Articles | Volume 31, issue 5
https://doi.org/10.5194/angeo-31-817-2013
© Author(s) 2013. This work is distributed under
the Creative Commons Attribution 3.0 License.
the Creative Commons Attribution 3.0 License.
https://doi.org/10.5194/angeo-31-817-2013
© Author(s) 2013. This work is distributed under
the Creative Commons Attribution 3.0 License.
the Creative Commons Attribution 3.0 License.
Regular paper
| 
06 May 2013
Regular paper |
| 06 May 2013
Comparative magnetotail flapping: an overview of selected events at Earth, Jupiter and Saturn
M. Volwerk
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
N. André
Centre d'Etude Spatiale des Rayonnements, Université de Toulouse, UPS, Toulouse, France
CNRS, UMR 5187, Toulouse, France
C. S. Arridge
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, UK
Centre for Planetary Sciences at UCL/Birkbeck, London, WC1E 6BT, UK
C. M. Jackman
Centre for Planetary Sciences at UCL/Birkbeck, London, WC1E 6BT, UK
Department of Physics and Astronomy, University College London, Gower Place, London, WC1E 6BT, UK
X. Jia
Dept. of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, USA
S. E. Milan
Department of Physics and Astronomy, University of Leicester, Leicester, UK
A. Radioti
Laboratoire de Physique Atmosphérique et Planétaire, Institut d'Astrophysique et de Géophysique, Université de Liège, Liège, Belgium
M. F. Vogt
Department of Physics and Astronomy, University of Leicester, Leicester, UK
A. P. Walsh
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, UK
now at: Science and Robotic Exploration Directorate, ESA/ESTEC, Noordwijk, the Netherlands
R. Nakamura
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
A. Masters
Institute of Space and Astronautical Science, JAXA, Sagamihara, Japan
C. Forsyth
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, UK
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This article is included in the Encyclopedia of Geosciences
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This article is included in the Encyclopedia of Geosciences
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Recently, the two-spacecraft mission BepiColombo was launched to explore Mercury. To measure the magnetic field precisely, in-flight calibration of the magnetometer offset is needed. Usually, the offset is evaluated from magnetic field observations in the solar wind. Since one of the spacecraft will remain within Mercury's magnetic environment, we examine an alternative calibration method. We show that this method is applicable and may be a valuable tool to determine the offset accurately.
This article is included in the Encyclopedia of Geosciences
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This article is included in the Encyclopedia of Geosciences
I. Richter, C. Koenders, H.-U. Auster, D. Frühauff, C. Götz, P. Heinisch, C. Perschke, U. Motschmann, B. Stoll, K. Altwegg, J. Burch, C. Carr, E. Cupido, A. Eriksson, P. Henri, R. Goldstein, J.-P. Lebreton, P. Mokashi, Z. Nemeth, H. Nilsson, M. Rubin, K. Szegö, B. T. Tsurutani, C. Vallat, M. Volwerk, and K.-H. Glassmeier
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We present a first report on magnetic field measurements made in the coma of comet 67P/C-G in its low-activity state. The plasma environment is dominated by quasi-coherent, large-amplitude, compressional magnetic field oscillations around 40mHz, differing from the observations at strongly active comets where waves at the cometary ion gyro-frequencies are the main feature. We propose a cross-field current instability associated with the newborn cometary ions as a possible source mechanism.
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This article is included in the Encyclopedia of Geosciences
Ariel Tello Fallau, Charlotte Goetz, Cyril Simon Wedlund, Martin Volwerk, and Anja Moeslinger
Ann. Geophys., 41, 569–587, https://doi.org/10.5194/angeo-41-569-2023, https://doi.org/10.5194/angeo-41-569-2023, 2023
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The plasma environment of comet 67P provides a unique laboratory to study plasma phenomena in the solar system. Previous studies have reported the existence of mirror modes at 67P but no further systematic investigation has so far been done. This study aims to learn more about these waves. We investigate the magnetic field measured by Rosetta and find 565 mirror mode signatures. The detected mirror modes are likely generated upstream of the observation and have been modified by the plasma.
