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470 results on '"Glassmeier, K.-H."'

1. Cometary plasma science: Open science questions for future space missions

Author

Goetz, C., Gunell, H., Volwerk, M., Beth, A., Eriksson, A., Galand, M., Henri, P., Nilsson, H., Wedlund, C. Simon, Alho, M., Andersson, L., Andre, N., De Keyser, J., Deca, J., Ge, Y., Glassmeier, K.-H., Hajra, R., Karlsson, T., Kasahara, S., Kolmasova, I., LLera, K., Madanian, H., Mann, I., Mazelle, C., Odelstad, E., Plaschke, F., Rubin, M., Sanchez-Cano, B., Snodgrass, C., and Vigren, E.

Published
2022
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4. BepiColombo - Mission Overview and Science Goals

Author

Benkhoff, J., Murakami, G., Baumjohann, W., Besse, S., Bunce, E., Casale, M., Cremosese, G., Glassmeier, K.-H., Hayakawa, H., Heyner, D., Hiesinger, H., Huovelin, J., Hussmann, H., Iafolla, V., Iess, L., Kasaba, Y., Kobayashi, M., Milillo, A., Mitrofanov, I. G., Montagnon, E., Novara, M., Orsini, S., Quemerais, E., Reininghaus, U., Saito, Y., Santoli, F., Stramaccioni, D., Sutherland, O., Thomas, N., Yoshikawa, I., and Zender, J.

Published
2021
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6. The BepiColombo Planetary Magnetometer MPO-MAG: What Can We Learn from the Hermean Magnetic Field?

Author

Heyner, D., Auster, H.-U., Fornaçon, K.-H., Carr, C., Richter, I., Mieth, J. Z. D., Kolhey, P., Exner, W., Motschmann, U., Baumjohann, W., Matsuoka, A., Magnes, W., Berghofer, G., Fischer, D., Plaschke, F., Nakamura, R., Narita, Y., Delva, M., Volwerk, M., Balogh, A., Dougherty, M., Horbury, T., Langlais, B., Mandea, M., Masters, A., Oliveira, J. S., Sánchez-Cano, B., Slavin, J. A., Vennerstrøm, S., Vogt, J., Wicht, J., and Glassmeier, K.-H.

Published
2021
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7. The BepiColombo–Mio Magnetometer en Route to Mercury

Author

Baumjohann, W., Matsuoka, A., Narita, Y., Magnes, W., Heyner, D., Glassmeier, K.-H., Nakamura, R., Fischer, D., Plaschke, F., Volwerk, M., Zhang, T. L., Auster, H.-U., Richter, I., Balogh, A., Carr, C. M., Dougherty, M., Horbury, T. S., Tsunakawa, H., Matsushima, M., Shinohara, M., Shibuya, H., Nakagawa, T., Hoshino, M., Tanaka, Y., Anderson, B. J., Russell, C. T., Motschmann, U., Takahashi, F., and Fujimoto, A.

Published
2020
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8. Investigating Mercury’s Environment with the Two-Spacecraft BepiColombo Mission

Author

Milillo, A., Fujimoto, M., Murakami, G., Benkhoff, J., Zender, J., Aizawa, S., Dósa, M., Griton, L., Heyner, D., Ho, G., Imber, S. M., Jia, X., Karlsson, T., Killen, R. M., Laurenza, M., Lindsay, S. T., McKenna-Lawlor, S., Mura, A., Raines, J. M., Rothery, D. A., André, N., Baumjohann, W., Berezhnoy, A., Bourdin, P. A., Bunce, E. J., Califano, F., Deca, J., de la Fuente, S., Dong, C., Grava, C., Fatemi, S., Henri, P., Ivanovski, S. L., Jackson, B. V., James, M., Kallio, E., Kasaba, Y., Kilpua, E., Kobayashi, M., Langlais, B., Leblanc, F., Lhotka, C., Mangano, V., Martindale, A., Massetti, S., Masters, A., Morooka, M., Narita, Y., Oliveira, J. S., Odstrcil, D., Orsini, S., Pelizzo, M. G., Plainaki, C., Plaschke, F., Sahraoui, F., Seki, K., Slavin, J. A., Vainio, R., Wurz, P., Barabash, S., Carr, C. M., Delcourt, D., Glassmeier, K.-H., Grande, M., Hirahara, M., Huovelin, J., Korablev, O., Kojima, H., Lichtenegger, H., Livi, S., Matsuoka, A., Moissl, R., Moncuquet, M., Muinonen, K., Quèmerais, E., Saito, Y., Yagitani, S., Yoshikawa, I., and Wahlund, J.-E.

