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Publications (10 of 154) Show all publications
Graham, D. B., Khotyaintsev, Y. V., Andre, M., Vaivads, A., Divin, A., Drake, J. F., . . . Dokgo, K. (2022). Direct observations of anomalous resistivity and diffusion in collisionless plasma. Nature Communications, 13(1), Article ID 2954.
Open this publication in new window or tab >>Direct observations of anomalous resistivity and diffusion in collisionless plasma
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2022 (English)In: Nature Communications, E-ISSN 2041-1723, Vol. 13, no 1, article id 2954Article in journal (Refereed) Published
Abstract [en]

Coulomb collisions provide plasma resistivity and diffusion but in many low-density astrophysical plasmas such collisions between particles are extremely rare. Scattering of particles by electromagnetic waves can lower the plasma conductivity. Such anomalous resistivity due to wave-particle interactions could be crucial to many processes, including magnetic reconnection. It has been suggested that waves provide both diffusion and resistivity, which can support the reconnection electric field, but this requires direct observation to confirm. Here, we directly quantify anomalous resistivity, viscosity, and cross-field electron diffusion associated with lower hybrid waves using measurements from the four Magnetospheric Multiscale (MMS) spacecraft. We show that anomalous resistivity is approximately balanced by anomalous viscosity, and thus the waves do not contribute to the reconnection electric field. However, the waves do produce an anomalous electron drift and diffusion across the current layer associated with magnetic reconnection. This leads to relaxation of density gradients at timescales of order the ion cyclotron period, and hence modifies the reconnection process.

It is suggested that waves can provide both diffusion and resistivity that can potentially support the reconnection electric field in low-density astrophysical plasmas. Here, the authors show, using direct spacecraft measurements, that the waves contribute to anomalous diffusion but do not contribute to the reconnection electric field.

Place, publisher, year, edition, pages
Springer NatureSpringer Nature, 2022
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-476810 (URN)10.1038/s41467-022-30561-8 (DOI)000800650200003 ()35618713 (PubMedID)
Funder
Swedish National Space Board, 128/17Swedish National Space Board, 176/15Swedish Research Council, 2016-05507European Commission, 2016-05507
Available from: 2022-06-20 Created: 2022-06-20 Last updated: 2024-01-15Bibliographically approved
Krasnoselskikh, V., Tsurutani, B. T., Dudok de Wit, T., Walker, S., Balikhin, M., Balat-Pichelin, M., . . . Fedorov, A. (2022). ICARUS: in-situ studies of the solar corona beyond Parker Solar Probe and Solar Orbiter. Experimental astronomy, 54(2-3), 277-315
Open this publication in new window or tab >>ICARUS: in-situ studies of the solar corona beyond Parker Solar Probe and Solar Orbiter
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2022 (English)In: Experimental astronomy, ISSN 0922-6435, E-ISSN 1572-9508, Vol. 54, no 2-3, p. 277-315Article in journal (Refereed) Published
Abstract [en]

The primary scientific goal of ICARUS (Investigation of Coronal AcceleRation and heating of solar wind Up to the Sun), a mother-daughter satellite mission, proposed in response to the ESA “Voyage 2050” Call, will be to determine how the magnetic field and plasma dynamics in the outer solar atmosphere give rise to the corona, the solar wind, and the entire heliosphere. Reaching this goal will be a Rosetta Stone step, with results that are broadly applicable within the fields of space plasma physics and astrophysics. Within ESA’s Cosmic Vision roadmap, these science goals address Theme 2: “How does the Solar System work?” by investigating basic processes occurring “From the Sun to the edge of the Solar System”. ICARUS will not only advance our understanding of the plasma environment around our Sun, but also of the numerous magnetically active stars with hot plasma coronae. ICARUS I will perform the first direct in situ measurements of electromagnetic fields, particle acceleration, wave activity, energy distribution, and flows directly in the regions in which the solar wind emerges from the coronal plasma. ICARUS I will have a perihelion altitude of 1 solar radius and will cross the region where the major energy deposition occurs. The polar orbit of ICARUS I will enable crossing the regions where both the fast and slow winds are generated. It will probe the local characteristics of the plasma and provide unique information about the physical processes involved in the creation of the solar wind. ICARUS II will observe this region using remote-sensing instruments, providing simultaneous, contextual information about regions crossed by ICARUS I and the solar atmosphere below as observed by solar telescopes. It will thus provide bridges for understanding the magnetic links between the heliosphere and the solar atmosphere. Such information is crucial to our understanding of the plasma physics and electrodynamics of the solar atmosphere. ICARUS II will also play a very important relay role, enabling the radio-link with ICARUS I. It will receive, collect, and store information transmitted from ICARUS I during its closest approach to the Sun. It will also perform preliminary data processing before transmitting it to Earth. Performing such unique in situ observations in the area where presumably hazardous solar energetic particles are energized, ICARUS will provide fundamental advances in our capabilities to monitor and forecast the space radiation environment. Therefore, the results from the ICARUS mission will be extremely crucial for future space explorations, especially for long-term crewed space missions.

