Articles | Volume 42, issue 2
https://doi.org/10.5194/angeo-42-371-2024
© Author(s) 2024. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
https://doi.org/10.5194/angeo-42-371-2024
© Author(s) 2024. This work is distributed under
the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
Regular paper
| 
12 Sep 2024
Regular paper |
| 12 Sep 2024
| 12 Sep 2024
The Cluster spacecrafts' view of the motion of the high-latitude magnetopause
Niklas Grimmich
CORRESPONDING AUTHOR
Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
Ferdinand Plaschke
Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
Benjamin Grison
Department of Space Physics, Institute of Atmospheric Physics Czech Academy of Sciences, Praha, Czech Republic
Fabio Prencipe
Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
Christophe Philippe Escoubet
ESA European Space Research and Technology Centre, Noordwijk, the Netherlands
Martin Owain Archer
Department of Physics, Imperial College London, London, UK
Ovidiu Dragos Constantinescu
Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
Institute for Space Sciences, Bucharest, Romania
Stein Haaland
Birkeland Centre for Space Science, University of Bergen, Bergen, Norway
Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany
The University Center in Svalbard, Longyearbyen, Norway
Rumi Nakamura
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
David Gary Sibeck
NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
Fabien Darrouzet
Royal Belgian Institute for Space Aeronomy, Brussels, Belgium
Mykhaylo Hayosh
Department of Space Physics, Institute of Atmospheric Physics Czech Academy of Sciences, Praha, Czech Republic
Romain Maggiolo
Royal Belgian Institute for Space Aeronomy, Brussels, Belgium
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Martin O. Archer
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Patrik Krcelic, Stein Haaland, Lukas Maes, Rikard Slapak, and Audrey Schillings
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Ferdinand Plaschke, Maria Jernej, Heli Hietala, and Laura Vuorinen
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Martin Volwerk, Charlotte Goetz, Ferdinand Plaschke, Tomas Karlsson, Daniel Heyner, and Brian Anderson
Ann. Geophys., 38, 51–60, https://doi.org/10.5194/angeo-38-51-2020, https://doi.org/10.5194/angeo-38-51-2020, 2020
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The magnetic field that is carried by the solar wind slowly decreases in strength as it moves further from the Sun. However, there are sometimes localized decreases in the magnetic field strength, called magnetic holes. These are small structures where the magnetic field strength decreases to less than 50 % of the surroundings and the plasma density increases. This paper presents a statistical study of the behaviour of these holes between Mercury and Venus using MESSENGER data.
Ferdinand Plaschke
Geosci. Instrum. Method. Data Syst., 8, 285–291, https://doi.org/10.5194/gi-8-285-2019, https://doi.org/10.5194/gi-8-285-2019, 2019
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Measuring the magnetic field onboard spacecraft requires regular in-flight calibration activities. Among those, determining the output of magnetometers under vanishing ambient magnetic fields, the so-called magnetometer offsets, is essential. Typically, characteristic rotations in solar wind magnetic fields are used to obtain these offsets. This paper addresses the question of how many solar wind data are needed to reach certain accuracy levels in offset determination.
Laura Vuorinen, Heli Hietala, and Ferdinand Plaschke
Ann. Geophys., 37, 689–697, https://doi.org/10.5194/angeo-37-689-2019, https://doi.org/10.5194/angeo-37-689-2019, 2019
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Before the solar wind encounters the Earth's magnetic field, it is first slowed down and deflected by the Earth's bow shock. We find that downstream of the bow shock regions where the shock normal and the solar wind magnetic field are almost parallel and the shock is more rippled, plasma jets with high earthward velocities are observed significantly more often than elsewhere downstream of the shock. Our results help us forecast the occurrence of these jets and their effects on Earth.
Ferdinand Plaschke, Hans-Ulrich Auster, David Fischer, Karl-Heinz Fornaçon, Werner Magnes, Ingo Richter, Dragos Constantinescu, and Yasuhito Narita
Geosci. Instrum. Method. Data Syst., 8, 63–76, https://doi.org/10.5194/gi-8-63-2019, https://doi.org/10.5194/gi-8-63-2019, 2019
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Raw output of spacecraft magnetometers has to be converted into meaningful units and coordinate systems before it is usable for scientific applications. This conversion is defined by 12 calibration parameters, 8 of which are more easily determined in flight if the spacecraft is spinning. We present theory and advanced algorithms to determine these eight parameters. They take into account the physical magnetometer and spacecraft behavior, making them superior to previously published algorithms.