Published
2020
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10. The nonmagnetic nucleus of comet 67P/Churyumov-Gerasimenko

Author

Auster, H.-U., Apathy, I., Berghofer, G., Fornacon, K.-H., Remizov, A., Carr, C., Güttler, C., Haerendel, G., Heinisch, P., Hercik, D., Hilchenbach, M., Kührt, E., Magnes, W., Motschmann, U., Richter, I., Russell, C. T., Przyklenk, A., Schwingenschuh, K., Sierks, H., and Glassmeier, K.-H.

Published
2015

13. The Cluster Virtual Observatory for ULF Waves.

Author

Constantinescu, O. D., Fornaçon, K. H., Motschmann, U., Glassmeier, K. H., Richter, I., and Plaschke, F.

Subjects
MAGNETIC field measurements, ONLINE databases, ELECTRON density, OBSERVATORIES, PLASMA waves, SOLAR wind, POYNTING theorem, SOLAR cycle
Abstract

Since its launch in 2000, the Cluster fleet visited a vast domain of the circum‐terrestrial environment, from the upstream solar wind and the distant tail, down to the plasmasphere, scanning in detail all magnetospheric regions during over two solar cycles. This led to an unprecedentedly rich data collection of multi‐point measurements which will be used for years to come to decipher the mechanisms of Solar‐Terrestrial interactions. The large volume of data gathered by Cluster requires special strategies to make efficient use of it. To address this issue we constructed a browsable database containing parameters of the detected Ultra low frequency waves and of the spacecraft formation geometry. The primary data used to derive the parameters are the magnetic field, the electric field and the electron density. The data is resampled to a cadence of 1 s and processed using a sliding analysis window of 2,048 s with a step of 256 s over 24 hr intervals. This results in time‐frequency arrays for each parameter covering the 0.5 mHz to 0.5 Hz frequency range. The database is accessible at http://plasma.spacescience.ro/cluster.html. In total there are 47 wave parameters in the database, among them being the ellipticity, the degree of polarization, the (unsigned) wave vector direction, and the Poynting vector. Plots for the planarity, elongation, and degeneration of the Cluster tetrahedron are also available. At the moment, the database covers measurements made between 01 January 2001 and 31 December 2020 with more data being added in time. Here we present this database, discuss the methods used to derive the parameters and give practical examples. Plain Language Summary: This work describe an on‐line database containing data and plots of physical quantities characterizing low frequency waves detected by the Cluster spacecraft fleet in the space plasma around the Earth. These quantities are derived using measurements of the magnetic field, electric field, and particles taken by the four spacecraft over 20 years. The plots can be used to quickly assess the plasma waves activity over a certain time interval, while the data can be used for further analysis. Key Points: The Cluster Virtual Observatory (CVO) is an on‐line archive of low frequency wave parameters based on Cluster measurementsThe CVO also provides the tetrahedron geometrical configuration parametersThe waves and configuration parameters are available as quick‐plots as well as binary Hierarchical Data Format data [ABSTRACT FROM AUTHOR]

Published
2023
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14. Magnetic holes between Earth and Mercury: BepiColombo cruise phase.

Author

Volwerk, M., Karlsson, T., Heyner, D., Goetz, C., Simon Wedlund, C., Plaschke, F., Schmid, D., Fischer, D., Mieth, J., Richter, I., Nakamura, R., Narita, Y., Magnes, W., Auster, U., Matsuoka, A., Baumjohann, W., and Glassmeier, K.-H.

Subjects
SOLAR system, SOLAR wind, MERCURY (Planet), MAGNETIC flux density, MAGNETIC structure, MERCURY
Abstract