This article is included in the Encyclopedia of Geosciences
Martin Volwerk, Cyril Simon Wedlund, David Mautner, Sebastián Rojas Mata, Gabriella Stenberg Wieser, Yoshifumi Futaana, Christian Mazelle, Diana Rojas-Castillo, César Bertucci, and Magda Delva
Ann. Geophys., 41, 389–408, https://doi.org/10.5194/angeo-41-389-2023, https://doi.org/10.5194/angeo-41-389-2023, 2023
Short summary
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Freshly created ions in solar wind start gyrating around the interplanetary magnetic field. When they cross the bow shock, they get an extra kick, and this increases the plasma pressure against the magnetic pressure. This leads to the creation of so-called mirror modes, regions where the magnetic field decreases in strength and the plasma density increases. These structures help in exploring how energy is transferred from the ions to the magnetic field and where around Venus this is happening.
This article is included in the Encyclopedia of Geosciences
Cyril Simon Wedlund, Martin Volwerk, Christian Mazelle, Sebastián Rojas Mata, Gabriella Stenberg Wieser, Yoshifumi Futaana, Jasper Halekas, Diana Rojas-Castillo, César Bertucci, and Jared Espley
Ann. Geophys., 41, 225–251, https://doi.org/10.5194/angeo-41-225-2023, https://doi.org/10.5194/angeo-41-225-2023, 2023
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Mirror modes are magnetic bottles found in the space plasma environment of planets contributing to the energy exchange with the solar wind. We use magnetic field measurements from the NASA Mars Atmosphere and Volatile EvolutioN mission to detect them around Mars and show how they evolve in time and space. The structures concentrate in two regions: one behind the bow shock and the other closer to the planet. They compete with other wave modes depending on the solar flux and heliocentric distance.
This article is included in the Encyclopedia of Geosciences
Weijie Sun, James A. Slavin, Rumi Nakamura, Daniel Heyner, Karlheinz J. Trattner, Johannes Z. D. Mieth, Jiutong Zhao, Qiu-Gang Zong, Sae Aizawa, Nicolas Andre, and Yoshifumi Saito
Ann. Geophys., 40, 217–229, https://doi.org/10.5194/angeo-40-217-2022, https://doi.org/10.5194/angeo-40-217-2022, 2022
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This paper presents observations of FTE-type flux ropes on the dayside during BepiColombo's Earth flyby. FTE-type flux ropes are a well-known feature of magnetic reconnection on the magnetopause, and they can be used to constrain the location of reconnection X-lines. Our study suggests that the magnetopause X-line passed BepiColombo from the north as it traversed the magnetopause. Moreover, our results also strongly support coalescence creating larger flux ropes by combining smaller ones.
This article is included in the Encyclopedia of Geosciences
Martin Volwerk, Beatriz Sánchez-Cano, Daniel Heyner, Sae Aizawa, Nicolas André, Ali Varsani, Johannes Mieth, Stefano Orsini, Wolfgang Baumjohann, David Fischer, Yoshifumi Futaana, Richard Harrison, Harald Jeszenszky, Iwai Kazumasa, Gunter Laky, Herbert Lichtenegger, Anna Milillo, Yoshizumi Miyoshi, Rumi Nakamura, Ferdinand Plaschke, Ingo Richter, Sebastián Rojas Mata, Yoshifumi Saito, Daniel Schmid, Daikou Shiota, and Cyril Simon Wedlund
Ann. Geophys., 39, 811–831, https://doi.org/10.5194/angeo-39-811-2021, https://doi.org/10.5194/angeo-39-811-2021, 2021
Short summary
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On 15 October 2020, BepiColombo used Venus as a gravity assist to change its orbit to reach Mercury in late 2021. During this passage of Venus, the spacecraft entered into Venus's magnetotail at a distance of 70 Venus radii from the planet. We have studied the magnetic field and plasma data and find that Venus's magnetotail is highly active. This is caused by strong activity in the solar wind, where just before the flyby a coronal mass ejection interacted with the magnetophere of Venus.