Nikolai Østgaard, Jone P. Reistad, Paul Tenfjord, Karl M. Laundal, Theresa Rexer, Stein E. Haaland, Kristian Snekvik, Michael Hesse, Stephen E. Milan, and Anders Ohma
Ann. Geophys., 36, 1577–1596, https://doi.org/10.5194/angeo-36-1577-2018, https://doi.org/10.5194/angeo-36-1577-2018, 2018
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Minna Palmroth, Heli Hietala, Ferdinand Plaschke, Martin Archer, Tomas Karlsson, Xóchitl Blanco-Cano, David Sibeck, Primož Kajdič, Urs Ganse, Yann Pfau-Kempf, Markus Battarbee, and Lucile Turc
Ann. Geophys., 36, 1171–1182, https://doi.org/10.5194/angeo-36-1171-2018, https://doi.org/10.5194/angeo-36-1171-2018, 2018
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Magnetosheath jets are high-velocity plasma structures that are commonly observed within the Earth's magnetosheath. Previously, they have mainly been investigated with spacecraft observations, which do not allow us to infer their spatial sizes, temporal evolution, or origin. This paper shows for the first time their dimensions, evolution, and origins within a simulation whose dimensions are directly comparable to the Earth's magnetosphere. The results are compared to previous observations.
Yaireska M. Collado-Vega, Virginia L. Kalb, David G. Sibeck, Kyoung-Joo Hwang, and Lutz Rastätter
Ann. Geophys., 36, 1117–1129, https://doi.org/10.5194/angeo-36-1117-2018, https://doi.org/10.5194/angeo-36-1117-2018, 2018
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This paper describes an algorithm that automatically detects vortices around the Earth's magnetosphere using the velocity field from simulated data. It also describes how the tool can be used to analyze further properties of the vortices including the velocity changes within their motion across the magnetosheath. Vortices developed at the magnetopause boundary contribute to the process of mass, momentum and energy transfer from the solar wind into the Earth's magnetosphere.
Xochitl Blanco-Cano, Markus Battarbee, Lucile Turc, Andrew P. Dimmock, Emilia K. J. Kilpua, Sanni Hoilijoki, Urs Ganse, David G. Sibeck, Paul A. Cassak, Robert C. Fear, Riku Jarvinen, Liisa Juusola, Yann Pfau-Kempf, Rami Vainio, and Minna Palmroth
Ann. Geophys., 36, 1081–1097, https://doi.org/10.5194/angeo-36-1081-2018, https://doi.org/10.5194/angeo-36-1081-2018, 2018
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We use the Vlasiator code to study the characteristics of transient structures that exist in the Earth's foreshock, i.e. upstream of the bow shock. The structures are cavitons and spontaneous hot flow anomalies (SHFAs). These transients can interact with the bow shock. We study the changes the shock suffers via this interaction. We also investigate ion distributions associated with the cavitons and SHFAs. A very important result is that the arrival of multiple SHFAs results in shock erosion.
Ferdinand Plaschke and Heli Hietala
Ann. Geophys., 36, 695–703, https://doi.org/10.5194/angeo-36-695-2018, https://doi.org/10.5194/angeo-36-695-2018, 2018
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Fast jets of solar wind particles drive through a slower environment in the magnetosheath, located sunward of the region dominated by the Earth’s magnetic field. THEMIS multi-spacecraft observations show that jets push ambient particles out of their way. These particles flow around the faster jets into the jets’ wake. Thereby, jets stir the magnetosheath, changing the properties of this key region whose particles and magnetic fields can directly interact with the Earth’s magnetic field.
