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28 results on '"Píša, D."'

1. First dust measurements with the Solar Orbiter Radio and Plasma Wave instrument

Author

Zaslavsky, A., Mann, I., Soucek, J., Czechowski, A., Pisa, D., Vaverka, J., Meyer-Vernet, N., Maksimovic, M., Lorfèvre, E., Issautier, K., Babić, K. Racković, Bale, S. D., Morooka, M., Vecchio, A., Chust, T., Khotyaintsev, Y., Krasnoselskikh, V., Kretzschmar, M., Plettemeier, D., Steller, M., Štverák, Š., Trávníček, P., and Vaivads, A.

Subjects
Physics - Space Physics
Abstract

Impacts of dust grains on spacecraft are known to produce typical impulsive signals in the voltage waveform recorded at the terminals of electric antennas. Such signals are routinely detected by the Time Domain Sampler (TDS) system of the Radio and Plasma Waves (RPW) instrument aboard Solar Orbiter. We investigate the capabilities of RPW in terms of interplanetary dust studies and present the first analysis of dust impacts recorded by this instrument. We discuss previously developed models of voltage pulses generation after a dust impact onto a spacecraft and present the relevant technical parameters for Solar Orbiter RPW as a dust detector. Then we present the statistical analysis of the dust impacts recorded by RPW/TDS from April 20th, 2020 to February 27th, 2021 between 0.5 AU and 1 AU. The study shows that the dust population studied presents a radial velocity component directed outward from the Sun, the order of magnitude of which can be roughly estimated as $v_{r, dust} \simeq 50$ km.$s^{-1}$. This is consistent with the flux of impactors being dominated by $\beta$-meteoroids. We estimate the cumulative flux of these grains at 1 AU to be roughly $F_\beta \simeq 8\times 10^{-5} $ m$^{-2}$s$^{-1}$, for particles of radius $r \gtrsim 100$ nm. The power law index $\delta$ of the cumulative mass flux of the impactors is evaluated by two differents methods (direct observations of voltage pulses and indirect effect on the impact rate dependency on the impact speed). Both methods give a result $\delta \simeq 0.3-0.4$. Solar Orbiter RPW proves to be a suitable instrument for interplanetary dust studies. These first results are promising for the continuation of the mission, in particular for the in-situ study of the dust cloud outside the ecliptic plane, which Solar Orbiter will be the first spacecraft to explore., Comment: 13 pages, 8 figures

Published
2021
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2. First-year ion-acoustic wave observations in the solar wind by the RPW/TDS instrument onboard Solar Orbiter

Author

Píša, D., Souček, J., Santolík, O., Hanzelka, M., Nicolaou, G., Maksimovic, M., Bale, S. D., Chust, T., Khotyaintsev, Y., Krasnoselskikh, V., Kretzschmar, M., Lorfèvre, E., Plettemeier, D., Steller, M., Štverák, Š., Trávníček, P., Vaivads, A., Vecchio, A., Horbury, T., O'Brien, H., Evans, V., Angelini, V., Owen, C. J., and Louarn, P.

Subjects
Physics - Space Physics, Astrophysics - Solar and Stellar Astrophysics, Physics - Plasma Physics
Abstract

Electric field measurements of the Time Domain Sampler (TDS) receiver, part of the Radio and Plasma Waves (RPW) instrument on board Solar Orbiter, often exhibit very intense broadband wave emissions at frequencies below 20~kHz in the spacecraft frame. In this paper, we present a year-long study of electrostatic fluctuations observed in the solar wind at an interval of heliocentric distances from 0.5 to 1~AU. The RPW/TDS observations provide a nearly continuous data set for a statistical study of intense waves below the local plasma frequency. The on-board and continuously collected and processed properties of waveform snapshots allow for the mapping plasma waves at frequencies between 200~Hz and 20~kHz. We used the triggered waveform snapshots and a Doppler-shifted solution of the dispersion relation for wave mode identification in order to carry out a detailed spectral and polarization analysis. Electrostatic ion-acoustic waves are the common wave emissions observed between the local electron and proton plasma frequency in the soler wind. The occurrence rate of ion-acoustic waves peaks around perihelion at distances of 0.5~AU and decreases with increasing distances, with only a few waves detected per day at 0.9~AU. Waves are more likely to be observed when the local proton moments and magnetic field are highly variable. A more detailed analysis of more than 10000 triggered waveform snapshots shows the mean wave frequency at about 3 kHz and wave amplitude about 2.5 mV/m. The wave amplitude varies as 1/R^(1.38) with the heliocentric distance. The relative phase distribution between two components of the E-field shows a mostly linear wave polarization. Electric field fluctuations are closely aligned with the directions of the ambient field lines. Only a small number (3%) of ion-acoustic waves are observed at larger magnetic discontinuities., Comment: 9 pages, 8 figures