This article is included in the Encyclopedia of Geosciences
Daniel Schmid, Yasuhito Narita, Ferdinand Plaschke, Martin Volwerk, Rumi Nakamura, and Wolfgang Baumjohann
Ann. Geophys., 39, 563–570, https://doi.org/10.5194/angeo-39-563-2021, https://doi.org/10.5194/angeo-39-563-2021, 2021
Short summary
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In this work we present the first analytical magnetosheath plasma flow model for the space environment around Mercury. The proposed model is relatively simple to implement and provides the possibility to trace the flow lines inside the Hermean magnetosheath. It can help to determine the the local plasma conditions of a spacecraft in the magnetosheath exclusively on the basis of the upstream solar wind parameters.
This article is included in the Encyclopedia of Geosciences
Martin Volwerk, David Mautner, Cyril Simon Wedlund, Charlotte Goetz, Ferdinand Plaschke, Tomas Karlsson, Daniel Schmid, Diana Rojas-Castillo, Owen W. Roberts, and Ali Varsani
Ann. Geophys., 39, 239–253, https://doi.org/10.5194/angeo-39-239-2021, https://doi.org/10.5194/angeo-39-239-2021, 2021
Short summary
Short summary
The magnetic field in the solar wind is not constant but varies in direction and strength. One of these variations shows a strong local reduction of the magnetic field strength and is called a magnetic hole. These holes are usually an indication that there is, or has been, a temperature difference in the plasma of the solar wind, with the temperature along the magnetic field lower than perpendicular. The MMS spacecraft data have been used to study the characteristics of these holes near Earth.
This article is included in the Encyclopedia of Geosciences
Alexander Lukin, Anton Artemyev, Evgeny Panov, Rumi Nakamura, Anatoly Petrukovich, Robert Ergun, Barbara Giles, Yuri Khotyaintsev, Per Arne Lindqvist, Christopher Russell, and Robert Strangeway
Ann. Geophys. Discuss., https://doi.org/10.5194/angeo-2020-76, https://doi.org/10.5194/angeo-2020-76, 2020
Revised manuscript not accepted
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We have collected statistics of 81 fast plasma flow events in the magnetotail with clear MMS observations of kinetic Alfven waves (KAWs). We show that KAWs electric field magnitudes correlates with thermal/subthermal electron flux anisotropy: wider energy range of electron anisotropic population corresponds to higher KAWs’ electric field intensity. These results indicate on an important role of KAWs in production of thermal field-aligned electron population of the Earth’s magnetotail.
This article is included in the Encyclopedia of Geosciences
Daniel Schmid, Ferdinand Plaschke, Yasuhito Narita, Daniel Heyner, Johannes Z. D. Mieth, Brian J. Anderson, Martin Volwerk, Ayako Matsuoka, and Wolfgang Baumjohann
Ann. Geophys., 38, 823–832, https://doi.org/10.5194/angeo-38-823-2020, https://doi.org/10.5194/angeo-38-823-2020, 2020
Short summary
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Recently, the two-spacecraft mission BepiColombo was launched to explore Mercury. To measure the magnetic field precisely, in-flight calibration of the magnetometer offset is needed. Usually, the offset is evaluated from magnetic field observations in the solar wind. Since one of the spacecraft will remain within Mercury's magnetic environment, we examine an alternative calibration method. We show that this method is applicable and may be a valuable tool to determine the offset accurately.
This article is included in the Encyclopedia of Geosciences
Angeline G. Burrell, Gareth Chisham, Stephen E. Milan, Liam Kilcommons, Yun-Ju Chen, Evan G. Thomas, and Brian Anderson
Ann. Geophys., 38, 481–490, https://doi.org/10.5194/angeo-38-481-2020, https://doi.org/10.5194/angeo-38-481-2020, 2020
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The Earth's polar upper atmosphere changes along with the magnetic field, other parts of the atmosphere, and the Sun. When studying these changes, knowing the polar region that the data come from is vital, as different processes dominate the area where the aurora is and poleward of the aurora (the polar cap). The boundary between these areas is hard to find, so this study used a different boundary and figured out how they are related. Future studies can now find their polar region more easily.