Tomas Karlsson, Ferdinand Plaschke, Heli Hietala, Martin Archer, Xóchitl Blanco-Cano, Primož Kajdič, Per-Arne Lindqvist, Göran Marklund, and Daniel J. Gershman
Ann. Geophys., 36, 655–677, https://doi.org/10.5194/angeo-36-655-2018, https://doi.org/10.5194/angeo-36-655-2018, 2018
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We have studied fast plasma jets outside of Earth’s magnetic environment. Such jets are small-scale structures with a limited lifetime, which may be important in determining the properties of the near-Earth space environment, due to their concentrated kinetic energy. We have used data from the NASA Magnetospheric MultiScale (MMS) satellites to study their properties in detail, to understand how these jets are formed. We have found evidence that there are at least two different types of jets.
Sudong Xiao, Tielong Zhang, Guoqiang Wang, Martin Volwerk, Yasong Ge, Daniel Schmid, Rumi Nakamura, Wolfgang Baumjohann, and Ferdinand Plaschke
Ann. Geophys., 35, 1015–1022, https://doi.org/10.5194/angeo-35-1015-2017, https://doi.org/10.5194/angeo-35-1015-2017, 2017
Christina Chu, Hui Zhang, David Sibeck, Antonius Otto, QiuGang Zong, Nick Omidi, James P. McFadden, Dennis Fruehauff, and Vassilis Angelopoulos
Ann. Geophys., 35, 443–451, https://doi.org/10.5194/angeo-35-443-2017, https://doi.org/10.5194/angeo-35-443-2017, 2017
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Hot flow anomalies (HFAs) at Earth's bow shock were identified in Time History of Events and Macroscale Interactions During Substorms (THEMIS) satellite data from 2007 to 2009. The events were classified as young or mature and regular or spontaneous hot flow anomalies (SHFAs). HFA–SHFA occurrence decreases with distance upstream from the bow shock. HFAs are more prevalent for radial interplanetary magnetic fields and solar wind speeds from 550 to 600 kms−1.
Dennis Frühauff, Ferdinand Plaschke, and Karl-Heinz Glassmeier
Ann. Geophys., 35, 117–121, https://doi.org/10.5194/angeo-35-117-2017, https://doi.org/10.5194/angeo-35-117-2017, 2017
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Vector magnetic field instruments mounted on spacecraft require precise in-flight calibration of the offsets of all three axes, i.e., the output in vanishing ambient field. While calibration of the spin plane offsets is trivial, we apply a new technique for determining the spin axis offset, not relying on solar wind data but on magnetosheath encounters. This technique is successfully applied to the satellites of the THEMIS mission to update the calibration parameters of the complete mission.
Martin Volwerk, Daniel Schmid, Bruce T. Tsurutani, Magda Delva, Ferdinand Plaschke, Yasuhito Narita, Tielong Zhang, and Karl-Heinz Glassmeier
Ann. Geophys., 34, 1099–1108, https://doi.org/10.5194/angeo-34-1099-2016, https://doi.org/10.5194/angeo-34-1099-2016, 2016
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The behaviour of mirror mode waves in Venus's magnetosheath is investigated for solar minimum and maximum conditions. It is shown that the total observational rate of these waves does not change much; however, the distribution over the magnetosheath is significantly different, as well as the growth and decay of the waves during these different solar activity conditions.
David Fischer, Werner Magnes, Christian Hagen, Ivan Dors, Mark W. Chutter, Jerry Needell, Roy B. Torbert, Olivier Le Contel, Robert J. Strangeway, Gernot Kubin, Aris Valavanoglou, Ferdinand Plaschke, Rumi Nakamura, Laurent Mirioni, Christopher T. Russell, Hannes K. Leinweber, Kenneth R. Bromund, Guan Le, Lawrence Kepko, Brian J. Anderson, James A. Slavin, and Wolfgang Baumjohann
Geosci. Instrum. Method. Data Syst., 5, 521–530, https://doi.org/10.5194/gi-5-521-2016, https://doi.org/10.5194/gi-5-521-2016, 2016
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This paper describes frequency and timing calibration, modeling and data processing and calibration for MMS magnetometers, resulting in a merged search choil and fluxgate data product.
