Search

Your search keyword '"Sauvaud, J-A"' showing total 1,002 results
Start Over Author "Sauvaud, J-A"
1,002 results on '"Sauvaud, J-A"'

1. AMBRE: A Compact Instrument to Measure Thermal Ions, Electrons and Electrostatic Charging Onboard Spacecraft

Author

Lavraud, B., Cara, A., Payan, D., Ballot, Y., Sauvaud, J. -A., Mathon, R., Camus, T., Chassela, O., Seran, H. -C., Tap, H., Bernal, O., Berthomier, M., Devoto, P., Fedorov, A., Rouzaud, J., Rubiella-Romeo, J., Techer, J. -D, Zely, D., Galinier, S., and Bruno, D.

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

The Active Monitor Box of Electrostatic Risks (AMBER) is a double-head thermal electron and ion electrostatic analyzer (energy range 0-30 keV) that was launched onboard the Jason-3 spacecraft in 2016. The next generation AMBER instrument, for which a first prototype was developed and then calibrated at the end of 2017, constitutes a significant evolution that is based on a single head to measure both species alternatively. The instrument developments focused on several new subsystems (front-end electronics, high-voltage electronics, mechanical design) that permit to reduce instrument resources down to ~ 1 kg and 1.5 W. AMBER is designed as a generic radiation monitor with a twofold purpose: (1) measure magnetospheric thermal ion and electron populations in the range 0-35 keV, with significant scientific potential (e.g., plasmasphere, ring current, plasma sheet), and (2) monitor spacecraft electrostatic charging and the plasma populations responsible for it, for electromagnetic cleanliness and operational purposes.

Published
2019
Full Text
View/download PDF

2. LatHyS global hybrid simulation of the BepiColombo second Venus flyby

Author

Aizawa, S., Persson, M., Menez, T., André, N., Modolo, R., Génot, V., Sanchez-Cano, B., Volwerk, M., Chaufray, J.-Y., Baskevitch, C., Heyner, D., Saito, Y., Harada, Y., Leblanc, F., Barthe, A., Penou, E., Fedorov, A., Sauvaud, J.-A., Yokota, S., Auster, U., Richter, I., Mieth, J., Horbury, T.S., Louarn, P., Owen, C.J., and Murakami, G.

Published
2022
Full Text
View/download PDF

3. BepiColombo mission confirms stagnation region of Venus and reveals its large extent

Author

Persson, M., Aizawa, S., André, N., Barabash, S., Saito, Y., Harada, Y., Heyner, D., Orsini, S., Fedorov, A., Mazelle, C., Futaana, Y., Hadid, L. Z., Volwerk, M., Collinson, G., Sanchez-Cano, B., Barthe, A., Penou, E., Yokota, S., Génot, V., Sauvaud, J. A., Delcourt, D., Fraenz, M., Modolo, R., Milillo, A., Auster, H.-U., Richter, I., Mieth, J. Z. D., Louarn, P., Owen, C. J., Horbury, T. S., Asamura, K., Matsuda, S., Nilsson, H., Wieser, M., Alberti, T., Varsani, A., Mangano, V., Mura, A., Lichtenegger, H., Laky, G., Jeszenszky, H., Masunaga, K., Signoles, C., Rojo, M., and Murakami, G.

Published
2022
Full Text
View/download PDF

4. Improved Energy Resolution Measurements of Electron Precipitation Observed During an IPDP‐Type EMIC Event

Author

Clilverd, M.A., Rodger, C.J., Hendry, A.T., Lozinski, A.R., Sauvaud, J.‐A., Lessard, M.R., Raita, T., Clilverd, M.A., Rodger, C.J., Hendry, A.T., Lozinski, A.R., Sauvaud, J.‐A., Lessard, M.R., and Raita, T.

Abstract

High energy resolution DEMETER satellite observations from the Instrument for the Detection of Particle (IDP) are analyzed during an electromagnetic ion cyclotron (EMIC)-induced electron precipitation event. Analysis of an Interval Pulsation with Diminishing Periods (IPDP)-type EMIC wave event, using combined satellite observations to correct for incident proton contamination, detected an energy precipitation spectrum ranging from ∼150 keV to ∼1.5 MeV. While inconsistent with many theoretical predictions of >1 MeV EMIC-induced electron precipitation, the finding is consistent with an increasing number of experimentally observed events detected using lower resolution integral channel measurements on the POES, FIREBIRD, and ELFIN satellites. Revised and improved DEMETER differential energy fluxes, after correction for incident proton contamination shows that they agree to within 40% in peak flux magnitude, and 85 keV (within 40%) for the energy at which the peak occurred as calculated from POES integral channel electron precipitation measurements. This work shows that a subset of EMIC waves found close to the plasmapause, that is, IPDP-type rising tone events, can produce electron precipitation with peak energies substantially below 1 MeV. The rising tone features of IPDP EMIC waves, along with the association with the high cold plasma density regime, and the rapidly varying electron density gradients of the plasmapause may be an important factor in the generation of such low energy precipitation, co-incident with a high energy tail. Our work highlights the importance of undertaking proton contamination correction when using the high-resolution DEMETER particle measurements to investigate EMIC-driven electron precipitation.

Published
2024

5. Structure and dynamics of the Hermean magnetosphere revealed by electron observations from the Mercury electron analyzer after the first three Mercury flybys of BepiColombo

Author

Rojo, M., Andre, N., Aizawa, S., Sauvaud, J. -A, Saito, Y., Harada, Y., Fedorov, A., Penou, E., Barthe, A., Persson, Moa, Yokota, S., Mazelle, C., Hadid, L. Z., Delcourt, D., Fontaine, D., Fraenz, M., Katra, B., Krupp, N., Murakami, G., Rojo, M., Andre, N., Aizawa, S., Sauvaud, J. -A, Saito, Y., Harada, Y., Fedorov, A., Penou, E., Barthe, A., Persson, Moa, Yokota, S., Mazelle, C., Hadid, L. Z., Delcourt, D., Fontaine, D., Fraenz, M., Katra, B., Krupp, N., and Murakami, G.