This article is included in the Encyclopedia of Geosciences
Guoqiang Wang, Tielong Zhang, Mingyu Wu, Daniel Schmid, Yufei Hao, and Martin Volwerk
Ann. Geophys., 38, 309–318, https://doi.org/10.5194/angeo-38-309-2020, https://doi.org/10.5194/angeo-38-309-2020, 2020
Short summary
Short summary
Currents are believed to exist in mirror-mode structures and to be self-consistent with the magnetic field depression. Bipolar currents are found in two ion-scale magnetic dips. The bipolar current in a small-size magnetic dip is mainly contributed by electron velocities, which is mainly formed by the magnetic gradient–curvature drift. For another large-size magnetic dip, the bipolar current is mainly caused by an ion bipolar velocity, which can be explained by the ion drift motions.
This article is included in the Encyclopedia of Geosciences
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
Short summary
Short summary
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.
This article is included in the Encyclopedia of Geosciences
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.
This article is included in the Encyclopedia of Geosciences
Shuai Zhang, Anmin Tian, Quanqi Shi, Hanlin Li, Alexander W. Degeling, I. Jonathan Rae, Colin Forsyth, Mengmeng Wang, Xiaochen Shen, Weijie Sun, Shichen Bai, Ruilong Guo, Huizi Wang, Andrew Fazakerley, Suiyan Fu, and Zuyin Pu
Ann. Geophys., 36, 1335–1346, https://doi.org/10.5194/angeo-36-1335-2018, https://doi.org/10.5194/angeo-36-1335-2018, 2018
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The features of ULF waves are statistically studied on the magnetotail stretched magnetic field lines (8 RE < R < 32 RE) by using 8 years of THEMIS data. The occurrence rates of ULF waves are higher in the post-midnight region than pre-midnight region. The frequency decreases with increasing radial distance of 8–16 RE and could be explained by much more standing waves in this region than in the region of 16–32 RE. The wave frequency is higher after the substorm onset than before it.
This article is included in the Encyclopedia of Geosciences
Martin Volwerk
Ann. Geophys., 36, 831–839, https://doi.org/10.5194/angeo-36-831-2018, https://doi.org/10.5194/angeo-36-831-2018, 2018
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Using Voyager 1 observations of Jupiter's Io plasma torus, we have determined the location of maximum brightness depending on longitude and the location of Jupiter’s moon Io. We obtain a third viewing direction of the torus (after Voyager 2 and ground observations) and thus two locations, left and right of Jupiter, which are important for the correct modeling of this structure. We also find that a narrow ribbon-like structure only appears when the brightness of the torus exceeds a certain value.
This article is included in the Encyclopedia of Geosciences
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
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.
This article is included in the Encyclopedia of Geosciences
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.
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Yann Pfau-Kempf, Heli Hietala, Steve E. Milan, Liisa Juusola, Sanni Hoilijoki, Urs Ganse, Sebastian von Alfthan, and Minna Palmroth
Ann. Geophys., 34, 943–959, https://doi.org/10.5194/angeo-34-943-2016, https://doi.org/10.5194/angeo-34-943-2016, 2016
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We have simulated the interaction of the solar wind – the charged particles and magnetic fields emitted by the Sun into space – with the magnetic field of the Earth. The solar wind flows supersonically and creates a shock when it encounters the obstacle formed by the geomagnetic field. We have identified a new chain of events which causes phenomena in the downstream region to eventually cause perturbations at the shock and even upstream. This is confirmed by ground and satellite observations.
This article is included in the Encyclopedia of Geosciences
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.