Context. Magnetic holes are ubiquitous structures in the solar wind and in planetary magnetosheaths. They consist of a strong depression of the magnetic field strength, most likely in pressure balance through increased plasma pressure, which is convected with the plasma flow. These structures are created through a plasma temperature anisotropy, where the perpendicular temperature (with respect to the magnetic field) is greater than the parallel temperature. The occurrence rate of these magnetic holes between Earth and Mercury can give us information about how the solar wind conditions develop on their way from the Sun to the outer Solar System. They also give information about basic plasma processes such as diffusion of magnetic structures. Aims. In this study we investigate the occurrence, size, and depth of magnetic holes during the cruise phase of BepiColombo and compare them with earlier studies. Methods. The BepiColombo magnetometer data were used to find the magnetic holes. We determined the size in seconds, the depth with respect to the background field, and the rotation angle of the background field across the structure. Minimum variance analysis delivers the polarization state of the magnetic holes. A direct comparison is made to the results obtained from the MESSENGER cruise phase. Results. We find an almost constant occurrence rate for magnetic holes between Mercury and Earth. The size of the holes is determined by the plasma conditions at the location where they are created and they grow in size, due to diffusion, as they move outwards in the Solar System. The greater the rotation of the background magnetic field across the structure, the larger the minimum size of the magnetic hole is. [ABSTRACT FROM AUTHOR]

Published
2023
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15. Does Magnetic Reconnection Occur in the Near Lunar Surface Environment?

Author

Sawyer, R. P., Halekas, J. S., Bonnell, J. W., Chen, L. J., McFadden, J., Glassmeier, K. H., Harada, Y., and Stanier, A.

Subjects
MAGNETIC reconnection, INTERPLANETARY magnetic fields, SOLAR wind, LUNAR surface, SOLAR magnetic fields, MAGNETIC fields
Abstract

The near lunar surface contains small‐scale magnetic field structures that provide a natural test bed for observing plasmas with a non‐zero Hall electric field, as well as potentially facilitating electron‐only reconnection. This study presents observational evidence of magnetized electrons as well as demagnetized ions when THEMIS‐ARTEMIS probe B reached an altitude of ∼15 km above the lunar surface. Additionally, observations suggest the presence of a field line topology change and traversal of a closed magnetic field structure containing solar wind electrons, suggestive of magnetic reconnection having occurred at some point between the solar wind interplanetary magnetic field and a lunar crustal magnetic field. Thus, the observations presented here are consistent with previous studies that predict prominent Hall electric fields near lunar crustal magnetic fields and further suggest that the solar wind interplanetary magnetic field may reconnect with lunar crustal magnetic fields, most likely via electron‐only reconnection. Plain Language Summary: While interactions between the solar wind and the Earth's magnetosphere have been well studied, there is still much to be learned by studying the interactions between the solar wind and the small‐scale lunar magnetic fields. Due to the small‐scale nature of the lunar magnetic fields, previous studies have suggested that the ions do not respond in the same manner as the electrons. The resulting effects lead to an electric field near regions of lunar magnetic fields. This study presents observational evidence of the aforementioned phenomena. Additionally, the spacecraft observations also suggest that magnetic reconnection, or the breaking of the lunar magnetic field lines and reconnection to the magnetic field in the solar wind, was occurring between the solar wind and the lunar magnetic fields. Key Points: Observations suggest magnetic reconnection occurs between the solar wind IMF and lunar crustal magnetic fieldsElectron pitch angle and velocity distributions suggest the spacecraft traversed a closed magnetic topology containing solar wind electronsWe report in‐situ observations of demagnetized ions and associated Hall electric fields near the lunar surface [ABSTRACT FROM AUTHOR]

Published
2023
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21. Identifying Ultra Low Frequency Waves in the Lunar Plasma Environment Using Trajectory Analysis and Resonance Conditions

Author

Howard, S. K, Halekas, J. S, Farrell, W. M, Mcfadden, J. P, and Glassmeier, K.-H

Subjects
Plasma Physics
Abstract

Abstract Recent studies show that localized crustal magnetic fields on the lunar surface can reflect a significant portion of the incoming solar wind protons. These reflected ions can drive a wide range of plasma waves. It is difficult to determine the intrinsic properties of low-frequency waves with single-spacecraft observations, which can be heavily Doppler shifted. We describe a technique to combine trajectory analysis of reflected protons with the Doppler shift and resonance conditions to identify ultralow-frequency waves at the Moon. On 31 January 2014 plasma waves were detected by one of the Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) probes as it approached the lunar wake; these waves were not detected by the second ARTEMIS probe located upstream in the undisturbed solar wind. The observed waves had a frequency below the local ion cyclotron frequency and had right-hand circular polarization in the reference frame of the Moon. By solving the Doppler shift and the cyclotron resonance equations, we determined the conditions for reflected ions to excite the observed waves. Simulated trajectories of reflected ions correspond to ARTEMIS ion observations and support the hypothesis that reflected ions are the primary driver of the waves. By combining trajectory analysis with the resonance conditions, we identify scenarios where ions that satisfy the resonance conditions are present in the right location to generate the observed waves. Using this method, we can uniquely identify the observed waves as upstream propagating right-hand polarized waves, subject to the assumption that they are generated by cyclotron resonance with ions.