Galina Korotova, David Sibeck, Mark Engebretson, John Wygant, Scott Thaller, Harlan Spence, Craig Kletzing, Vassilis Angelopoulos, and Robert Redmon
Ann. Geophys., 34, 985–998, https://doi.org/10.5194/angeo-34-985-2016, https://doi.org/10.5194/angeo-34-985-2016, 2016
Lukas Maes, Romain Maggiolo, and Johan De Keyser
Ann. Geophys., 34, 961–974, https://doi.org/10.5194/angeo-34-961-2016, https://doi.org/10.5194/angeo-34-961-2016, 2016
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Ion outflow from the ionospheric regions at the highest latitudes is mainly driven by solar illumination. It is an important factor affecting atmospheric escape and space weather. But this region rotates into and out of the sunlight on a daily and seasonal basis. This creates daily and seasonal variations in the outflow, even with both hemispheres combined. The north–south asymmetry in Earth's magnetic field causes extra variations and asymmetries. This was studied with a simple empirical model.
Ferdinand Plaschke and Yasuhito Narita
Ann. Geophys., 34, 759–766, https://doi.org/10.5194/angeo-34-759-2016, https://doi.org/10.5194/angeo-34-759-2016, 2016
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Spacecraft-mounted magnetic field instruments (magnetometers) need to be routinely calibrated. This involves determining the magnetometer outputs in vanishing ambient magnetic fields, the so-called offsets. We introduce and test a new method to determine these offsets with high accuracy, the mirror mode method, which is complementary to existing methods. The mirror mode method should be highly beneficial to current and future magnetic field observations near Earth, other planets, and comets.
Egor V. Yushkov, Anton V. Artemyev, Anatoly A. Petrukovich, and Rumi Nakamura
Ann. Geophys., 34, 739–750, https://doi.org/10.5194/angeo-34-739-2016, https://doi.org/10.5194/angeo-34-739-2016, 2016
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In the paper we study flapping wave structures, generated in the neutral plane of the Earth magnetotail. Investigated flapping is an important process of magnetosphere dynamics, connected with magnetic energy transformation and magnetic storm formation. Large separation of Cluster spacecraft allows us to estimate both local and global properties of flapping current sheets, the typical flapping times and propagation directions.
Takuma Nakamura, Rumi Nakamura, and Hiroshi Haseagwa
Ann. Geophys., 34, 357–367, https://doi.org/10.5194/angeo-34-357-2016, https://doi.org/10.5194/angeo-34-357-2016, 2016
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Magnetic reconnection is a key process in space and laboratory plasmas which transfers energies through the magnetic field topology change. The topology change in this process takes place in a small scale region called the electron diffusion region (EDR). In this paper, using high-resolution fully kinetic simulations, we successfully obtained the firm scaling laws of spatial dimensions of the EDR. The obtained scalings allow us to precisely predict observable dimensions of the EDR in real space.
Sudong Xiao, Tielong Zhang, Yasong Ge, Guoqiang Wang, Wolfgang Baumjohann, and Rumi Nakamura
Ann. Geophys., 34, 303–311, https://doi.org/10.5194/angeo-34-303-2016, https://doi.org/10.5194/angeo-34-303-2016, 2016
Y. Narita, R. Nakamura, W. Baumjohann, K.-H. Glassmeier, U. Motschmann, and H. Comişel
Ann. Geophys., 34, 85–89, https://doi.org/10.5194/angeo-34-85-2016, https://doi.org/10.5194/angeo-34-85-2016, 2016
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Four-spacecraft Cluster observations of turbulent fluctuations in the magnetic reconnection region in the geomagnetic tail show for the first time an indication of ion Bernstein waves, electromagnetic waves that propagate nearly perpendicular to the mean magnetic field and are in resonance with ions. Bernstein waves may influence current sheet dynamics in the reconnection outflow such as a bifurcation of the current sheet.
P. M. E. Décréau, S. Aoutou, A. Denazelle, I. Galkina, J.-L. Rauch, X. Vallières, P. Canu, S. Rochel Grimald, F. El-Lemdani Mazouz, and F. Darrouzet
Ann. Geophys., 33, 1285–1300, https://doi.org/10.5194/angeo-33-1285-2015, https://doi.org/10.5194/angeo-33-1285-2015, 2015
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We present here cases of wide banded Non Thermal Continuum (NTC) observed from the multi-point Cluster observatory. We point out that a large portion of the plasmasphere boundary layer, covering magnetic latitudes from 0 to above 30°, is radiating these radio waves. The radiation is confined inside multiple beams of small cone angles. We show how the spectral signature evolves, from integer harmonics of the electron gyrofrequency, when the observatory moves away from their sources.