Abstract

Context: The Mercury electron analyzer (MEA) obtained new electron observations during the first three Mercury flybys by BepiColombo on October 1, 2021 (MFB1), June 23 , 2022 (MFB2), and June 19, 2023 (MFB3). BepiColombo entered the dusk side magnetotail from the flank magnetosheath in the northern hemisphere, crossed the Mercury solar orbital equator around midnight in the magnetotail, traveled from midnight to dawn in the southern hemisphere near the closest approach, and exited from the post-dawn magnetosphere into the dayside magnetosheath. Aims: We aim to identify the magnetospheric boundaries and describe the structure and dynamics of the electron populations observed in the various regions explored along the flyby trajectories. Methods: We derive 4s time resolution electron densities and temperatures from MEA observations. We compare and contrast our new BepiColombo electron observations with those obtained from the Mariner 10 scanning electron spectrometer (SES) 49 yr ago. Results: A comparison to the averaged magnetospheric boundary crossings of MESSENGER indicates that the magnetosphere of Mercury was compressed during MFB1, close to its average state during MFB2, and highly compressed during MFB3. Our new MEA observations reveal the presence of a wake effect very close behind Mercury when BepiColombo entered the shadow region, a significant dusk-dawn asymmetry in electron fluxes in the nightside magnetosphere, and strongly fluctuating electrons with energies above 100s eV in the dawnside magnetosphere. Magnetospheric electron densities and temperatures are in the range of 10-30 cm-3 and above a few 100s eV in the pre-midnight-sector, and in the range of 1-100 cm-3 and well below 100 eV in the post-midnight sector, respectively. Conclusions: The MEA electron observations of different solar wind properties encountered during the first three Mercury flybys reveal the highly dynamic response and variability of the solar wind-magnetosphere interactions at Merc

Published
2024
Full Text
View/download PDF

6. Electron moments derived from the Mercury Electron Analyzer during the cruise phase of BepiColombo

Author

Rojo, M., Persson, M., Sauvaud, J. -a., Aizawa, S., Nicolaou, G., Penou, E., Barthe, A., Andre, N., Mazelle, C., Fedorov, A., Yokota, S., Saito, Y., Heyner, D., Richter, I., Auster, U., Schmid, D., Fischer, D., Horbury, T., Owen, C. J., Maksimovic, M., Khotyaintsev, Yuri V., Louarn, P., Murakami, G., Rojo, M., Persson, M., Sauvaud, J. -a., Aizawa, S., Nicolaou, G., Penou, E., Barthe, A., Andre, N., Mazelle, C., Fedorov, A., Yokota, S., Saito, Y., Heyner, D., Richter, I., Auster, U., Schmid, D., Fischer, D., Horbury, T., Owen, C. J., Maksimovic, M., Khotyaintsev, Yuri V., Louarn, P., and Murakami, G.

Abstract

Aims. We derive electron density and temperature from observations obtained by the Mercury Electron Analyzer on board Mio during the cruise phase of BepiColombo while the spacecraft is in a stacked configuration. Methods. In order to remove the secondary electron emission contribution, we first fit the core electron population of the solar wind with a Maxwellian distribution. We then subtract the resulting distribution from the complete electron spectrum, and suppress the residual count rates observed at low energies. Hence, our corrected count rates consist of the sum of the fitted Maxwellian core electron population with a contribution at higher energies. We finally estimate the electron density and temperature from the corrected count rates using a classical integration method. We illustrate the results of our derivation for two case studies, including the second Venus flyby of BepiColombo when the Solar Orbiter spacecraft was located nearby, and for a statistical study using observations obtained to date for distances to the Sun ranging from 0.3 to 0.9 AU. Results. When compared either to measurements of Solar Orbiter or to measurements obtained by HELIOS and Parker Solar Probe, our method leads to a good estimation of the electron density and temperature. Hence, despite the strong limitations arising from the stacked configuration of BepiColombo during its cruise phase, we illustrate how we can retrieve reasonable estimates for the electron density and temperature for timescales from days down to several seconds.

Published
2024
Full Text
View/download PDF

7. Improved Energy Resolution Measurements of Electron Precipitation Observed During an IPDP‐Type EMIC Event.

Author

Clilverd, M. A., Rodger, C. J., Hendry, A. T., Lozinski, A. R., Sauvaud, J.‐A., Lessard, M. R., and Raita, T.

Subjects
ELECTRONS, LOW temperature plasmas, ELECTRON density, INTERVAL analysis, ELECTROMAGNETIC interactions, ELECTRON energy loss spectroscopy
Abstract