Place, publisher, year, edition, pages
Springer Nature, 2022
Keywords
Solar wind, Heliophysics, Solar atmosphere, Space mission
National Category
Astronomy, Astrophysics and Cosmology Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-512819 (URN)10.1007/s10686-022-09878-1 (DOI)000941045200001 ()
Available from: 2023-09-29 Created: 2023-09-29 Last updated: 2024-01-17Bibliographically approved
Norgren, C., Graham, D. B., Argall, M. R., Steinvall, K., Hesse, M., Khotyaintsev, Y. V., . . . Plaschke, F. (2022). Millisecond observations of nonlinear wave-electron interaction in electron phase space holes. Physics of Plasmas, 29(1), Article ID 012309.
Open this publication in new window or tab >>Millisecond observations of nonlinear wave-electron interaction in electron phase space holes
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2022 (English)In: Physics of Plasmas, ISSN 1070-664X, E-ISSN 1089-7674, Vol. 29, no 1, article id 012309Article in journal (Refereed) Published
Abstract [en]

Electron phase space holes (EHs) associated with electron trapping are commonly observed as bipolar electric field signatures in both space and laboratory plasma. Until recently, it has not been possible to resolve EHs in electron measurements. We report observations of EHs in the plasma sheet boundary layer, here identified as the separatrix region of magnetic reconnection in the magnetotail. The intense EHs are observed together with an electron beam moving toward the X line, showing signs of thermalization. Using the electron drift instrument onboard the satellites of the Magnetospheric Multiscale mission, we make direct millisecond measurements of the electron particle flux associated with individual electron phase space holes. The electron flux is measured at a millisecond cadence in a narrow parallel speed range within that of the trapped electrons. The flux modulations are of order unity and are direct evidence of the strong nonlinear wave-electron interaction that may effectively thermalize beams and contribute to transforming directed drift energy to thermal energy. (C) 2022 Author(s). All article content, except where otherwise noted, is licensed under a Creative Commons Attribution (CC BY) license (http://creativecommons.org/licenses/by/4.0/).

Place, publisher, year, edition, pages
American Institute of Physics (AIP)AIP Publishing, 2022
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-467448 (URN)10.1063/5.0073097 (DOI)000748468100001 ()
Available from: 2022-02-14 Created: 2022-02-14 Last updated: 2024-01-15Bibliographically approved
Allen, R. C., Cernuda, I., Pacheco, D., Berger, L., Xu, Z. G., von Forstner, J. L., . . . Yedla, M. (2021). Energetic ions in the Venusian system: Insights from the first Solar Orbiter flyby. Astronomy and Astrophysics, 656, Article ID A7.
Open this publication in new window or tab >>Energetic ions in the Venusian system: Insights from the first Solar Orbiter flyby
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2021 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 656, article id A7Article in journal (Refereed) Published
Abstract [en]

The Solar Orbiter flyby of Venus on 27 December 2020 allowed for an opportunity to measure the suprathermal to energetic ions in the Venusian system over a large range of radial distances to better understand the acceleration processes within the system and provide a characterization of galactic cosmic rays near the planet. Bursty suprathermal ion enhancements (up to similar to 10 keV) were observed as far as similar to 50R(V) downtail. These enhancements are likely related to a combination of acceleration mechanisms in regions of strong turbulence, current sheet crossings, and boundary layer crossings, with a possible instance of ion heating due to ion cyclotron waves within the Venusian tail. Upstream of the planet, suprathermal ions are observed that might be related to pick-up acceleration of photoionized exospheric populations as far as 5R(V) upstream in the solar wind as has been observed before by missions such as Pioneer Venus Orbiter and Venus Express. Near the closest approach of Solar Orbiter, the Galactic cosmic ray (GCR) count rate was observed to decrease by approximately 5 percent, which is consistent with the amount of sky obscured by the planet, suggesting a negligible abundance of GCR albedo particles at over 2 R-V. Along with modulation of the GCR population very close to Venus, the Solar Orbiter observations show that the Venusian system, even far from the planet, can be an effective accelerator of ions up to similar to 30 keV. This paper is part of a series of the first papers from the Solar Orbiter Venus flyby.