G. Verbanac, V. Pierrard, M. Bandić, F. Darrouzet, J.-L. Rauch, and P. Décréau
Ann. Geophys., 33, 1271–1283, https://doi.org/10.5194/angeo-33-1271-2015, https://doi.org/10.5194/angeo-33-1271-2015, 2015
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Using Cluster data, we develop plasmapause Lpp models parameterized by solar wind coupling functions and geomagnetic activity indices. We show that the Lpp response to the changes in the interplanetary conditions depends on the magnetic local time. The faster plasmapause response is observed in the post-midnight sector. At low activity, Lpp exhibits the largest values on the dayside. For enhanced activity, displacements towards larger values on the evening side are identified.
G. I. Korotova, D. G. Sibeck, K. Tahakashi, L. Dai, H. E. Spence, C. A. Kletzing, J. R. Wygant, J. W. Manweiler, P. S. Moya, K.-J. Hwang, and R. J. Redmon
Ann. Geophys., 33, 955–964, https://doi.org/10.5194/angeo-33-955-2015, https://doi.org/10.5194/angeo-33-955-2015, 2015
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We studied localized Pc 4 pulsations in the pre-midnight inner magnetosphere observed by Van Allen Probe B on May 1 2013. Although we attribute the pulsations to a drift-bounce resonance, we demonstrate that the energy-dependent response of the ion fluxes result from pulsation-associated velocities sweeping energy-dependent radial ion flux gradients back and forth past the spacecraft.
M. O. Archer, T. S. Horbury, P. Brown, J. P. Eastwood, T. M. Oddy, B. J. Whiteside, and J. G. Sample
Ann. Geophys., 33, 725–735, https://doi.org/10.5194/angeo-33-725-2015, https://doi.org/10.5194/angeo-33-725-2015, 2015
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The first in-flight results from a new design of miniaturised magnetometer (MAGIC - MAGnetometer from Imperial College), aboard the first CINEMA (Cubesat for Ions, Neutrals, Electrons and MAgnetic fields) spacecraft in low Earth orbit, are presented. Not only can this sensor be used for determining attitude, but it is also able to detect the extremely small (20-40 nT) magnetic field signatures of field-aligned currents at the auroral oval. Thus, there are science capabilities with such sensors.
P. Robert, N. Cornilleau-Wehrlin, R. Piberne, Y. de Conchy, C. Lacombe, V. Bouzid, B. Grison, D. Alison, and P. Canu
Geosci. Instrum. Method. Data Syst., 3, 153–177, https://doi.org/10.5194/gi-3-153-2014, https://doi.org/10.5194/gi-3-153-2014, 2014
H. Gunell, G. Stenberg Wieser, M. Mella, R. Maggiolo, H. Nilsson, F. Darrouzet, M. Hamrin, T. Karlsson, N. Brenning, J. De Keyser, M. André, and I. Dandouras
Ann. Geophys., 32, 991–1009, https://doi.org/10.5194/angeo-32-991-2014, https://doi.org/10.5194/angeo-32-991-2014, 2014
A. P. Walsh, S. Haaland, C. Forsyth, A. M. Keesee, J. Kissinger, K. Li, A. Runov, J. Soucek, B. M. Walsh, S. Wing, and M. G. G. T. Taylor
Ann. Geophys., 32, 705–737, https://doi.org/10.5194/angeo-32-705-2014, https://doi.org/10.5194/angeo-32-705-2014, 2014
D. Schmid, M. Volwerk, F. Plaschke, Z. Vörös, T. L. Zhang, W. Baumjohann, and Y. Narita
Ann. Geophys., 32, 651–657, https://doi.org/10.5194/angeo-32-651-2014, https://doi.org/10.5194/angeo-32-651-2014, 2014
R. Wang, R. Nakamura, T. Zhang, A. Du, W. Baumjohann, Q. Lu, and A. N. Fazakerley
Ann. Geophys., 32, 239–248, https://doi.org/10.5194/angeo-32-239-2014, https://doi.org/10.5194/angeo-32-239-2014, 2014