High energy resolution DEMETER satellite observations from the Instrument for the Detection of Particle (IDP) are analyzed during an electromagnetic ion cyclotron (EMIC)‐induced electron precipitation event. Analysis of an Interval Pulsation with Diminishing Periods (IPDP)‐type EMIC wave event, using combined satellite observations to correct for incident proton contamination, detected an energy precipitation spectrum ranging from ∼150 keV to ∼1.5 MeV. While inconsistent with many theoretical predictions of >1 MeV EMIC‐induced electron precipitation, the finding is consistent with an increasing number of experimentally observed events detected using lower resolution integral channel measurements on the POES, FIREBIRD, and ELFIN satellites. Revised and improved DEMETER differential energy fluxes, after correction for incident proton contamination shows that they agree to within 40% in peak flux magnitude, and 85 keV (within 40%) for the energy at which the peak occurred as calculated from POES integral channel electron precipitation measurements. This work shows that a subset of EMIC waves found close to the plasmapause, that is, IPDP‐type rising tone events, can produce electron precipitation with peak energies substantially below 1 MeV. The rising tone features of IPDP EMIC waves, along with the association with the high cold plasma density regime, and the rapidly varying electron density gradients of the plasmapause may be an important factor in the generation of such low energy precipitation, co‐incident with a high energy tail. Our work highlights the importance of undertaking proton contamination correction when using the high‐resolution DEMETER particle measurements to investigate EMIC‐driven electron precipitation. Plain Language Summary: Energetic electrons are lost rapidly from the outer radiation belt. Several processes are thought to drive the electron losses. One process is through interactions with electromagnetic ion cyclotron (EMIC) waves. Theoretical studies suggest that electrons primarily with energy >1 MeV are lost through this process, however, previous experimental satellite observations indicate that precipitation bursts with much lower electron energies are more common. One issue is that the previous satellite observations were made with poor energy resolution and are challenging to interpret due to coincident proton precipitation, which contaminate the electron measurements. Here we use observations from the DEMETER satellite which we have corrected for proton contamination. The measurements, made with higher energy resolution than before, confirm that indeed, low energy electron precipitation can happen when EMIC waves drive electron losses. The study finds that this lower energy characteristic is likely to be driven by a small subset of rising tone EMIC waves, known as Interval Pulsation with Diminishing Periods (IPDP), typically confined to the magnetic local time evening sector. Key Points: An electromagnetic ion cyclotron wave event (an interval of pulsations with diminishing period, IPDP) was studied from Low Earth OrbitCo‐incident satellite observations detected IPDP‐induced energetic electron precipitation, starting at 150 keV, peaking at 215 keVHigh‐resolution measurements from the DEMETER satellite show enhanced fluxes from 215 keV to 1.5 MeV exhibiting a "hard" power‐law spectrum [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

8. Observation of Energetic particles between a pair of Corotating Interaction Regions

Author

Wu, Z., Chen, Y., Li, G., Zhao, L. L., Ebert, R. W., Desai, M. I., Mason, G. M., Lavraud, B., Zhao, L., Liu, Y. C. -M., Guo, F., Tang, C. L., Landi, E., and Sauvaud, J.

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

We report observations of the acceleration and trapping of energetic ions and electrons between a pair of corotating interaction regions (CIRs). The event occurred in Carrington Rotation 2060. Observed at spacecraft STEREO-B, the two CIRs were separated by less than 5 days. In contrast to other CIR events, the fluxes of energetic ions and electrons in this event reached their maxima between the trailing-edge of the first CIR and the leading edge of the second CIR. The radial magnetic field (Br) reversed its sense and the anisotropy of the flux also changed from sunward to anti-sunward between the two CIRs. Furthermore, there was an extended period of counter-streaming suprathermal electrons between the two CIRs. Similar observations for this event were also obtained for ACE and STEREO-A. We conjecture that these observations were due to a "U-shape" large scale magnetic field topology connecting the reverse shock of the first CIR and the forward shock of the second CIR. Such a disconnected U-shaped magnetic field topology may have formed due to magnetic reconnection in the upper corona.

Published
2014
Full Text
View/download PDF

9. Solar wind driven plasma fluxes from the Venus ionosphere

Author

Perez-de-Tejada, H., Lundin, R., Barabash, S., Zhang, T. L., Sauvaud, J. A., Durand-Manterola, H. J., and Reyes-Ruiz, M.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Measurements conducted with the ASPERA-4 instrument and the magnetometer of the Venus Express spacecraft show that the dynamic pressure of planetary O+ ion fluxes measured in the Venus wake can be significantly larger than the local magnetic pressure and, as a result, those ions are not being driven by magnetic forces but by the kinetic energy of the solar wind. Beams of planetary O+ ions with those properties have been detected in several orbits of the Venus Express through the wake as the spacecraft traverses by the noon-midnight plane along its near polar trajectory. The momentum flux of the O+ ions leads to superalfvenic flow conditions. It is suggested that such O+ ion beams are produced in the vicinity of the magnetic polar regions of the Venus ionosphere where the solar wind erodes the local plasma leading to plasma channels that extend downstream from those regions., Comment: 13 pages, 4 figures

Published
2012
Full Text
View/download PDF

10. Signatures of Interchange Reconnection: STEREO, ACE and Hinode Observations Combined

Author

Baker, D., Rouillard, A. P., van Driel-Gesztelyi, L., Demoulin, P., Harra, L. K., Lavraud, B., Davies, J. A., Optiz, A., Luhmann, J. G., Sauvaud, J. A., and Galvin, A. B.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Combining STEREO, ACE and Hinode observations has presented an opportunity to follow a filament eruption and coronal mass ejection (CME) on the 17th of October 2007 from an active region (AR) inside a coronal hole (CH) into the heliosphere. This particular combination of `open' and closed magnetic topologies provides an ideal scenario for interchange reconnection to take place. With Hinode and STEREO data we were able to identify the emergence time and type of structure seen in the in-situ data four days later. On the 21st, ACE observed in-situ the passage of an ICME with `open' magnetic topology. The magnetic field configuration of the source, a mature AR located inside an equatorial CH, has important implications for the solar and interplanetary signatures of the eruption. We interpret the formation of an `anemone' structure of the erupting AR and the passage in-situ of the ICME being disconnected at one leg, as manifested by uni-directional suprathermal electron flux in the ICME, to be a direct result of interchange reconnection between closed loops of the CME originating from the AR and `open' field lines of the surrounding CH., Comment: 13 pages, 13 figures, accepted Annales Geophysicae

