. TC-1, at its apogee, skimmed the magnetopause for almost 8 hours (between 08:00-16:00 UT). Flux Transfer Events (FTEs), moving southward/tailward from the reconnection site, were observed by TC-1 throughout almost all of the period. Cluster, travelling on a mainly dawn-dusk trajectory, crossed the magnetopause at around 10:30 UT in the same Magnetic Local Time (MLT) sector as TC-1 and remained close to the magnetopause boundary layer in the southern hemisphere. The four Cluster spacecraft observed FTEs for a period of 6.5 hours between 07:30 and 14:00 UT. From the properties of these FTEs, the reconnection site was located northward of both TC-1 and Cluster on the dawn flank of the magnetosphere. Reconnection occurred between draped magnetosheath and closed magnetospheric field lines. Despite variable interplanetary magnetic field (IMF) conditions and IMF-B z turnings, the IMF clock-angle remained greater than 70° and the location site appeared to remain relatively stable in position during the whole period. This result is in agreement with previous studies which reported that the dayside reconnection remained active for an IMF clock-angle greater than 70°. The simultaneous observation of FTEs at both Cluster and TC-1, separated by 2 hours in MLT, implies that the reconnection site on the magnetopause must have been extended over several hours in MLT. This event has been already presented in more details in [1].

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Baumjohann W, Matsuoka A, Glassmeier KH, Russell CT, Nagai T, Hoshino M, Nakagawa T, Balogh A, Slavin JA, Nakamura R, Magnes Wet al., 2006, The magnetosphere of Mercury and its solar wind environment: Open issues and scientific questions, 35th COSPAR Scientific Assembly, Publisher: ELSEVIER SCIENCE LTD, Pages: 604-+, ISSN: 0273-1177

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Hasegawa H, Sonnerup BUO, Owen CJ, Klecker B, Paschmann G, Balogh A, Reme Het al., 2006, The structure of flux transfer events recovered from Cluster data, ANNALES GEOPHYSICAE, Vol: 24, Pages: 603-618, ISSN: 0992-7689

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• Citations: 95

Amm O, Nakamura R, Frey HU, Ogawa Y, Kubyshkina M, Balogh A, Reme Het al., 2006, Substorm topology in the ionosphere and magnetosphere during a flux rope event in the magnetotail, ANNALES GEOPHYSICAE, Vol: 24, Pages: 735-750, ISSN: 0992-7689

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• Citations: 11

Németh Z, Facskó G, Erdos G, Balogh Aet al., 2006, Plasma mixing as a cause of solar wind magnetic field variations, 35th COSPAR Scientific Assembly, Publisher: ELSEVIER SCIENCE LTD, Pages: 467-472, ISSN: 0273-1177

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• Citations: 1