Published
2021
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3. Kinetic Electrostatic Waves and their Association with Current Structures in the Solar Wind

Author

Graham, D. B., Khotyaintsev, Yu. V., Vaivads, A., Edberg, N. J. T., Eriksson, A. I., Johansson, E., Sorriso-Valvo, L., Maksimovic, M., Souček, J., Píša, D., Bale, S. D., Chust, T., Kretzschmar, M., Krasnoselskikh, V., Lorfèvre, E., Plettemeier, D., Steller, M., Štverák, Š., Trávníček, P., Vecchio, A., Horbury, T. S., O'Brien, H., Evans, V., and Angelini, V.

Subjects
Physics - Space Physics, Astrophysics - Solar and Stellar Astrophysics, Physics - Plasma Physics
Abstract

A variety of kinetic waves develop in the solar wind. The relationship between these waves and larger-scale structures, such as current sheets and ongoing turbulence remain a topic of investigation. Similarly, the instabilities producing ion-acoustic waves in the solar wind remains an open question. The goals of this paper are to investigate kinetic electrostatic Langmuir and ion-acoustic waves in the solar wind at 0.5 AU and determine whether current sheets and associated streaming instabilities can produce the observed waves. The relationship between these waves and currents is investigated statistically. Solar Orbiter's Radio and Plasma Waves instrument suite provides high-resolution snapshots of the fluctuating electric field. The Low Frequency Receiver resolves the waveforms of ion-acoustic waves and the Time Domain Sampler resolves the waveforms of both ion-acoustic and Langmuir waves. Using these waveform data we determine when these waves are observed in relation to current structures in the solar wind, estimated from the background magnetic field. Langmuir and ion-acoustic waves are frequently observed in the solar wind. Ion-acoustic waves are observed about 1% of the time at 0.5 AU. The waves are more likely to be observed in regions of enhanced currents. However, the waves typically do not occur at current structures themselves. The observed currents in the solar wind are too small to drive instability by the relative drift between single ion and electron populations. When multi-component ion and/or electron distributions are present the observed currents may be sufficient for instability. Ion beams are the most plausible source of ion-acoustic waves. The spacecraft potential is confirmed to be a reliable probe of the background electron density by comparing the peak frequencies of Langmuir waves with the plasma frequency calculated from the spacecraft potential., Comment: 13 pages, 12 figures

Published
2021
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4. Virtual European Solar & Planetary Access (VESPA): a Planetary Science Virtual Observatory cornerstone

Author

Erard, S., Cecconi, B., Sidaner, P. Le, Chauvin, C., Rossi, A. P., Minin, M., Capria, T., Ivanovski, S., Schmitt, B., Genot, V., Andre, N., Marmo, C., Vandaele, A. C., Trompet, L., Scherf, M., Hueso, R., Maattanen, A., Carry, B., Achilleos, N., Soucek, J., Pisa, D., Benson, K., Fernique, P., and Millour, E.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Europlanet-2020 programme, which ended on Aug 31st, 2019, included an activity called VESPA (Virtual European Solar and Planetary Access), which focused on adapting Virtual Observatory (VO) techniques to handle Planetary Science data. This paper describes some aspects of VESPA at the end of this 4-years development phase and at the onset of the newly selected Europlanet-2024 programme starting in 2020. The main objectives of VESPA are to facilitate searches both in big archives and in small databases, to enable data analysis by providing simple data access and online visualization functions, and to allow research teams to publish derived data in an interoperable environment as easily as possible. VESPA encompasses a wide scope, including surfaces, atmospheres, magnetospheres and planetary plasmas, small bodies, helio-physics, exoplanets, and spectroscopy in solid phase. This system relies in particular on standards and tools developed for the Astronomy VO (IVOA) and extends them where required to handle specificities of Solar System studies. It also aims at making the VO compatible with tools and protocols developed in different contexts, for instance GIS for planetary surfaces, or time series tools for plasma-related measurements. An essential part of the activity is to publish a significant amount of high-quality data in this system, with a focus on derived products resulting from data analysis or simulations., Comment: Submitted to Data Science Journal