Published
2009
Full Text
View/download PDF

11. Electron moments derived from the Mercury Electron Analyzer during the cruise phase of BepiColombo

Author

Rojo, M., primary, Persson, M., additional, Sauvaud, J.-A., additional, Aizawa, S., additional, Nicolaou, G., additional, Penou, E., additional, Barthe, A., additional, André, N., additional, Mazelle, C., additional, Fedorov, A., additional, Yokota, S., additional, Saito, Y., additional, Heyner, D., additional, Richter, I., additional, Auster, U., additional, Schmid, D., additional, Fischer, D., additional, Horbury, T., additional, Owen, C.J., additional, Maksimovic, M., additional, Khotyaintsev, Y., additional, Louarn, P., additional, and Murakami, G., additional

Published
2023
Full Text
View/download PDF

12. A Comprehensive View of the 2006 December 13 CME: From the Sun to Interplanetary Space

Author

Liu, Y., Luhmann, J. G., Müller-Mellin, R., Schroeder, P. C., Wang, L., Lin, R. P., Bale, S. D., Li, Y., Acuña, M. H., and Sauvaud, J. -A.

Subjects
Astrophysics
Abstract

The biggest halo coronal mass ejection (CME) since the Halloween storm in 2003, which occurred on 2006 December 13, is studied in terms of its solar source and heliospheric consequences. The CME is accompanied by an X3.4 flare, EUV dimmings and coronal waves. It generated significant space weather effects such as an interplanetary shock, radio bursts, major solar energetic particle (SEP) events, and a magnetic cloud (MC) detected by a fleet of spacecraft including STEREO, ACE, Wind and Ulysses. Reconstruction of the MC with the Grad-Shafranov (GS) method yields an axis orientation oblique to the flare ribbons. Observations of the SEP intensities and anisotropies show that the particles can be trapped, deflected and reaccelerated by the large-scale transient structures. The CME-driven shock is observed at both the Earth and Ulysses when they are separated by 74$^{\circ}$ in latitude and 117$^{\circ}$ in longitude, the largest shock extent ever detected. The ejecta seems missed at Ulysses. The shock arrival time at Ulysses is well predicted by an MHD model which can propagate the 1 AU data outward. The CME/shock is tracked remarkably well from the Sun all the way to Ulysses by coronagraph images, type II frequency drift, in situ measurements and the MHD model. These results reveal a technique which combines MHD propagation of the solar wind and type II emissions to predict the shock arrival time at the Earth, a significant advance for space weather forecasting especially when in situ data are available from the Solar Orbiter and Sentinels., Comment: 26 pages, 10 figures. 2008, ApJ, in press

Published
2008
Full Text
View/download PDF

13. Author Correction: The loss of ions from Venus through the plasma wake

Author

Barabash, S., Fedorov, A., Sauvaud, J. J., Lundin, R., Russell, C. T., Futaana, Y., Zhang, T. L., Andersson, H., Brinkfeldt, K., Grigoriev, A., Holmström, M., Yamauchi, M., Asamura, K., Baumjohann, W., Lammer, H., Coates, A. J., Kataria, D. O., Linder, D. R., Curtis, C. C., Hsieh, K. C., Sandel, B. R., Grande, M., Gunell, H., Koskinen, H. E. J., Kallio, E., Riihelä, P., Säles, T., Schmidt, W., Kozyra, J., Krupp, N., Fränz, M., Woch, J., Luhmann, J., McKenna-Lawlor, S., Mazelle, C., Thocaven, J.-J., Orsini, S., Cerulli-Irelli, R., Mura, A., Milillo, A., Maggi, M., Roelof, E., Brandt, P., Szego, K., Winningham, J. D., Frahm, R. A., Scherrer, J., Sharber, J. R., Wurz, P., and Bochsler, P.

Published
2022
Full Text
View/download PDF

14. Plasma Acceleration above Martian Magnetic Anomalies

Author

Lundin, R., Winningham, D., Barabash, S., Frahm, R., Holmström, M., Sauvaud, J. A., Fedorov, A., Asamura, K., Coates, A. J., Soobiah, Y., Hsieh, K. C., Grande, M., Koskinen, H., Kallio, E., Kozyra, J., Woch, J., Fraenz, M., Brain, D., Luhmann, J., McKenna-Lawler, S., Orsini, R. S., Brandt, P., and Wurz, P.

Published
2006

15. Temporal Evolution of the Solar-Wind Electron Core Density at Solar Minimum by Correlating SWEA Measurements from STEREO A and B

Author

Opitz, A., Sauvaud, J.-A., Fedorov, A., Wurz, P., Luhmann, J. G., Lavraud, B., Russell, C. T., Kellogg, P., Briand, C., Henri, P., Malaspina, D. M., Louarn, P., Curtis, D. W., Penou, E., Karrer, R., Galvin, A. B., Larson, D. E., Dandouras, I., and Schroeder, P.

Subjects
Physics, Extraterrestrial Physics, Space Sciences, Meteorology/Climatology, Astrophysics and Astroparticles
Abstract

The twin STEREO spacecraft provide a unique tool to study the temporal evolution of the solar-wind properties in the ecliptic since their longitudinal separation increases with time. We derive the characteristic temporal variations at ∼ 1 AU between two different plasma parcels ejected from the same solar source by excluding the spatial variations from our datasets. As part of the onboard IMPACT instrument suite, the SWEA electron experiment provides the solar-wind electron core density at two different heliospheric vantage points. We analyze these density datasets between March and August 2007 and find typical solar minimum conditions. After adjusting for the theoretical time lag between the two spacecraft, we compare the two density datasets. We find that their correlation decreases as the time difference increases between two ejections. The correlation coefficient is about 0.80 for a time lag of a half day and 0.65 for two days. These correlation coefficients from the electron core density are somewhat lower than the ones from the proton bulk velocity obtained in an earlier study, though they are still high enough to consider the solar wind as persistent after two days. These quantitative results reflect the variability of the solar-wind properties in space and time, and they might serve as input for solar-wind models.