This article is included in the Encyclopedia of Geosciences
Ingo Richter, Hans-Ulrich Auster, Gerhard Berghofer, Chris Carr, Emanuele Cupido, Karl-Heinz Fornaçon, Charlotte Goetz, Philip Heinisch, Christoph Koenders, Bernd Stoll, Bruce T. Tsurutani, Claire Vallat, Martin Volwerk, and Karl-Heinz Glassmeier
Ann. Geophys., 34, 609–622, https://doi.org/10.5194/angeo-34-609-2016, https://doi.org/10.5194/angeo-34-609-2016, 2016
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We have analysed the magnetic field measurements performed on the ROSETTA orbiter and the lander PHILAE during PHILAE's descent to comet 67P/Churyumov-Gerasimenko on 12 November 2014. We observed a new type of low-frequency wave with amplitudes of ~ 3 nT, frequencies of 20–50 mHz, wavelengths of ~ 300 km, and propagation velocities of ~ 6 km s−1. The waves are generated in a ~ 100 km region around the comet a show a highly correlated behaviour, which could only be determined by two-point observations.
This article is included in the Encyclopedia of Geosciences
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.
This article is included in the Encyclopedia of Geosciences
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.
This article is included in the Encyclopedia of Geosciences
M. Volwerk, I. Richter, B. Tsurutani, C. Götz, K. Altwegg, T. Broiles, J. Burch, C. Carr, E. Cupido, M. Delva, M. Dósa, N. J. T. Edberg, A. Eriksson, P. Henri, C. Koenders, J.-P. Lebreton, K. E. Mandt, H. Nilsson, A. Opitz, M. Rubin, K. Schwingenschuh, G. Stenberg Wieser, K. Szegö, C. Vallat, X. Vallieres, and K.-H. Glassmeier
Ann. Geophys., 34, 1–15, https://doi.org/10.5194/angeo-34-1-2016, https://doi.org/10.5194/angeo-34-1-2016, 2016
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The solar wind magnetic field drapes around the active nucleus of comet 67P/CG, creating a magnetosphere. The solar wind density increases and with that the pressure, which compresses the magnetosphere, increasing the magnetic field strength near Rosetta. The higher solar wind density also creates more ionization through collisions with the gas from the comet. The new ions are picked-up by the magnetic field and generate mirror-mode waves, creating low-field high-density "bottles" near 67P/CG.
This article is included in the Encyclopedia of Geosciences
Z. H. Yao, J. Liu, C. J. Owen, C. Forsyth, I. J. Rae, Z. Y. Pu, H. S. Fu, X.-Z. Zhou, Q. Q. Shi, A. M. Du, R. L. Guo, and X. N. Chu
Ann. Geophys., 33, 1301–1309, https://doi.org/10.5194/angeo-33-1301-2015, https://doi.org/10.5194/angeo-33-1301-2015, 2015
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We use THEMIS large data set of dipolarization front events to build a 2-D pressure distribution in XZ plane, and thus derive the current system around the dipolarization front. Our results show that a banana current loop is formed around the dipolarization front. This current is also suggested to be the reason for the magnetic dip observed ahead of the dipolarization front. In addition, the current density is too small to contribute a substorm current wedge.
This article is included in the Encyclopedia of Geosciences
B. Bonfond, J. Gustin, J.-C. Gérard, D. Grodent, A. Radioti, B. Palmaerts, S. V. Badman, K. K. Khurana, and C. Tao
Ann. Geophys., 33, 1203–1209, https://doi.org/10.5194/angeo-33-1203-2015, https://doi.org/10.5194/angeo-33-1203-2015, 2015
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Early models of the main auroral emission at Jupiter assumed axisymmetry, but significant local time variability is obvious on any image of the Jovian aurorae. Here we use Far-UV images from the Hubble Space Telescope to further characterise these variations on a statistical basis. We show that the dusk side sector is ~3 times brighter than the dawn side and we suggest that such an asymmetry could be the result of a partial ring current in the night side magnetosphere.
This article is included in the Encyclopedia of Geosciences
B. Bonfond, J. Gustin, J.-C. Gérard, D. Grodent, A. Radioti, B. Palmaerts, S. V. Badman, K. K. Khurana, and C. Tao
Ann. Geophys., 33, 1211–1219, https://doi.org/10.5194/angeo-33-1211-2015, https://doi.org/10.5194/angeo-33-1211-2015, 2015
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Early models of the main auroral emission at Jupiter assumed axisymmetry, but significant local time variability is obvious on any image of the Jovian aurorae. Here we use far-UV images from the Hubble Space Telescope to further characterize these variations on a statistical basis. We show that the dusk side sector is ~3 times brighter than the dawn side, and we suggest that such an asymmetry could be the result of a partial ring current in the nightside magnetosphere.