Published
2019

5. VESPA: a community-driven Virtual Observatory in Planetary Science

Author

Erard, S., Cecconi, B., Sidaner, P. Le, Rossi, A. P., Capria, T., Schmitt, B., Génot, V., André, N., Vandaele, A. C., Scherf, M., Hueso, R., Määttänen, A., Thuillot, W., Carry, B., Achilleos, N., Marmo, C., Santolik, O., Benson, K., Fernique, P., Beigbeder, L., Millour, E., Rousseau, B., Andrieu, F., Chauvin, C., Minin, M., Ivanoski, S., Longobardo, A., Bollard, P., Albert, D., Gangloff, M., Jourdane, N., Bouchemit, M., Glorian, J. -M., Trompet, L., Al-Ubaidi, T., Juaristi, J., Desmars, J., Guio, P., Delaa, O., Lagain, A., Soucek, J., and Pisa, D.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The VESPA data access system focuses on applying Virtual Observatory (VO) standards and tools to Planetary Science. Building on a previous EC-funded Europlanet program, it has reached maturity during the first year of a new Europlanet 2020 program (started in 2015 for 4 years). The infrastructure has been upgraded to handle many fields of Solar System studies, with a focus both on users and data providers. This paper describes the broad lines of the current VESPA infrastructure as seen by a potential user, and provides examples of real use cases in several thematic areas. These use cases are also intended to identify hints for future developments and adaptations of VO tools to Planetary Science., Comment: Planetary and Space Sciences (in press), Special Issue "Enabling Open and Interoperable Access to Planetary Science and Heliophysics Databases and Tools". 43 pages, 14 figures, 1 table

Published
2017
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6. Ion‐Acoustic Waves Associated With Interplanetary Shocks.

Author

Boldú, J. J., Graham, D. B., Morooka, M., André, M., Khotyaintsev, Yu. V., Dimmock, A., Píša, D., Souček, J., Maksimovic, M., Louarn, P., Fedorov, A., Nicolaou, G., and Owen, C.

Subjects
ELECTRON distribution, PLASMA waves, ELECTRIC currents, PLASMA instabilities, THERMODYNAMIC equilibrium
Abstract

Ion‐acoustic waves (IAWs) commonly occur near interplanetary (IP) shocks. These waves are important because of their potential role in the dissipation required for collisionless shocks to exist. We study IAW occurrence statistically at different heliocentric distances using Solar Orbiter to identify the processes responsible for IAW generation near IP shocks. We show that close to IP shocks the occurrence rate of IAW increases and peaks at the ramp. In the upstream region, the IAW activity is highly variable among different shocks and increases with decreasing distance from the Sun. We show that the observed currents near IP shocks are insufficient to reach the threshold for the current‐driven instability. We argue that two‐stream proton distributions and suprathermal electrons are likely sources of the waves. Plain Language Summary: Ion‐acoustic waves (IAWs) are fluctuations in the electric field that occur at frequencies close to the ion plasma frequency. These waves are commonly found in the solar wind and often cluster around interplanetary (IP) shock waves. In this study, we investigate and quantify how common IAWs are in the vicinity of IP shocks. Our research revealed that IAW activity is enhanced before and after most IP shock passages. Furthermore, IAWs are more likely to be observed preceding IP shocks that are closer to the Sun. We find that the occurrence rate of IAWs shows no clear dependence on the IP shock parameters. We explore the possible mechanisms that could explain the presence of these IAWs. For instance, IAW modes can be excited by electric currents if the associated drift velocity between ions and electrons is above a certain threshold. However, the currents alone are not strong enough to generate the IAWs found near IP shocks. We discuss other potential generation mechanisms, such as velocity distributions of ions and electrons deviating from thermodynamic equilibrium. Key Points: The occurrence of Ion‐acoustic waves (IAWs) is enhanced at interplanetary (IP) shocks, peaking at the shock rampThe occurrence rate of IAWs in the upstream region of IP shocks increases with decreasing radial distance from the SunIAWs are observed upstream of an IP shock together with two‐stream protons and an electron strahl [ABSTRACT FROM AUTHOR]