Published
2010

16. A Multispacecraft Analysis of a Small-Scale Transient Entrained by Solar Wind Streams

Author

Rouillard, A. P., Savani, N. P., Davies, J. A., Lavraud, B., Forsyth, R. J., Morley, S. K., Opitz, A., Sheeley, N. R., Burlaga, L. F., Sauvaud, J.-A., Simunac, K. D., Luhmann, J. G., Galvin, A. B., Crothers, S. R., Davis, C. J., Harrison, R. A., Lockwood, M., Eyles, C. J., Bewsher, D., and Brown, D. S.

Subjects
Physics, Extraterrestrial Physics, Space Sciences, Meteorology/Climatology, Astrophysics, Sun: magnetic field, Sun: corotating interaction regions, Interplanetary medium: coronal mass ejection
Abstract

The images taken by the Heliospheric Imagers (HIs), part of the SECCHI imaging package onboard the pair of STEREO spacecraft, provide information on the radial and latitudinal evolution of the plasma compressed inside corotating interaction regions (CIRs). A plasma density wave imaged by the HI instrument onboard STEREO-B was found to propagate towards STEREO-A, enabling a comparison between simultaneous remote-sensing and in situ observations of its structure to be performed. In situ measurements made by STEREO-A show that the plasma density wave is associated with the passage of a CIR. The magnetic field compressed after the CIR stream interface (SI) is found to have a planar distribution. Minimum variance analysis of the magnetic field vectors shows that the SI is inclined at 54° to the orbital plane of the STEREO-A spacecraft. This inclination of the CIR SI is comparable to the inclination of the associated plasma density wave observed by HI. A small-scale magnetic cloud with a flux rope topology and radial extent of 0.08 AU is also embedded prior to the SI. The pitch-angle distribution of suprathermal electrons measured by the STEREO-A SWEA instrument shows that an open magnetic field topology in the cloud replaced the heliospheric current sheet locally. These observations confirm that HI observes CIRs in difference images when a small-scale transient is caught up in the compression region.

Published
2009

21. Electro Magnetic Ion Cyclotron Wave-induced Electron Precipitation: Ground-based and Satellite Observations

Author

Clilverd, M., Rodger, C., Hendry, A., Crack, M., Lozinski, A., Raita, T., Ulich, T., and Sauvaud, J.

Abstract

The study of Electro Magnetic Ion Cyclotron (EMIC) wave-induced electron precipitation has a legacy in early work suggesting EMIC waves could precipitate relativistic electrons. As such, EMIC waves represent a significant loss process for the Outer Radiation Belt, and deposit high energy electron precipitation flux deep into the atmosphere. Here we present an analysis of an example of EMIC-induced electron precipitation observed by two satellites in Low Earth Orbit, combined with EMIC wave signatures in ground-based magnetometers in Finland, and Antarctica. Electron precipitation spectral information is provided by satellite data which considers the energy range of scattered electrons during the potential EMIC wave event. We investigate the high energy resolution DEMETER IDP electron measurements in the 80keV - 2MeV range, when the detector was looking into the bounce-loss-cone, i.e., flying over the North Atlantic region.In order to assess the effect of potential proton precipitation contamination of the IDP detector we use nearby POES proton flux measurements, compensating for the IDP protective aluminium foil through a calculation of the attenuation of the proton spectrum using the integrated MULASSIS transport code. Our results are considered in the context of recent work indicating a wide energy range of non-relativistic electron precipitation is present in EMIC-induced precipitation in addition to the relativistic energy electrons suggested from the original theoretical suggestions. Our confirmation of non-relativistic energy ranges in EMIC-induced precipitation events supports the atmospheric chemical modelling analysis undertaken recently which showed that EMIC-induced precipitation is capable of causing notable composition changes., The 28th IUGG General Assembly (IUGG2023) (Berlin 2023)

Published
2023
Full Text
View/download PDF

22. Early MAVEN Deep Dip campaign reveals thermosphere and ionosphere variability

Author

Bougher, S., Jakosky, B., Halekas, J., Grebowsky, J., Luhmann, J., Mahaffy, P., Connerney, J., Eparvier, F., Ergun, R., Larson, D., McFadden, J., Mitchell, D., Schneider, N., Zurek, R., Mazelle, C., Andersson, L., Andrews, D., Baird, D., Baker, D. N., Bell, J. M., Benna, M., Brain, D., Chaffin, M., Chamberlin, P., Chaufray, J.-Y., Clarke, J., Collinson, G., Combi, M., Crary, F., Cravens, T., Crismani, M., Curry, S., Curtis, D., Deighan, J., Delory, G., Dewey, R., DiBraccio, G., Dong, C., Dong, Y., Dunn, P., Elrod, M., England, S., Eriksson, A., Espley, J., Evans, S., Fang, X., Fillingim, M., Fortier, K., Fowler, C. M., Fox, J., Gröller, H., Guzewich, S., Hara, T., Harada, Y., Holsclaw, G., Jain, S. K., Jolitz, R., Leblanc, F., Lee, C. O., Lee, Y., Lefevre, F., Lillis, R., Livi, R., Lo, D., Ma, Y., Mayyasi, M., McClintock, W., McEnulty, T., Modolo, R., Montmessin, F., Morooka, M., Nagy, A., Olsen, K., Peterson, W., Rahmati, A., Ruhunusiri, S., Russell, C. T., Sakai, S., Sauvaud, J.-A., Seki, K., Steckiewicz, M., Stevens, M., Stewart, A. I. F., Stiepen, A., Stone, S., Tenishev, V., Thiemann, E., Tolson, R., Toublanc, D., Vogt, M., Weber, T., Withers, P., Woods, T., and Yelle, R.