I. Y. Vasko, A. V. Artemyev, A. A. Petrukovich, R. Nakamura, and L. M. Zelenyi
Ann. Geophys., 32, 133–146, https://doi.org/10.5194/angeo-32-133-2014, https://doi.org/10.5194/angeo-32-133-2014, 2014
R. Nakamura, F. Plaschke, R. Teubenbacher, L. Giner, W. Baumjohann, W. Magnes, M. Steller, R. B. Torbert, H. Vaith, M. Chutter, K.-H. Fornaçon, K.-H. Glassmeier, and C. Carr
Geosci. Instrum. Method. Data Syst., 3, 1–11, https://doi.org/10.5194/gi-3-1-2014, https://doi.org/10.5194/gi-3-1-2014, 2014
P. M. E. Décréau, S. Kougblénou, G. Lointier, J.-L. Rauch, J.-G. Trotignon, X. Vallières, P. Canu, S. Rochel Grimald, F. El-Lemdani Mazouz, and F. Darrouzet
Ann. Geophys., 31, 2097–2121, https://doi.org/10.5194/angeo-31-2097-2013, https://doi.org/10.5194/angeo-31-2097-2013, 2013
F. Plaschke, H. Hietala, and V. Angelopoulos
Ann. Geophys., 31, 1877–1889, https://doi.org/10.5194/angeo-31-1877-2013, https://doi.org/10.5194/angeo-31-1877-2013, 2013
F. R. Cardoso, W. D. Gonzalez, D. G. Sibeck, M. Kuznetsova, and D. Koga
Ann. Geophys., 31, 1853–1866, https://doi.org/10.5194/angeo-31-1853-2013, https://doi.org/10.5194/angeo-31-1853-2013, 2013
Y. Narita, R. Nakamura, and W. Baumjohann
Ann. Geophys., 31, 1605–1610, https://doi.org/10.5194/angeo-31-1605-2013, https://doi.org/10.5194/angeo-31-1605-2013, 2013
Y. M. Collado-Vega, R. L. Kessel, D. G. Sibeck, V. L. Kalb, R. A. Boller, and L. Rastaetter
Ann. Geophys., 31, 1463–1483, https://doi.org/10.5194/angeo-31-1463-2013, https://doi.org/10.5194/angeo-31-1463-2013, 2013
A. V. Artemyev, A. A. Petrukovich, R. Nakamura, and L. M. Zelenyi
Ann. Geophys., 31, 1109–1114, https://doi.org/10.5194/angeo-31-1109-2013, https://doi.org/10.5194/angeo-31-1109-2013, 2013
G. Paschmann, S. Haaland, B. Sonnerup, and T. Knetter
Ann. Geophys., 31, 871–887, https://doi.org/10.5194/angeo-31-871-2013, https://doi.org/10.5194/angeo-31-871-2013, 2013
M. Volwerk, N. André, C. S. Arridge, C. M. Jackman, X. Jia, S. E. Milan, A. Radioti, M. F. Vogt, A. P. Walsh, R. Nakamura, A. Masters, and C. Forsyth
Ann. Geophys., 31, 817–833, https://doi.org/10.5194/angeo-31-817-2013, https://doi.org/10.5194/angeo-31-817-2013, 2013
C. P. Escoubet, J. Berchem, K. J. Trattner, F. Pitout, R. Richard, M. G. G. T. Taylor, J. Soucek, B. Grison, H. Laakso, A. Masson, M. Dunlop, I. Dandouras, H. Reme, A. Fazakerley, and P. Daly
Ann. Geophys., 31, 713–723, https://doi.org/10.5194/angeo-31-713-2013, https://doi.org/10.5194/angeo-31-713-2013, 2013
C. Nabert, K.-H. Glassmeier, and F. Plaschke
Ann. Geophys., 31, 419–437, https://doi.org/10.5194/angeo-31-419-2013, https://doi.org/10.5194/angeo-31-419-2013, 2013
M. O. Archer and T. S. Horbury
Ann. Geophys., 31, 319–331, https://doi.org/10.5194/angeo-31-319-2013, https://doi.org/10.5194/angeo-31-319-2013, 2013
A. Alexandrova, R. Nakamura, V. S. Semenov, I. V. Kubyshkin, S. Apatenkov, E. V. Panov, D. Korovinskiy, H. Biernat, W. Baumjohann, K.-H. Glassmeier, and J. P. McFadden
Ann. Geophys., 30, 1727–1741, https://doi.org/10.5194/angeo-30-1727-2012, https://doi.org/10.5194/angeo-30-1727-2012, 2012
Related subject area
Subject: Magnetosphere & space plasma physics | Keywords: Solar wind–magnetosphere interactions
Velocity of magnetic holes in the solar wind from Cluster multipoint measurements
Storm time polar cap expansion: interplanetary magnetic field clock angle dependence
Solar wind magnetic holes can cross the bow shock and enter the magnetosheath
Comment on