Published
2024
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7. Langmuir waves associated with magnetic holes in the solar wind.

Author

Boldú, J. J., Graham, D. B., Morooka, M., André, M., Khotyaintsev, Yu. V., Karlsson, T., Souček, J., Píša, D., and Maksimovic, M.

Subjects
SOLAR radio bursts, SOLAR wind, PLASMA Langmuir waves, PLASMA waves, DISTRIBUTION (Probability theory), MAGNETIC fields, RADIO waves
Abstract

Context. Langmuir waves (electrostatic waves near the electron plasma frequency) are often observed in the solar wind and may play a role in the energy dissipation of electrons. The largest amplitude Langmuir waves are typically associated with type II and III solar radio bursts and planetary foreshocks. In addition, Langmuir waves not related to radio bursts occur in the solar wind, but their source is not well understood. Langmuir waves have been observed inside isolated magnetic holes, suggesting that magnetic holes play an important role in the generation of Langmuir waves. Aims. We provide the statistical distribution of Langmuir waves in the solar wind at different heliocentric distances. In particular, we investigate the relationship between magnetic holes and Langmuir waves. We identify possible source regions of Langmuir waves in the solar wind, other than radio bursts, by analyzing the local plasma conditions. Methods. We analyzed data from Solar Orbiter's Radio and Plasma Waves (RPW) and Magnetometer (MAG) instruments. We used the triggered electric field snapshots and onboard statistical data (STAT) of the Time Domain Sampler (TDS) of RPW to identify Langmuir waves and investigate their properties. The plasma densities were derived from the spacecraft potential estimated by RPW. The MAG data were used to monitor the background magnetic field and detect magnetic holes, which are defined as regions with an isolated decrease in |B| of 50% or more compared to the background level. The statistical analysis was performed on data from 2020 to 2021, comprising heliocentric distances between 0.5 AU and 1 AU. Results. We show that 78% of the Langmuir waves in the solar wind not connected to radio bursts occur in regions of local magnetic field depletions, including the regions classified as isolated magnetic holes. We also show that the Langmuir waves occur more frequently inside magnetic holes than in any other region in the solar wind, which indicates that magnetic holes are important source regions of solar wind Langmuir waves. We find that Langmuir waves associated with magnetic holes in the solar wind typically have lower amplitudes than those associated with radio bursts. [ABSTRACT FROM AUTHOR]

Published
2023
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9. Plasma Wave Observations with Cassini at Saturn

Author

Hospodarsky, George B., primary, Menietti, J. D., additional, Píša, D., additional, Kurth, W. S., additional, Gurnett, D. A., additional, Persoon, A. M., additional, Leisner, J. S., additional, and Averkamp, T. F., additional

Published
2016
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10. First near-relativistic solar electron events observed by EPD onboard Solar Orbiter