Place, publisher, year, edition, pages
EDP SciencesEDP Sciences, 2021
Keywords
acceleration of particles, planets and satellites, terrestrial planets, planet-star interactions, planetary systems, turbulence, waves
National Category
Astronomy, Astrophysics and Cosmology Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-464272 (URN)10.1051/0004-6361/202140803 (DOI)000730246400013 ()
Funder
Swedish National Space BoardSwedish National Space Board, 2020-00111
Available from: 2022-01-19 Created: 2022-01-19 Last updated: 2024-01-15Bibliographically approved
Maksimovic, M., Soucek, J., Chust, T., Khotyaintsev, Y. V., Kretzschmar, M., Bonnin, X., . . . Zouganelis, I. (2021). First observations and performance of the RPW instrument on board the Solar Orbiter mission. Astronomy and Astrophysics, 656, Article ID A41.
Open this publication in new window or tab >>First observations and performance of the RPW instrument on board the Solar Orbiter mission
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2021 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 656, article id A41Article in journal (Refereed) Published
Abstract [en]

The Radio and Plasma Waves (RPW) instrument on the ESA Solar Orbiter mission is designed to measure in situ magnetic and electric fields and waves from the continuum up to several hundred kHz. The RPW also observes solar and heliospheric radio emissions up to 16 MHz. It was switched on and its antennae were successfully deployed two days after the launch of Solar Orbiter on February 10, 2020. Since then, the instrument has acquired enough data to make it possible to assess its performance and the electromagnetic disturbances it experiences. In this article, we assess its scientific performance and present the first RPW observations. In particular, we focus on a statistical analysis of the first observations of interplanetary dust by the instrument's Thermal Noise Receiver. We also review the electro-magnetic disturbances that RPW suffers, especially those which potential users of the instrument data should be aware of before starting their research work.

Place, publisher, year, edition, pages
EDP SciencesEDP Sciences, 2021
Keywords
solar wind, Sun, radio radiation, general
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:uu:diva-464276 (URN)10.1051/0004-6361/202141271 (DOI)000730246400039 ()
Funder
Swedish National Space Board
Available from: 2022-01-17 Created: 2022-01-17 Last updated: 2024-01-15Bibliographically approved
Pisa, D., Souček, J., Santolik, O., Hanzelka, M., Nicolaou, G., Maksimovic, M., . . . Louarn, P. (2021). First-year ion-acoustic wave observations in the solar wind by the RPW/TDS instrument on board Solar Orbiter. Astronomy and Astrophysics, 656, Article ID A14.
Open this publication in new window or tab >>First-year ion-acoustic wave observations in the solar wind by the RPW/TDS instrument on board Solar Orbiter
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2021 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 656, article id A14Article in journal (Refereed) Published
Abstract [en]

Context. 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. During the first year of the mission, the RPW/TDS instrument was operating from the first perihelion in mid-June 2020 and through the first flyby of Venus in late December 2020. Aims. 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.

Methods. 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.

Results. Electrostatic ion-acoustic waves are the most common wave emissions observed between the local electron and proton plasma frequency by the TDS receiver during the first year of the mission. 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 10 000 triggered waveform snapshots shows the mean wave frequency at about 3 kHz and wave amplitude about 2.5 mV m(-1). The wave amplitude varies as R-1.38 with the heliocentric distance. The relative phase distribution between two components of the E-field projected in the Y - Z Spacecraft Reference Frame (SRF) plane 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.

Place, publisher, year, edition, pages
EDP SciencesEDP Sciences, 2021
Keywords
waves, solar wind, plasmas, instabilities
National Category
Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-464273 (URN)10.1051/0004-6361/202140928 (DOI)000730246400038 ()
Funder
Swedish National Space Board
Available from: 2022-01-19 Created: 2022-01-19 Last updated: 2024-01-15Bibliographically approved
Catapano, F., Retino, A., Zimbardo, G., Alexandrova, A., Cohen, I. J., Turner, D. L., . . . Burch, J. L. (2021). In Situ Evidence of Ion Acceleration between Consecutive Reconnection Jet Fronts. Astrophysical Journal, 908(1), Article ID 73.
Open this publication in new window or tab >>In Situ Evidence of Ion Acceleration between Consecutive Reconnection Jet Fronts
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2021 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 908, no 1, article id 73Article in journal (Refereed) Published
Abstract [en]