From the Sun to Earth: effects of the 25 August 2018 geomagnetic storm
GUMICS-4 analysis of interplanetary coronal mass ejection impact on Earth during low and typical Mach number solar winds
Local time extent of magnetopause reconnection using space–ground coordination
The asymmetric geospace as displayed during the geomagnetic storm on 17 August 2001
Transfer entropy and cumulant-based cost as measures of nonlinear causal relationships in space plasmas: applications to Dst
Henriette Trollvik, Tomas Karlsson, and Savvas Raptis
Ann. Geophys., 41, 327–337, https://doi.org/10.5194/angeo-41-327-2023, https://doi.org/10.5194/angeo-41-327-2023, 2023
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The solar wind is in a plasma state and can exhibit a range of phenomena like waves and instabilities. One observed phenomenon in the solar wind is magnetic holes (MHs). They are localized depressions in the magnetic field. We studied the motion of MHs using the multispacecraft ESA Cluster mission. We derived their velocities in the solar wind frame and found that both linear and rotational MHs are convected with the solar wind.
Beket Tulegenov, Joachim Raeder, William D. Cramer, Banafsheh Ferdousi, Timothy J. Fuller-Rowell, Naomi Maruyama, and Robert J. Strangeway
Ann. Geophys., 41, 39–54, https://doi.org/10.5194/angeo-41-39-2023, https://doi.org/10.5194/angeo-41-39-2023, 2023
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We study how the polar regions of the Earth connect to space along magnetic field lines. While the Earth's magnetic field is mostly the shape of a dipole, at high latitudes the field lines tend to be open and connect to interplanetary space. This area of open field line is called the polar cap, and it is highly dynamic. Through data analysis and computer simulations, we find that the shape of the polar cap is closely controlled by the magnetic field embedded in the solar wind.
Tomas Karlsson, Henriette Trollvik, Savvas Raptis, Hans Nilsson, and Hadi Madanian
Ann. Geophys., 40, 687–699, https://doi.org/10.5194/angeo-40-687-2022, https://doi.org/10.5194/angeo-40-687-2022, 2022
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Magnetic holes are curious localized dropouts of magnetic field strength in the solar wind (the flow of ionized gas continuously streaming out from the sun). In this paper we show that these magnetic holes can cross the bow shock (where the solar wind brake down to subsonic velocity) and enter the region close to Earth’s magnetosphere. These structures may therefore represent a new type of non-uniform solar wind–magnetosphere interaction.
Invariability of relationship between the polar cap magnetic activity and geoeffective interplanetary electric fieldby Troshichev et al. (2011)
Peter Stauning
Ann. Geophys. Discuss., https://doi.org/10.5194/angeo-2020-52, https://doi.org/10.5194/angeo-2020-52, 2020
Preprint withdrawn
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In Troshichev et al. (2006) an error was made in the calculations of Polar Cap (PC) index scaling parameters. For the publication commented here, Troshichev et al. (2011), the authors state having used scaling parameters of the invalid PC index version but have actually substituted parameters from another version instead. The mingling of PC index versions has resulted in erroneous illustrations in Figs. 1, 2, 3, 6, 7, and 8 and the issuing of non-substantiated statements.