Author

Gómez-Herrero, R., primary, Pacheco, D., additional, Kollhoff, A., additional, Espinosa Lara, F., additional, Freiherr von Forstner, J. L., additional, Dresing, N., additional, Lario, D., additional, Balmaceda, L., additional, Krupar, V., additional, Malandraki, O. E., additional, Aran, A., additional, Bučík, R., additional, Klassen, A., additional, Klein, K.-L., additional, Cernuda, I., additional, Eldrum, S., additional, Reid, H., additional, Mitchell, J. G., additional, Mason, G. M., additional, Ho, G. C., additional, Rodríguez-Pacheco, J., additional, Wimmer-Schweingruber, R. F., additional, Heber, B., additional, Berger, L., additional, Allen, R. C., additional, Janitzek, N. P., additional, Laurenza, M., additional, De Marco, R., additional, Wijsen, N., additional, Kartavykh, Y. Y., additional, Dröge, W., additional, Horbury, T. S., additional, Maksimovic, M., additional, Owen, C. J., additional, Vecchio, A., additional, Bonnin, X., additional, Kruparova, O., additional, Píša, D., additional, Souček, J., additional, Louarn, P., additional, Fedorov, A., additional, O’Brien, H., additional, Evans, V., additional, Angelini, V., additional, Zucca, P., additional, Prieto, M., additional, Sánchez-Prieto, S., additional, Carrasco, A., additional, Blanco, J. J., additional, Parra, P., additional, Rodríguez-Polo, O., additional, Martín, C., additional, Terasa, J. C., additional, Boden, S., additional, Kulkarni, S. R., additional, Ravanbakhsh, A., additional, Yedla, M., additional, Xu, Z., additional, Andrews, G. B., additional, Schlemm, C. E., additional, Seifert, H., additional, Tyagi, K., additional, Lees, W. J., additional, and Hayes, J., additional

Published
2021
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11. First-year ion-acoustic wave observations in the solar wind by the RPW/TDS instrument on board Solar Orbiter

Author

Píša, D., primary, Souček, J., additional, Santolík, O., additional, Hanzelka, M., additional, Nicolaou, G., additional, Maksimovic, M., additional, Bale, S. D., additional, Chust, T., additional, Khotyaintsev, Y., additional, Krasnoselskikh, V., additional, Kretzschmar, M., additional, Lorfèvre, E., additional, Plettemeier, D., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vaivads, A., additional, Vecchio, A., additional, Horbury, T., additional, O’Brien, H., additional, Evans, V., additional, Angelini, V., additional, Owen, C. J., additional, and Louarn, P., additional

Published
2021
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12. First dust measurements with the Solar Orbiter Radio and Plasma Wave instrument

Author

Zaslavsky, A., primary, Mann, I., additional, Soucek, J., additional, Czechowski, A., additional, Píša, D., additional, Vaverka, J., additional, Meyer-Vernet, N., additional, Maksimovic, M., additional, Lorfèvre, E., additional, Issautier, K., additional, Rackovic Babic, K., additional, Bale, S. D., additional, Morooka, M., additional, Vecchio, A., additional, Chust, T., additional, Khotyaintsev, Y., additional, Krasnoselskikh, V., additional, Kretzschmar, M., additional, Plettemeier, D., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, and Vaivads, A., additional

Published
2021
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13. Solar Orbiter Radio and Plasma Waves – Time Domain Sampler: In-flight performance and first results

Author

Soucek, J., primary, Píša, D., additional, Kolmasova, I., additional, Uhlir, L., additional, Lan, R., additional, Santolík, O., additional, Krupar, V., additional, Kruparova, O., additional, Baše, J., additional, Maksimovic, M., additional, Bale, S. D., additional, Chust, T., additional, Khotyaintsev, Yu. V., additional, Krasnoselskikh, V., additional, Kretzschmar, M., additional, Lorfèvre, E., additional, Plettemeier, D., additional, Steller, M., additional, Štverák, Š., additional, Vaivads, A., additional, Vecchio, A., additional, Bérard, D., additional, and Bonnin, X., additional

Published
2021
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14. Kinetic electrostatic waves and their association with current structures in the solar wind

Author

Graham, D. B., primary, Khotyaintsev, Yu. V., additional, Vaivads, A., additional, Edberg, N. J. T., additional, Eriksson, A. I., additional, Johansson, E. P. G., additional, Sorriso-Valvo, L., additional, Maksimovic, M., additional, Souček, J., additional, Píša, D., additional, Bale, S. D., additional, Chust, T., additional, Kretzschmar, M., additional, Krasnoselskikh, V., additional, Lorfèvre, E., additional, Plettemeier, D., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vecchio, A., additional, Horbury, T. S., additional, O’Brien, H., additional, Evans, V., additional, and Angelini, V., additional