Published
2017
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22. Interplanetary Coronal Mass Ejection Observed at STEREO-A, Mars, Comet 67P/Churyumov-Gerasimenko, Saturn,and New Horizons En Route to Pluto: Comparison of Its Forbush Decreases at 1.4, 3.1, and 9.9 AU

Author

Witasse, O, Sánchez-Cano, B, Mays, M. L, Kajdic, P, Opgenoorth, H, Elliott, H. A, Richardson, I. G, Zouganelis, I, Zender, J, Wimmer-Schweingruber, R. F, Turc, L, Taylor, M. G. G. T, Roussos, E, Rouillard, A, Richter, I, Richardson, J. D, Ramstad, R, Provan, G, Posner, A, Plaut, J. J, Odstrcil, D, Nilsson, H, Niemenen, P, Milan, S. E, Mandt, K, Lohf, H, Lester, M, Lebreton, J.-P, Kuulkers, E, Krupp, N, Koenders, C, James, M. K, Intzekara, D, Holmstrom, M, Hassler, D. M, Hall, B. E. S, Guo, J, Goldstein, R, Goetz, C, Glassmeier, K. H, Genot, V, Evans, H, Espley, J, Edberg, N. J. T, Dougherty, M, Cowley, S. W. H, Burch, J, Behar, E, Barabash, S, Andrews, D. J, and Altobelli, N

Subjects
Lunar And Planetary Science And Exploration
Abstract

We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, Mars Atmosphere and Volatile EvolutioN Mission (MAVEN), Mars Odyssey, and Mars Science Laboratory (MSL) missions, 44 h before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9 AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a nonambiguous signature at New Horizons. A potential detection of this ICME by Voyager 2 at 110-111 AU is also discussed. The multispacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116deg, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P, and Saturn.

Published
2017
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28. The fluxgate magnetometer of the BepiColombo Mercury Planetary Orbiter

Author

Glassmeier, K.-H., Auster, H.-U., Heyner, D., Okrafka, K., Carr, C., Berghofer, G., Anderson, B.J., Balogh, A., Baumjohann, W., Cargill, P., Christensen, U., Delva, M., Dougherty, M., Fornaçon, K.-H., Horbury, T.S., Lucek, E.A., Magnes, W., Mandea, M., Matsuoka, A., Matsushima, M., Motschmann, U., Nakamura, R., Narita, Y., O’Brien, H., Richter, I., Schwingenschuh, K., Shibuya, H., Slavin, J.A., Sotin, C., Stoll, B., Tsunakawa, H., Vennerstrom, S., Vogt, J., and Zhang, T.

Published
2010
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29. On Electron-Scale Whistler Turbulence in the Solar Wind

Author

Narita, Y, Nakamura, R, Baumjohann, W, Glassmeier, K.-H, Motschmann, U, Giles, B, Magnes, W, Fischer, D, Torbert, R. B, and Russell, C. T

Subjects
Plasma Physics, General
Abstract

For the first time, the dispersion relation for turbulence magnetic field fluctuations in the solar wind is determined directly on small scales of the order of the electron inertial length, using four-point magnetometer observations from the Magnetospheric Multiscale mission. The data are analyzed using the high-resolution adaptive wave telescope technique. Small-scale solar wind turbulence is primarily composed of highly obliquely propagating waves, with dispersion consistent with that of the whistler mode.

Published
2016
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33. Cometary plasma science

Author

Goetz, C., Gunell, H., Volwerk, M., Beth, A., Eriksson, A., Galand, M., Henri, Pierre, Nilsson, H., Wedlund, C. Simon, Alho, M., Andersson, L., Andre, N., De Keyser, J., Deca, J., Ge, Y., Glassmeier, K.-H., Hajra, R., Karlsson, T., Kasahara, S., Kolmasova, I., LLera, K., Madanian, H., Mann, I., Mazelle, C., Odelstad, E., Plaschke, F., Rubin, M., Sanchez-Cano, B., Snodgrass, C., Vigren, E., ESA - ESTEC (Netherlands), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics]
Abstract