Mirko Piersanti, Paola De Michelis, Dario Del Moro, Roberta Tozzi, Michael Pezzopane, Giuseppe Consolini, Maria Federica Marcucci, Monica Laurenza, Simone Di Matteo, Alessio Pignalberi, Virgilio Quattrociocchi, and Piero Diego
Ann. Geophys., 38, 703–724, https://doi.org/10.5194/angeo-38-703-2020, https://doi.org/10.5194/angeo-38-703-2020, 2020
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This paper presents a comprehensive analysis of the solar event that occurred on 25 August 2018. This kind of comprehensive analysis plays a key role in better understanding the complexity of the processes occurring in the Sun–Earth system determining the geoeffectiveness of manifestations of solar activity. The analysis presented here shows for the first time a direct link between characteristics of solar perturbation, the magnetosphere–ionosphere system response and space weather effects.
Antti Lakka, Tuija I. Pulkkinen, Andrew P. Dimmock, Emilia Kilpua, Matti Ala-Lahti, Ilja Honkonen, Minna Palmroth, and Osku Raukunen
Ann. Geophys., 37, 561–579, https://doi.org/10.5194/angeo-37-561-2019, https://doi.org/10.5194/angeo-37-561-2019, 2019
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We study how the Earth's space environment responds to two different amplitude interplanetary coronal mass ejection (ICME) events that occurred in 2012 and 2014 by using the GUMICS-4 global MHD model. We examine local and large-scale dynamics of the Earth's space environment and compare simulation results to in situ data. It is shown that during moderate driving simulation agrees well with the measurements; however, GMHD results should be interpreted cautiously during strong driving.
Ying Zou, Brian M. Walsh, Yukitoshi Nishimura, Vassilis Angelopoulos, J. Michael Ruohoniemi, Kathryn A. McWilliams, and Nozomu Nishitani
Ann. Geophys., 37, 215–234, https://doi.org/10.5194/angeo-37-215-2019, https://doi.org/10.5194/angeo-37-215-2019, 2019
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Magnetopause reconnection is a process whereby the Sun explosively transfers energy to the Earth. Whether the process is spatially patchy or spatially continuous and extended has been under long debate. We use space–ground coordination to overcome the limitations of previous studies and reliably interpret spatial extent. Our result strongly indicates that both patchy and extended reconnection is possible and, interestingly, that extended reconnection grows from a localized patch via spreading.
Nikolai Østgaard, Jone P. Reistad, Paul Tenfjord, Karl M. Laundal, Theresa Rexer, Stein E. Haaland, Kristian Snekvik, Michael Hesse, Stephen E. Milan, and Anders Ohma
Ann. Geophys., 36, 1577–1596, https://doi.org/10.5194/angeo-36-1577-2018, https://doi.org/10.5194/angeo-36-1577-2018, 2018
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In this paper we take advantage of having two auroral imaging missions giving simultaneous data of both the southern and northern aurora. Combined with all available in situ measurements from space and global ground-based networks, we explore the asymmetric behavior of geospace. We find large auroral asymmetries and different reconnection geometry in the two hemispheres. During substorm expansion phase asymmetries are reduced.
Jay R. Johnson, Simon Wing, and Enrico Camporeale
Ann. Geophys., 36, 945–952, https://doi.org/10.5194/angeo-36-945-2018, https://doi.org/10.5194/angeo-36-945-2018, 2018
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The magnetospheric response to the solar wind is nonlinear. Information theoretical tools are able to characterize the nonlinearities in the system. We show that nonlinear significance of Dst peaks at lags of 3–12 hours which can be attributed to VBs, which also exhibits similar behavior. However, the nonlinear significance that peaks at lags of 25, 50, and 90 hours can be attributed to internal dynamics, which may be related to the relaxation of the ring current.
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Short summary
In our study, we looked at the boundary between the Earth's magnetic field and the interplanetary magnetic field emitted by the Sun, called the magnetopause. While other studies focus on the magnetopause motion near Earth's Equator, we have studied it in polar regions. The motion of the magnetopause is faster towards the Earth than towards the Sun. We also found that the occurrence of unusual magnetopause locations is due to similar solar influences in the equatorial and polar regions.
In our study, we looked at the boundary between the Earth's magnetic field and the...