Processes driven by unsteady reconnection can efficiently accelerate particles in many astrophysical plasmas. An example is the reconnection jet fronts in an outflow region. We present evidence of suprathermal ion acceleration between two consecutive reconnection jet fronts observed by the Magnetospheric Multiscale mission in the terrestrial magnetotail. An earthward propagating jet is approached by a second faster jet. Between the jets, the thermal ions are mostly perpendicular to magnetic field, are trapped, and are gradually accelerated in the parallel direction up to 150 keV. Observations suggest that ions are predominantly accelerated by a Fermi-like mechanism in the contracting magnetic bottle formed between the two jet fronts. The ion acceleration mechanism is presumably efficient in other environments where jet fronts produced by variable rates of reconnection are common and where the interaction of multiple jet fronts can also develop a turbulent environment, e.g., in stellar and solar eruptions.

Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP)IOP PUBLISHING LTD, 2021
Keywords
Space plasmas, Plasma jets, Solar magnetic reconnection
National Category
Astronomy, Astrophysics and Cosmology Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-437420 (URN)10.3847/1538-4357/abce5a (DOI)000618345100001 ()
Available from: 2021-03-11 Created: 2021-03-11 Last updated: 2024-01-15Bibliographically approved
Chust, T., Kretzschmar, M., Graham, D. B., Le Contel, O., Retino, A., Alexandrova, A., . . . Angelini, V. (2021). Observations of whistler mode waves by Solar Orbiter's RPW Low Frequency Receiver (LFR): In-flight performance and first results. Astronomy and Astrophysics, 656, Article ID A17.
Open this publication in new window or tab >>Observations of whistler mode waves by Solar Orbiter's RPW Low Frequency Receiver (LFR): In-flight performance and first results
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2021 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 656, article id A17Article in journal (Refereed) Published
Abstract [en]

Context. The Radio and Plasma Waves (RPW) instrument is one of the four in situ instruments of the ESA/NASA Solar Orbiter mission, which was successfully launched on February 10, 2020. The Low Frequency Receiver (LFR) is one of its subsystems, designed to characterize the low frequency electric (quasi-DC - 10 kHz) and magnetic (similar to 1 Hz-10 kHz) fields that develop, propagate, interact, and dissipate in the solar wind plasma. Combined with observations of the particles and the DC magnetic field, LFR measurements will help to improve the understanding of the heating and acceleration processes at work during solar wind expansion.

Aims. The capability of LFR to observe and analyze a variety of low frequency plasma waves can be demontrated by taking advantage of whistler mode wave observations made just after the near-Earth commissioning phase of Solar Orbiter. In particular, this is related to its capability of measuring the wave normal vector, the phase velocity, and the Poynting vector for determining the propagation characteristics of the waves.

Methods. Several case studies of whistler mode waves are presented, using all possible LFR onboard digital processing products, waveforms, spectral matrices, and basic wave parameters.

Results. Here, we show that whistler mode waves can be very properly identified and characterized, along with their Doppler-shifted frequency, based on the waveform capture as well as on the LFR onboard spectral analysis.

Conclusions. Despite the fact that calibrations of the electric and magnetic data still require some improvement, these first whistler observations show a good overall consistency between the RPW LFR data, indicating that many science results on these waves, as well as on other plasma waves, can be obtained by Solar Orbiter in the solar wind.

Place, publisher, year, edition, pages
EDP SciencesEDP Sciences, 2021
Keywords
solar wind, waves, plasmas, instrumentation, miscellaneous
National Category
Astronomy, Astrophysics and Cosmology Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-464268 (URN)10.1051/0004-6361/202140932 (DOI)000730246400055 ()
Funder
Swedish National Space Board
Available from: 2022-01-19 Created: 2022-01-19 Last updated: 2024-01-15Bibliographically approved
Soucek, J., Pisa, D., Kolmasova, I., Uhlir, L., Lan, R., Santolik, O., . . . Bonnin, X. (2021). Solar Orbiter Radio and Plasma Waves - Time Domain Sampler: In-flight performance and first results. Astronomy and Astrophysics, 656, Article ID A26.
Open this publication in new window or tab >>Solar Orbiter Radio and Plasma Waves - Time Domain Sampler: In-flight performance and first results
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2021 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 656, article id A26Article in journal (Refereed) Published
Abstract [en]

Context. The Radio and Plasma Waves (RPW) instrument on board Solar Orbiter has been operating nearly continuously since the launch in February 2020. The Time Domain Sampler (TDS) receiver of the RPW instrument is dedicated to waveform measurements of plasma waves and dust impact signatures in an intermediate frequency range from 0.2 to 200 kHz.