Published
2015

23. MAVEN observations of the response of Mars to an interplanetary coronal mass ejection

Author

Jakosky, B. M., Grebowsky, J. M., Luhmann, J. G., Connerney, J., Eparvier, F., Ergun, R., Halekas, J., Larson, D., Mahaffy, P., McFadden, J., Mitchell, D. F., Schneider, N., Zurek, R., Bougher, S., Brain, D., Ma, Y. J., Mazelle, C., Andersson, L., Andrews, D., Baird, D., Baker, D., Bell, J. M., Benna, M., Chaffin, M., Chamberlin, P., Chaufray, Y.-Y., Clarke, J., Collinson, G., Combi, M., Crary, F., Cravens, T., Crismani, M., Curry, S., Curtis, D., Deighan, J., Delory, G., Dewey, R., DiBraccio, G., Dong, C., Dong, Y., Dunn, P., Elrod, M., England, S., Eriksson, A., Espley, J., Evans, S., Fang, X., Fillingim, M., Fortier, K., Fowler, C. M., Fox, J., Gröller, H., Guzewich, S., Hara, T., Harada, Y., Holsclaw, G., Jain, S. K., Jolitz, R., Leblanc, F., Lee, C. O., Lee, Y., Lefevre, F., Lillis, R., Livi, R., Lo, D., Mayyasi, M., McClintock, W., McEnulty, T., Modolo, R., Montmessin, F., Morooka, M., Nagy, A., Olsen, K., Peterson, W., Rahmati, A., Ruhunusiri, S., Russell, C. T., Sakai, S., Sauvaud, J.-A., Seki, K., Steckiewicz, M., Stevens, M., Stewart, A. I. F., Stiepen, A., Stone, S., Tenishev, V., Thiemann, E., Tolson, R., Toublanc, D., Vogt, M., Weber, T., Withers, P., Woods, T., and Yelle, R.

Published
2015

24. Birth of a comet magnetosphere: A spring of water ions

Author

Nilsson, H., Stenberg-Wieser, G., Behar, E., Wedlund, C. S., Gunell, H., Yamauchi, M., Lundin, R., Barabash, S., Wieser, M., Carr, C., Cupido, E., Burch, J., Fedorov, A., Sauvaud, J.-A., Koskinen, H., Kallio, E., Lebreton, J.-P., Eriksson, A., Edberg, N., Goldstein, R., Henri, P., Koenders, C., Mokashi, P., Nemeth, Z., Richter, I., Szego, K., Volwerk, M., Vallat, C., and Rubin, M.

Published
2015

27. STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

Author

Luhmann, J. G., Curtis, D. W., Schroeder, P., McCauley, J., Lin, R. P., Larson, D. E., Bale, S. D., Sauvaud, J. -A., Aoustin, C., Mewaldt, R. A., Cummings, A. C., Stone, E. C., Davis, A. J., Cook, W. R., Kecman, B., Wiedenbeck, M. E., von Rosenvinge, T., Acuna, M. H., Reichenthal, L. S., Shuman, S., Wortman, K. A., Reames, D. V., Mueller-Mellin, R., Kunow, H., Mason, G. M., Walpole, P., Korth, A., Sanderson, T. R., Russell, C. T., Gosling, J. T., and Russell, C. T., editor

Published
2008
Full Text
View/download PDF

28. The Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) for the Mars Express Mission

Author

Barabash, S., Lundin, R., Andersson, H., Brinkfeldt, K., Grigoriev, A., Gunell, H., Holmström, M., Yamauchi, M., Asamura, K., Bochsler, P., Wurz, P., Cerulli-Irelli, R., Mura, A., Milillo, A., Maggi, M., Orsini, S., Coates, A. J., Linder, D. R., Kataria, D. O., Curtis, C. C., Hsieh, K. C., Sandel, B. R., Frahm, R. A., Sharber, J. R., Winningham, J. D., Grande, M., Kallio, E., Koskinen, H., Riihelä, P., Schmidt, W., Säles, T., Kozyra, J. U., Krupp, N., Woch, J., Livi, S., Luhmann, J. G., McKenna-Lawlor, S., Roelof, E. C., Williams, D. J., Sauvaud, J.-A., Fedorov, A., Thocaven, J.-J., and Russell, C. T., editor

Published
2007
Full Text
View/download PDF

29. IMF Direction Derived from Cycloid-Like Ion Distributions Observed by Mars Express

Author

Yamauchi, M., Futaana, Y., Fedorov, A., Dubinin, E., Lundin, R., Sauvaud, J.-A., Winningham, D., Frahm, R., Barabash, S., Holmstrom, M., Woch, J., Fraenz, M., Budnik, E., Borg, H., Sharber, J. R., Coates, A. J., Soobiah, Y, Koskinen, H., Kallio, E., Asamura, K., Hayakawa, H., Curtis, C., Hsieh, K. C., Sandel, B. R., Grande, M., Grigoriev, A., Wurz, P., Orsini, S., Brandt, P., Mckenna-Lawler, S., Kozyra, J., Luhmann, J., and Russell, C. T., editor

Published
2007
Full Text
View/download PDF

30. Auroral Plasma Acceleration above Martian Magnetic Anomalies

Author

Lundin, R., Winningham, D., Barabash, S., Frahm, R., Brain, D., Nilsson, H., Holmström, M., Yamauchi, M., Sharber, J. R., Sauvaud, J.-A., Fedorov, A., Asamura, K., Hayakawa, H., Coates, A. J., Soobiah, Y., Curtis, C., Hsieh, K. C., Grande, M., Koskinen, H., Kallio, E., Kozyra, J., Woch, J., Fraenz, M., Luhmann, J., Mckenna-Lawler, S., Orsini, S., Brandt, P., Wurz, P., and Russell, C. T., editor

Published
2007
Full Text
View/download PDF

31. The MAVEN Solar Wind Electron Analyzer

Author

Mitchell, D. L., Mazelle, C., Sauvaud, J.-A., Thocaven, J.-J., Rouzaud, J., Fedorov, A., Rouger, P., Toublanc, D., Taylor, E., Gordon, D., Robinson, M., Heavner, S., Turin, P., Diaz-Aguado, M., Curtis, D. W., Lin, R. P., and Jakosky, B. M.