This article is included in the Encyclopedia of Geosciences
Z. Nemeth, K. Szego, L. Foldy, M. G. Kivelson, X. Jia, K. M. Ramer, S. W. H. Cowley, G. Provan, and M. Thomsen
Ann. Geophys., 33, 1195–1202, https://doi.org/10.5194/angeo-33-1195-2015, https://doi.org/10.5194/angeo-33-1195-2015, 2015
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The latitudinal structure of the nightside outer magnetosphere of Saturn was studied by using Cassini CAPS plasma measurements. It was found that the plasma density and the azimuthal velocity decrease simultaneously as the spacecraft moves away from the magnetic equator. The magnetosphere exhibits an “onion shell like” structure: the inner regions spin rapidly corotating with the planet, but moving outward and/or further away from the equatorial plane one can encounter slower and slower shells.
This article is included in the Encyclopedia of Geosciences
I. Richter, C. Koenders, H.-U. Auster, D. Frühauff, C. Götz, P. Heinisch, C. Perschke, U. Motschmann, B. Stoll, K. Altwegg, J. Burch, C. Carr, E. Cupido, A. Eriksson, P. Henri, R. Goldstein, J.-P. Lebreton, P. Mokashi, Z. Nemeth, H. Nilsson, M. Rubin, K. Szegö, B. T. Tsurutani, C. Vallat, M. Volwerk, and K.-H. Glassmeier
Ann. Geophys., 33, 1031–1036, https://doi.org/10.5194/angeo-33-1031-2015, https://doi.org/10.5194/angeo-33-1031-2015, 2015
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We present a first report on magnetic field measurements made in the coma of comet 67P/C-G in its low-activity state. The plasma environment is dominated by quasi-coherent, large-amplitude, compressional magnetic field oscillations around 40mHz, differing from the observations at strongly active comets where waves at the cometary ion gyro-frequencies are the main feature. We propose a cross-field current instability associated with the newborn cometary ions as a possible source mechanism.
This article is included in the Encyclopedia of Geosciences
M. Volwerk, K.-H. Glassmeier, M. Delva, D. Schmid, C. Koenders, I. Richter, and K. Szegö
Ann. Geophys., 32, 1441–1453, https://doi.org/10.5194/angeo-32-1441-2014, https://doi.org/10.5194/angeo-32-1441-2014, 2014
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We discuss three flybys (within an 8-day time span) of comet 1P/Halley by VEGA 1, 2 and Giotto. Looking at two different plasma phenomena: mirror mode waves and field line draping; we study the differences in SW--comet interaction between these three flybys. We find that on this time scale (comparable to Rosetta's orbits) there is a significant difference, both caused by changing outgassing rate of the comet and changes in the solar wind. We discuss implications for Rosetta RPC observations.
This article is included in the Encyclopedia of Geosciences
A. Varsani, C. J. Owen, A. N. Fazakerley, C. Forsyth, A. P. Walsh, M. André, I. Dandouras, and C. M. Carr
Ann. Geophys., 32, 1093–1117, https://doi.org/10.5194/angeo-32-1093-2014, https://doi.org/10.5194/angeo-32-1093-2014, 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
M. Volwerk, C. Koenders, M. Delva, I. Richter, K. Schwingenschuh, M. S. Bentley, and K.-H. Glassmeier
Ann. Geophys., 31, 2201–2206, https://doi.org/10.5194/angeo-31-2201-2013, https://doi.org/10.5194/angeo-31-2201-2013, 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
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
M. Volwerk, X. Jia, C. Paranicas, W. S. Kurth, M. G. Kivelson, and K. K. Khurana
Ann. Geophys., 31, 45–59, https://doi.org/10.5194/angeo-31-45-2013, https://doi.org/10.5194/angeo-31-45-2013, 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