Aims. This article presents the first data from the RPW-TDS receiver and discusses the in-flight performance of the instrument and, in particular, the on-board wave and dust detection algorithm. We present the TDS data products and its scientific operation. We demonstrate the content of the dataset on several examples. In particular, we study the distribution of solar Langmuir waves in the first year of observations and one Type III burst event.

Methods. The on-board detection algorithm is described in detail in this article and classifies the observed waveform snapshots, identifying plasma waves and dust impacts based on the ratio of their maximum amplitude to their median and on the spectral bandwidth. The algorithm allows TDS to downlink the most scientifically relevant waveforms and to perform an on-board statistical characterization of the processed data.

Results. The detection algorithm of TDS is shown to perform very well in its detection of plasma waves and dust impacts with a high accuracy. The initial analysis of statistical data returned by TDS shows that sporadic Langmuir waves that are not associated with Type III events are routinely observed in the inner heliosphere, with a clear increase in occurrence rate closer to the Sun. We also present an example of RPW observations during an encounter of the source region of a Type III burst, which exploits the on-board calculated histograms data.

Place, publisher, year, edition, pages
EDP SciencesEDP Sciences, 2021
Keywords
plasmas, solar wind, waves, Sun, radio radiation, space vehicles, instruments, heliosphere
National Category
Astronomy, Astrophysics and Cosmology Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-464270 (URN)10.1051/0004-6361/202140948 (DOI)000730246400036 ()
Funder
Swedish National Space Board, 20/136
Available from: 2022-01-19 Created: 2022-01-19 Last updated: 2024-01-15Bibliographically approved
Matteini, L., Laker, R., Horbury, T., Woodham, L., Bale, S. D., Stawarz, J. E., . . . Müller, D. (2021). Solar Orbiter's encounter with the tail of comet C/2019 Y4 (ATLAS): Magnetic field draping and cometary pick-up ion waves. Astronomy and Astrophysics, 656, Article ID A39.
Open this publication in new window or tab >>Solar Orbiter's encounter with the tail of comet C/2019 Y4 (ATLAS): Magnetic field draping and cometary pick-up ion waves
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2021 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 656, article id A39Article in journal (Refereed) Published
Abstract [en]

Context. Solar Orbiter is expected to have flown close to the tail of comet C/2019 Y4 (ATLAS) during the spacecraft’s first perihelion in June 2020. Models predict a possible crossing of the comet tails by the spacecraft at a distance from the Sun of approximately 0.5 AU.

Aims. This study is aimed at identifying possible signatures of the interaction of the solar wind plasma with material released by comet ATLAS, including the detection of draped magnetic field as well as the presence of cometary pick-up ions and of ion-scale waves excited by associated instabilities. This encounter provides us with the first opportunity of addressing such dynamics in the inner Heliosphere and improving our understanding of the plasma interaction between comets and the solar wind.

Methods. We analysed data from all in situ instruments on board Solar Orbiter and compared their independent measurements in order to identify and characterize the nature of structures and waves observed in the plasma when the encounter was predicted.

Results. We identified a magnetic field structure observed at the start of 4 June, associated with a full magnetic reversal, a local deceleration of the flow and large plasma density, and enhanced dust and energetic ions events. The cross-comparison of all these observations support a possible cometary origin for this structure and suggests the presence of magnetic field draping around some low-field and high-density object. Inside and around this large scale structure, several ion-scale wave-forms are detected that are consistent with small-scale waves and structures generated by cometary pick-up ion instabilities.

Conclusions. Solar Orbiter measurements are consistent with the crossing through a magnetic and plasma structure of cometary origin embedded in the ambient solar wind. We suggest that this corresponds to the magnetotail of one of the fragments of comet ATLAS or to a portion of the tail that was previously disconnected and advected past the spacecraft by the solar wind.

Place, publisher, year, edition, pages
EDP SciencesEDP Sciences, 2021
Keywords
solar wind, comets: individual: C/2019 Y4 ATLAS, plasmas, waves, instabilities
National Category
Astronomy, Astrophysics and Cosmology Fusion, Plasma and Space Physics
Identifiers
urn:nbn:se:uu:diva-464454 (URN)10.1051/0004-6361/202141229 (DOI)000730246400011 ()
Funder
Swedish National Space Board
Available from: 2022-01-17 Created: 2022-01-17 Last updated: 2024-01-15Bibliographically approved
Organisations
Identifiers
ORCID iD: ORCID iD iconorcid.org/0000-0003-1654-841X

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