Published
2021
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15. First observations and performance of the RPW instrument on board the Solar Orbiter mission

Author

Maksimovic, M., primary, Souček, J., additional, Chust, T., additional, Khotyaintsev, Y., additional, Kretzschmar, M., additional, Bonnin, X., additional, Vecchio, A., additional, Alexandrova, O., additional, Bale, S. D., additional, Bérard, D., additional, Brochot, J.-Y., additional, Edberg, N. J. T., additional, Eriksson, A., additional, Hadid, L. Z., additional, Johansson, E. P. G., additional, Karlsson, T., additional, Katra, B., additional, Krasnoselskikh, V., additional, Krupař, V., additional, Lion, S., additional, Lorfèvre, E., additional, Matteini, L., additional, Nguyen, Q. N., additional, Píša, D., additional, Piberne, R., additional, Plettemeier, D., additional, Rucker, H. O., additional, Santolík, O., additional, Steinvall, K., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vaivads, A., additional, Zaslavsky, A., additional, Chaintreuil, S., additional, Dekkali, M., additional, Astier, P.-A., additional, Barbary, G., additional, Boughedada, K., additional, Cecconi, B., additional, Chapron, F., additional, Collin, C., additional, Dias, D., additional, Guéguen, L., additional, Lamy, L., additional, Leray, V., additional, Malac-Allain, L. R., additional, Pantellini, F., additional, Parisot, J., additional, Plasson, P., additional, Thijs, S., additional, Fratter, I., additional, Bellouard, E., additional, Danto, P., additional, Julien, S., additional, Guilhem, E., additional, Fiachetti, C., additional, Sanisidro, J., additional, Laffaye, C., additional, Gonzalez, F., additional, Pontet, B., additional, Quéruel, N., additional, Jannet, G., additional, Fergeau, P., additional, Dudok de Wit, T., additional, Vincent, T., additional, Agrapart, C., additional, Pragout, J., additional, Bergerard-Timofeeva, M., additional, Delory, G. T., additional, Turin, P., additional, Jeandet, A., additional, Leroy, P., additional, Pellion, J.-C., additional, Bouzid, V., additional, Recart, W., additional, Kolmašová, I., additional, Krupařová, O., additional, Uhlíř, L., additional, Lán, R., additional, Baše, J., additional, André, M., additional, Bylander, L., additional, Cripps, V., additional, Cully, C., additional, Jansson, S.-E., additional, Puccio, W., additional, Břínek, J., additional, Ottacher, H., additional, Angelini, V., additional, Berthomier, M., additional, Evans, V., additional, Goetz, K., additional, Hellinger, P., additional, Horbury, T. S., additional, Issautier, K., additional, Kontar, E., additional, Le Contel, O., additional, Louarn, P., additional, Martinović, M., additional, Müller, D., additional, O’Brien, H., additional, Owen, C. J., additional, Retino, A., additional, Rodríguez-Pacheco, J., additional, Sahraoui, F., additional, Sanchez, L., additional, Walsh, A. P., additional, Wimmer-Schweingruber, R. F., additional, and Zouganelis, I., additional

Published
2021
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16. Solar Orbiter’s first Venus flyby: Observations from the Radio and Plasma Wave instrument

Author

Hadid, L. Z., primary, Edberg, N. J. T., additional, Chust, T., additional, Píša, D., additional, Dimmock, A. P., additional, Morooka, M. W., additional, Maksimovic, M., additional, Khotyaintsev, Yu. V., additional, Souček, J., additional, Kretzschmar, M., additional, Vecchio, A., additional, Le Contel, O., additional, Retino, A., additional, Allen, R. C., additional, Volwerk, M., additional, Fowler, C. M., additional, Sorriso-Valvo, L., additional, Karlsson, T., additional, Santolík, O., additional, Kolmašová, I., additional, Sahraoui, F., additional, Stergiopoulou, K., additional, Moussas, X., additional, Issautier, K., additional, Dewey, R. M., additional, Klein Wolt, M., additional, Malandraki, O. E., additional, Kontar, E. P., additional, Howes, G. G., additional, Bale, S. D., additional, Horbury, T. S., additional, Martinović, M., additional, Vaivads, A., additional, Krasnoselskikh, V., additional, Lorfèvre, E., additional, Plettemeier, D., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, O’Brien, H., additional, Evans, V., additional, Angelini, V., additional, Velli, M. C., additional, and Zouganelis, I., additional