International audience; Comets hold the key to the understanding of our Solar System, its formation and its evolution, and to the fundamental plasma processes at work both in it and beyond it. A comet nucleus emits gas as it is heated by the sunlight. The gas forms the coma, where it is ionised, becomes a plasma, and eventually interacts with the solar wind. Besides these neutral and ionised gases, the coma also contains dust grains, released from the comet nucleus. As a cometary atmosphere develops when the comet travels through the Solar System, large-scale structures, such as the plasma boundaries, develop and disappear, while at planets such large-scale structures are only accessible in their fully grown, quasi-steady state. In situ measurements at comets enable us to learn both how such large-scale structures are formed or reformed and how small-scale processes in the plasma affect the formation and properties of these large scale structures. Furthermore, a comet goes through a wide range of parameter regimes during its life cycle, where either collisional processes, involving neutrals and charged particles, or collisionless processes are at play, and might even compete in complicated transitional regimes. Thus a comet presents a unique opportunity to study this parameter space, from an asteroid-like to a Mars- and Venus-like interaction. The Rosetta mission and previous fast flybys of comets have together made many new discoveries, but the most important breakthroughs in the understanding of cometary plasmas are yet to come. The Comet Interceptor mission will provide a sample of multi-point measurements at a comet, setting the stage for a multi-spacecraft mission to accompany a comet on its journey through the Solar System. This White Paper, submitted in response to the European Space Agency’s Voyage 2050 call, reviews the present-day knowledge of cometary plasmas, discusses the many questions that remain unanswered, and outlines a multi-spacecraft European Space Agency mission to accompany a comet that will answer these questions by combining both multi-spacecraft observations and a rendezvous mission, and at the same time advance our understanding of fundamental plasma physics and its role in planetary systems.

Published
2021
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34. OSS (Outer Solar System): a fundamental and planetary physics mission to Neptune, Triton and the Kuiper Belt

Author

Christophe, B., Spilker, L. J., Anderson, J. D., André, N., Asmar, S. W., Aurnou, J., Banfield, D., Barucci, A., Bertolami, O., Bingham, R., Brown, P., Cecconi, B., Courty, J. -M., Dittus, H., Fletcher, L. N., Foulon, B., Francisco, F., Gil, P. J. S., Glassmeier, K. H., Grundy, W., Hansen, C., Helbert, J., Helled, R., Hussmann, H., Lamine, B., Lämmerzahl, C., Lamy, L., Lehoucq, R., Lenoir, B., Levy, A., Orton, G., Páramos, J., Poncy, J., Postberg, F., Progrebenko, S. V., Reh, K. R., Reynaud, S., Robert, C., Samain, E., Saur, J., Sayanagi, K. M., Schmitz, N., Selig, H., Sohl, F., Spilker, T. R., Srama, R., Stephan, K., Touboul, P., and Wolf, P.

Published
2012
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39. THEMIS observations of two substorms on February 26, 2008

Author

Chu, XiangNing, Pu, ZuYin, Cao, Xin, Wang, Jue, Mishin, V., Angelopoulos, V., Liu, Jiang, Wei, Yong, Glassmeier, K. H., Mcfadden, J., Larson, D., Mende, S., Frey, H., Russell, C. T., Mann, I., Sibeck, D., Zong, QiuGang, Fu, SuiYan, Xie, Lun, Saifudinova, T. I., Tolochko, M. V., Sapronova, L. A., Reme, H., and Lucek, E.

Published
2010
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41. First Results from the THEMIS Mission

Author

Angelopoulos, V., Sibeck, D., Carlson, C. W., McFadden, J. P., Larson, D., Lin, R. P., Bonnell, J. W., Mozer, F. S., Ergun, R., Cully, C., Glassmeier, K. H., Auster, U., Roux, A., LeContel, O., Frey, S., Phan, T., Mende, S., Frey, H., Donovan, E., Russell, C. T., Strangeway, R., Liu, J., Mann, I., Rae, J., Raeder, J., Li, X., Liu, W., Singer, H. J., Sergeev, V. A., Apatenkov, S., Parks, G., Fillingim, M., and Sigwarth, J.

Published
2008
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43. First Results of the THEMIS Search Coil Magnetometers

Author

Le Contel, O., Roux, A., Robert, P., Coillot, C., Bouabdellah, A., de la Porte, B., Alison, D., Ruocco, S., Angelopoulos, V., Bromund, K., Chaston, C. C., Cully, C., Auster, H. U., Glassmeier, K. H., Baumjohann, W., Carlson, C. W., McFadden, J. P., and Larson, D.