Published
2016
Full Text
View/download PDF

32. Fast Plasma Investigation for Magnetospheric Multiscale

Author

Pollock, C., Moore, T., Jacques, A., Burch, J., Gliese, U., Saito, Y., Omoto, T., Avanov, L., Barrie, A., Coffey, V., Dorelli, J., Gershman, D., Giles, B., Rosnack, T., Salo, C., Yokota, S., Adrian, M., Aoustin, C., Auletti, C., Aung, S., Bigio, V., Cao, N., Chandler, M., Chornay, D., Christian, K., Clark, G., Collinson, G., Corris, T., De Los Santos, A., Devlin, R., Diaz, T., Dickerson, T., Dickson, C., Diekmann, A., Diggs, F., Duncan, C., Figueroa-Vinas, A., Firman, C., Freeman, M., Galassi, N., Garcia, K., Goodhart, G., Guererro, D., Hageman, J., Hanley, J., Hemminger, E., Holland, M., Hutchins, M., James, T., Jones, W., Kreisler, S., Kujawski, J., Lavu, V., Lobell, J., LeCompte, E., Lukemire, A., MacDonald, E., Mariano, A., Mukai, T., Narayanan, K., Nguyan, Q., Onizuka, M., Paterson, W., Persyn, S., Piepgrass, B., Cheney, F., Rager, A., Raghuram, T., Ramil, A., Reichenthal, L., Rodriguez, H., Rouzaud, J., Rucker, A., Saito, Y., Samara, M., Sauvaud, J.-A., Schuster, D., Shappirio, M., Shelton, K., Sher, D., Smith, D., Smith, K., Smith, S., Steinfeld, D., Szymkiewicz, R., Tanimoto, K., Taylor, J., Tucker, C., Tull, K., Uhl, A., Vloet, J., Walpole, P., Weidner, S., White, D., Winkert, G., Yeh, P.-S., and Zeuch, M.

Published
2016
Full Text
View/download PDF

33. Cluster Observes the High-Altitude Cusp Region

Author

Lavraud, B., Réme, H., Dunlop, M. W., Bosqued, J.-M., Dandouras, I., Sauvaud, J.-A., Keiling, A., Phan, T. D., Lundin, R., Cargill, P. J., Escoubet, C. P., Carlson, C. W., McFadden, J. P., Parks, G. K., Moebius, E., Kistler, L. M., Amata, E., Bavassano-Cattaneo, M.-B., Korth, A., Klecker, B., Balogh, A., Fritz, Theodore A., editor, and Fung, Shing F., editor

Published
2005
Full Text
View/download PDF

35. Magnetosheath Interaction with the high Latitude Magnetopause

Author

Savin, S., Skalsky, A., Zelenyi, L., Avanov, L., Borodkova, N., Klimov, S., Lutsenko, V., Panov, E., Romanov, S., Smirnov, V., Yermolaev, Yu., Song, P., Amata, E., Consolini, G., Fritz, T. A., Buechner, J., Nikutowski, B., Blecki, J., Farrugia, C., Maynard, N., Pickett, J., Sauvaud, J. A., Rauch, J. L., Trotignon, J. G., Khotyaintsev, Y., Stasiewicz, K., Fritz, Theodore A., editor, and Fung, Shing F., editor

Published
2005
Full Text
View/download PDF

38. The Mars Atmosphere and Volatile Evolution (MAVEN) Mission

Author

Jakosky, B. M., Lin, R. P., Grebowsky, J. M., Luhmann, J. G., Mitchell, D. F., Beutelschies, G., Priser, T., Acuna, M., Andersson, L., Baird, D., Baker, D., Bartlett, R., Benna, M., Bougher, S., Brain, D., Carson, D., Cauffman, S., Chamberlin, P., Chaufray, J.-Y., Cheatom, O., Clarke, J., Connerney, J., Cravens, T., Curtis, D., Delory, G., Demcak, S., DeWolfe, A., Eparvier, F., Ergun, R., Eriksson, A., Espley, J., Fang, X., Folta, D., Fox, J., Gomez-Rosa, C., Habenicht, S., Halekas, J., Holsclaw, G., Houghton, M., Howard, R., Jarosz, M., Jedrich, N., Johnson, M., Kasprzak, W., Kelley, M., King, T., Lankton, M., Larson, D., Leblanc, F., Lefevre, F., Lillis, R., Mahaffy, P., Mazelle, C., McClintock, W., McFadden, J., Mitchell, D. L., Montmessin, F., Morrissey, J., Peterson, W., Possel, W., Sauvaud, J.-A., Schneider, N., Sidney, W., Sparacino, S., Stewart, A. I. F., Tolson, R., Toublanc, D., Waters, C., Woods, T., Yelle, R., and Zurek, R.