Published
2021
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17. The Solar Orbiter Radio and Plasma Waves (RPW) instrument (Corrigendum)

Author

Maksimovic, M., primary, Bale, S. D., additional, Chust, T., additional, Khotyaintsev, Y., additional, Krasnoselskikh, V., additional, Kretzschmar, M., additional, Plettemeier, D., additional, Rucker, H. O., additional, Souček, J., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vaivads, A., additional, Chaintreuil, S., additional, Dekkali, M., additional, Alexandrova, O., additional, Astier, P.-A., additional, Barbary, G., additional, Bérard, D., additional, Bonnin, X., additional, Boughedada, K., additional, Cecconi, B., additional, Chapron, F., additional, Chariet, M., additional, Collin, C., additional, de Conchy, Y., additional, Dias, D., additional, Guéguen, L., additional, Lamy, L., additional, Leray, V., additional, Lion, S., additional, Malac-Allain, L. R., additional, Matteini, L., additional, Nguyen, Q. N., additional, Pantellini, F., additional, Parisot, J., additional, Plasson, P., additional, Thijs, S., additional, Vecchio, A., additional, Fratter, I., additional, Bellouard, E., additional, Lorfèvre, E., additional, Danto, P., additional, Julien, S., additional, Guilhem, E., additional, Fiachetti, C., additional, Sanisidro, J., additional, Laffaye, C., additional, Gonzalez, F., additional, Pontet, B., additional, Quéruel, N., additional, Jannet, G., additional, Fergeau, P., additional, Brochot, J.-Y., additional, Cassam-Chenai, G., additional, Dudok de Wit, T., additional, Timofeeva, M., additional, Vincent, T., additional, Agrapart, C., additional, Delory, G. T., additional, Turin, P., additional, Jeandet, A., additional, Leroy, P., additional, Pellion, J.-C., additional, Bouzid, V., additional, Katra, B., additional, Piberne, R., additional, Recart, W., additional, Santolík, O., additional, Kolmašová, I., additional, Krupař, V., additional, Krupařová, O., additional, Píša, D., additional, Uhlíř, L., additional, Lán, R., additional, Baše, J., additional, Ahlèn, L., additional, André, M., additional, Bylander, L., additional, Cripps, V., additional, Cully, C., additional, Eriksson, A., additional, Jansson, S.-E., additional, Johansson, E. P. G., additional, Karlsson, T., additional, Puccio, W., additional, Břínek, J., additional, Öttacher, H., additional, Panchenko, M., additional, Berthomier, M., additional, Goetz, K., additional, Hellinger, P., additional, Horbury, T. S., additional, Issautier, K., additional, Kontar, E., additional, Krucker, S., additional, Le Contel, O., additional, Louarn, P., additional, Martinović, M., additional, Owen, C. J., additional, Retino, A., additional, Rodríguez-Pacheco, J., additional, Sahraoui, F., additional, Wimmer-Schweingruber, R. F., additional, Zaslavsky, A., additional, and Zouganelis, I., additional

Published
2021
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18. The Solar Orbiter Radio and Plasma Waves (RPW) instrument