Published
2008
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44. The THEMIS Fluxgate Magnetometer

Author

Auster, H. U., Glassmeier, K. H., Magnes, W., Aydogar, O., Baumjohann, W., Constantinescu, D., Fischer, D., Fornacon, K. H., Georgescu, E., Harvey, P., Hillenmaier, O., Kroth, R., Ludlam, M., Narita, Y., Nakamura, R., Okrafka, K., Plaschke, F., Richter, I., Schwarzl, H., Stoll, B., Valavanoglou, A., and Wiedemann, M.

Published
2008
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47. ROMAP: Rosetta Magnetometer and Plasma Monitor

Author

Auster, H. U., Apathy, I., Berghofer, G., Remizov, A., Roll, R., Fornacon, K. H., Glassmeier, K. H., Haerendel, G., Hejja, I., Kührt, E., Magnes, W., Moehlmann, D., Motschmann, U., Richter, I., Rosenbauer, H., Russell, C. T., Rustenbach, J., Sauer, K., Schwingenschuh, K., Szemerey, I., and Waesch, R.

Published
2007
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48. RPC: The Rosetta Plasma Consortium

Author

Carr, C., Cupido, E., Lee, C. G. Y., Balogh, A., Beek, T., Burch, J. L., Dunford, C. N., Eriksson, A. I., Gill, R., Glassmeier, K. H., Goldstein, R., Lagoutte, D., Lundin, R., Lundin, K., Lybekk, B., Michau, J. L., Musmann, G., Nilsson, H., Pollock, C., Richter, I., and Trotignon, J. G.

Published
2007
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49. The Solar Orbiter magnetometer

Author

Horbury, T. S., O'Brien, H., Carrasco Blazquez, I., Bendyk, M., Brown, P., Hudson, R., Evans, V., Carr, C. M., Beek, T. J., Cupido, E, Bhattacharya, S., Dominguez, J.-A., Matthews, L., Myklebust, V. R., Whiteside, B., Bale, S. D., Baumjohann, W., Burgess, D., Carbone, V, Cargill, P, Eastwood, J, Erdös, G, Fletcher, L, Forsyth, R, Giacalone, J, Glassmeier, K.-H., Goldstein, M L, Hoeksema, T, Lockwood, Mike, Magnes, W, Maksimovic, M, Marsch, E, Matthaeus, W. H., Murphy, N, Nakariakov, V M, Owen, C J, Owens, Mathew, Rodriguez-Pacheco, J, Richter, I, Riley, P, Russell, C T, Schwartz, S, Vainio, R, Velli, M, Vennerstrom, S, Walsh, R, Wimmer-Schweingruber, R F, Zank, G, Müller, D, Zouganelis, I, and Walsh, A

Subjects
Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

The magnetometer instrument on the Solar Orbiter mission is designed to measure the magnetic field local to the spacecraft continuously for the entire mission duration. The need to characterise not only the background magnetic field but also its variations on scales from far above to well below the proton gyroscale result in challenging requirements on stability, precision, and noise, as well as magnetic and operational limitations on both the spacecraft and other instruments. The challenging vibration and thermal environment has led to significant development of the mechanical sensor design. The overall instrument design, performance, data products, and operational strategy are described.

Published
2020

50. Plasma and Energetic Particle Behaviors During Asymmetric Magnetic Reconnection at the Magnetopause

Author

Lee, S. H, Zhang, H, Zong, Q.-G, Otto, A, Sibeck, D. G, Wang, Y, Glassmeier, K.-H, Daly, P.W, and Reme, H

Subjects
Geophysics
Abstract

The factors controlling asymmetric reconnection and the role of the cold plasma population in the reconnection process are two outstanding questions. We present a case study of multipoint Cluster observations demonstrating that the separatrix and flow boundary angles are greater on the magnetosheath than on the magnetospheric side of the magnetopause, probably due to the stronger density than magnetic field asymmetry at this boundary. The motion of cold plasmaspheric ions entering the reconnection region differs from that of warmer magnetosheath and magnetospheric ions. In contrast to the warmer ions, which are probably accelerated by reconnection in the diffusion region near the subsolar magnetopause, the colder ions are simply entrained by 𝐄×𝐁 drifts at high latitudes on the recently reconnected magnetic field lines. This indicates that plasmaspheric ions can sometimes play only a very limited role in asymmetric reconnection, in contrast to previous simulation studies. Three cold ion populations (probably H+, He+, and O+) appear in the energy spectrum, consistent with ion acceleration to a common velocity.

Published
2014
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