Published
2015
Full Text
View/download PDF

40. Fast Plasma Investigation for Magnetospheric Multiscale

Author

Pollock, C., primary, Moore, T., additional, Jacques, A., additional, Burch, J., additional, Gliese, U., additional, Saito, Y., additional, Omoto, T., additional, Avanov, L., additional, Barrie, A., additional, Coffey, V., additional, Dorelli, J., additional, Gershman, D., additional, Giles, B., additional, Rosnack, T., additional, Salo, C., additional, Yokota, S., additional, Adrian, M., additional, Aoustin, C., additional, Auletti, C., additional, Aung, S., additional, Bigio, V., additional, Cao, N., additional, Chandler, M., additional, Chornay, D., additional, Christian, K., additional, Clark, G., additional, Collinson, G., additional, Corris, T., additional, De Los Santos, A., additional, Devlin, R., additional, Diaz, T., additional, Dickerson, T., additional, Dickson, C., additional, Diekmann, A., additional, Diggs, F., additional, Duncan, C., additional, Figueroa-Vinas, A., additional, Firman, C., additional, Freeman, M., additional, Galassi, N., additional, Garcia, K., additional, Goodhart, G., additional, Guererro, D., additional, Hageman, J., additional, Hanley, J., additional, Hemminger, E., additional, Holland, M., additional, Hutchins, M., additional, James, T., additional, Jones, W., additional, Kreisler, S., additional, Kujawski, J., additional, Lavu, V., additional, Lobell, J., additional, LeCompte, E., additional, Lukemire, A., additional, MacDonald, E., additional, Mariano, A., additional, Mukai, T., additional, Narayanan, K., additional, Nguyan, Q., additional, Onizuka, M., additional, Paterson, W., additional, Persyn, S., additional, Piepgrass, B., additional, Cheney, F., additional, Rager, A., additional, Raghuram, T., additional, Ramil, A., additional, Reichenthal, L., additional, Rodriguez, H., additional, Rouzaud, J., additional, Rucker, A., additional, Samara, M., additional, Sauvaud, J.-A., additional, Schuster, D., additional, Shappirio, M., additional, Shelton, K., additional, Sher, D., additional, Smith, D., additional, Smith, K., additional, Smith, S., additional, Steinfeld, D., additional, Szymkiewicz, R., additional, Tanimoto, K., additional, Taylor, J., additional, Tucker, C., additional, Tull, K., additional, Uhl, A., additional, Vloet, J., additional, Walpole, P., additional, Weidner, S., additional, White, D., additional, Winkert, G., additional, Yeh, P.-S., additional, and Zeuch, M., additional

Published
2016
Full Text
View/download PDF

41. Author Correction: The loss of ions from Venus through the plasma wake

Author

Barabash, S, Fedorov, A, Sauvaud, J J, Lundin, R, Russell, C T, Futaana, Y, Zhang, T L, Andersson, H, Brinkfeldt, K, Grigoriev, A, Holmström, M, Yamauchi, M, Asamura, K, Baumjohann, W, Lammer, H, Coates, A J, Kataria, D O, Linder, D R, Curtis, C C, Hsieh, K C, Sandel, B R, Grande, M, Gunell, H, Koskinen, H E J, Kallio, E, Riihelä, P, Säles, T, Schmidt, W, Kozyra, J, Krupp, N, Fränz, M, Woch, J, Luhmann, J, McKenna-Lawlor, S, Mazelle, C, Thocaven, J-J, Orsini, S, Cerulli-Irelli, R, Mura, A, Milillo, A, Maggi, M, Roelof, E, Brandt, P, Szego, K, Winningham, J D, Frahm, R A, Scherrer, J, Sharber, J R, Wurz, P, and Bochsler, P

Subjects
Multidisciplinary, 530 Physik
Published
2022

42. The Cluster Ion Spectrometry (CIS) Experiment

Author

Rème, H., Bosqued, J. M., Sauvaud, J. A., Cros, A., Dandouras, J., Aoustin, C., Bouyssou, J., Camus, Th., Cuvilo, J., Martz, C., Médale, J. L., Perrier, H., Romefort, D., Rouzaud, J., d’Uston, C., Möbius, E., Crocker, K., Granoff, M., Kistler, L. M., Popecki, M., Hovestadt, D., Klecker, B., Paschmann, G., Scholer, M., Carlson, C. W., Curtis, D. W., Lin, R. P., McFadden, J. P., Formisano, V., Amata, E., Bavassano-Cattaneo, M. B., Baldetti, P., Belluci, G., Bruno, R., Chionchio, G., Di Lellis, A., Shelley, E. G., Ghielmetti, A. G., Lennartsson, W., Korth, A., Rosenbauer, H., Lundin, R., Olsen, S., Parks, G. K., McCarthy, M., Balsiger, H., Escoubet, C. P., editor, Russell, C. T., editor, and Schmidt, R., editor

Published
1997
Full Text
View/download PDF

47. Shift of the Magnetopause Reconnection Line to the Winter Hemisphere Under Southward IMF Conditions: Geotail and MMS Observations

Author

Kitamura, N, Hasegawa, H, Saito, Y, Shinohara, I, Yokota, S, Nagai, T, Pollock, C. J, Giles, B. L, Moore, T. E, Dorelli, J. C, Gershman, D. J, Avanov, L. A, Paterson, W. R, Coffey, V. N, Chandler, M. O, Sauvaud, J. A, Lavraud, B, Torbert, R. B, Russell, C. T, Strangeway, R. J, and Burch, J. L

Subjects
Astrophysics
Abstract

At 02:13 UT on 18 November 2015 when the geomagnetic dipole was tilted by -27deg, the MMS spacecraft observed southward reconnection jets near the subsolar magnetopause under southward and dawnward interplanetary magnetic field conditions. Based on four-spacecraft estimations of the magnetic field direction near the separatrix and the motion and direction of the current sheet, the location of the reconnection line was estimated to be approx.1.8 R(sub E) or further northward of MMS. The Geotail spacecraft at GSM Z approx. 1.4 R(sub E) also observed southward reconnection jets at the dawnside magnetopause 30-40 min later. The estimated reconnection line location was northward of GSM Z approx.2 R(sub E). This crossing occurred when MMS observed purely southward magnetic fields in the magnetosheath. The simultaneous observations are thus consistent with the hypothesis that the dayside magnetopause reconnection line shifts from the subsolar point toward the northem (winter) hemisphere due to the effect of geomagnetic dipole tilt.

Published
2016
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results