Author

Maksimovic, M., primary, Bale, S. D., additional, Chust, T., additional, Khotyaintsev, Y., additional, Krasnoselskikh, V., additional, Kretzschmar, M., additional, Plettemeier, D., additional, Rucker, H. O., additional, Souček, J., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vaivads, A., additional, Chaintreuil, S., additional, Dekkali, M., additional, Alexandrova, O., additional, Astier, P.-A., additional, Barbary, G., additional, Bérard, D., additional, Bonnin, X., additional, Boughedada, K., additional, Cecconi, B., additional, Chapron, F., additional, Chariet, M., additional, Collin, C., additional, de Conchy, Y., additional, Dias, D., additional, Guéguen, L., additional, Lamy, L., additional, Leray, V., additional, Lion, S., additional, Malac-Allain, L. R., additional, Matteini, L., additional, Nguyen, Q. N., additional, Pantellini, F., additional, Parisot, J., additional, Plasson, P., additional, Thijs, S., additional, Vecchio, A., additional, Fratter, I., additional, Bellouard, E., additional, Lorfèvre, E., additional, Danto, P., additional, Julien, S., additional, Guilhem, E., additional, Fiachetti, C., additional, Sanisidro, J., additional, Laffaye, C., additional, Gonzalez, F., additional, Pontet, B., additional, Quéruel, N., additional, Jannet, G., additional, Fergeau, P., additional, Brochot, J.-Y., additional, Cassam-Chenai, G., additional, Dudok de Wit, T., additional, Timofeeva, M., additional, Vincent, T., additional, Agrapart, C., additional, Delory, G. T., additional, Turin, P., additional, Jeandet, A., additional, Leroy, P., additional, Pellion, J.-C., additional, Bouzid, V., additional, Katra, B., additional, Piberne, R., additional, Recart, W., additional, Santolík, O., additional, Kolmašová, I., additional, Krupař, V., additional, Krupařová, O., additional, Píša, D., additional, Uhlíř, L., additional, Lán, R., additional, Baše, J., additional, Ahlèn, L., additional, André, M., additional, Bylander, L., additional, Cripps, V., additional, Cully, C., additional, Eriksson, A., additional, Jansson, S.-E., additional, Johansson, E. P. G., additional, Karlsson, T., additional, Puccio, W., additional, Břínek, J., additional, Öttacher, H., additional, Panchenko, M., additional, Berthomier, M., additional, Goetz, K., additional, Hellinger, P., additional, Horbury, T. S., additional, Issautier, K., additional, Kontar, E., additional, Krucker, S., additional, Le Contel, O., additional, Louarn, P., additional, Martinović, M., additional, Owen, C. J., additional, Retino, A., additional, Rodríguez-Pacheco, J., additional, Sahraoui, F., additional, Wimmer-Schweingruber, R. F., additional, Zaslavsky, A., additional, and Zouganelis, I., additional

Published
2020
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27. Electrostatic solitary waves observed at Saturn by Cassini inside 10 Rsand near Enceladus

Author

Pickett, J. S., Kurth, W. S., Gurnett, D. A., Huff, R. L., Faden, J. B., Averkamp, T. F., Píša, D., and Jones, G. H.

Abstract

We have analyzed the Cassini Radio and Plasma Wave Science Wideband Receiver (WBR) data specifically looking for the presence of bipolar electrostatic solitary waves (ESWs). Typical examples of these ESWs are provided to show that when they are present, several of them may be detected over a few to several millisecond time span. We carried out an event study of an Enceladus encounter which took place on 9 October 2008. Approximately 30 min prior to and during the crossing of the Enceladus dust plume, several ESWs are observed with amplitudes of about 100 μV/m up to about 140 mV/m, and time durations of several tens of microseconds up to 250 µs. The highest amplitudes (over 10 mV/m) were observed only during the closest approach to Enceladus. We also carried out an ESW survey using the WBR for all years from 2004 to 2008 for distances less than 10 Rs. The survey clearly shows that most of the ESWs are found on the nightside, with a high percentage of them in the range of 4–6 Rs. This location is consistent with the densest part of Saturn's E ring and Enceladus' orbit. These are the first extended survey results of ESWs near Saturn and the first reported ESWs in connection with Enceladus. We discuss possibilities for the generation of these nonlinear ESWs, which involve current, beam, and acoustic, including dust, instabilities. These are the first reported ESWs observed in connection with EnceladusThese are the first survey results of the location of ESWs observed near SaturnCharacteristics of ESWs observed near Saturn are provided

Published
2015
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