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13 results on '"Berghmans D"'

1. Observations of fan-spine topology by Solar Orbiter/EUI: Rotational motions and indications of Alfvén waves.

Author

Petrova, E., Van Doorsselaere, T., Berghmans, D., Parenti, S., Valori, G., and Plowman, J.

Subjects
PLASMA Alfven waves, SOLAR oscillations, SOLAR corona, SOLAR atmosphere, SPECTRAL imaging
Abstract

Context. Torsional Alfvén waves do not produce any intensity variation and are therefore challenging to observe with imaging instruments. Previously, Alfvén wave observations were reported throughout all the layers of the solar atmosphere using spectral imaging. Aims. We present a torsional Alfvén wave detected in an inverted Y-shaped structure observed with the HRIEUV telescope of the EUI instrument on board Solar Orbiter in its 174 Å channel. The feature consists of two footpoints connected through short loops and a spine with a length of 30 mm originating from one of the footpoints. Methods. We made use of the simultaneous observations from two other instruments on board Solar Orbiter. The first one is the Polarimetric and Helioseismic Imager, which is used to derive the magnetic configuration of the observed feature. The second is the Spectral Imaging of the Coronal Environment (SPICE) instrument, which provided observations of intensity maps in different lines, including Ne VIII and C III lines. We also address the issues of the SPICE point spread function and its influence on the Doppler maps via performed forward-modeling analysis. Results. The difference movie constructed from the HRIEUV images shows clear signatures of propagating rotational motions in the spine. We measured propagation speeds of 136 km s−1–160 km s−1, which are consistent with the expected Alfvén speeds. Evidence of rotational motions in the transverse direction with velocities of 26 km s−1–60 km s−1 serves as an additional indication of torsional waves being present. Doppler maps obtained with SPICE show a strong signal in the spine region. Under the assumption that the recovered point spread function is mostly correct, synthesized raster images confirm that this signal is predominantly physical. Conclusions. We conclude that the presented observations are compatible with an interpretation of either propagating torsional Alfvén waves in a low coronal structure or the untwisting of a flux rope. This is the first time we have seen signatures of propagating torsional motion in the corona as observed by the three instruments on board Solar Orbiter. [ABSTRACT FROM AUTHOR]

Published
2024
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2. Temperature of quiet Sun small scale brightenings observed by EUI on board Solar Orbiter: Evidence for a cooler component.

Author

Dolliou, A., Parenti, S., Auchère, F., Bocchialini, K., Pelouze, G., Antolin, P., Berghmans, D., Harra, L., Long, D. M., Schühle, U., Kraaikamp, E., Stegen, K., Verbeeck, C., Gissot, S., Aznar Cuadrado, R., Buchlin, E., Mierla, M., Teriaca, L., and Zhukov, A. N.

Subjects
SOLAR temperature, HELIOSEISMOLOGY, LIGHT curves, SOLAR radiation, THERMAL analysis
Abstract

Context. On May 30, 2020, small and short-lived extreme-UV (EUV) brightenings in the quiet Sun were observed over a four-minute sequence by the EUV channel of the Extreme Ultraviolet Imager – High Resolution Imager (EUIHRIEUV) on board the Solar Orbiter. The brightenings' physical origin and possible impact on coronal or transition region (TR) heating are still to be determined. Aims. Our aim is to derive the statistical thermal evolution of these events in order to establish their coronal or TR origin. Methods. Our thermal analysis took advantage of the multithermal sensitivity of the Atmospheric Imaging Assembly (AIA) imager on board the Solar Dynamics Observatory. We first identified the HRIEUV events in the six coronal bands of AIA. We then performed a statistical time lag analysis that quantified the delays between the light curves from different bands, as these time lags can give significant insight into the temperature evolution of the events. The analysis was performed taking into account the possible contribution of the background and foreground emissions to the results. Results. For all nine couples of AIA bands analyzed, the brightening events are characterized by time lags inferior to the AIA cadence of 12 s. Our interpretation for these short time lags is the possible copresence of events that reach or do not reach coronal temperatures (≈1 MK). We believe that the cool population dominates the events analyzed in this work. [ABSTRACT FROM AUTHOR]

Published
2023
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5. Understanding the origins of the heliosphere: integrating observations and measurements from Parker Solar Probe, Solar Orbiter, and other space- and ground-based observatories.

Author

Velli, M., Harra, L. K., Vourlidas, A., Schwadron, N., Panasenco, O., Liewer, P. C., Müller, D., Zouganelis, I., St Cyr, O. C., Gilbert, H., Nieves-Chinchilla, T., Auchère, F., Berghmans, D., Fludra, A., Horbury, T. S., Howard, R. A., Krucker, S., Maksimovic, M., Owen, C. J., and Rodríguez-Pacheco, J.

Subjects
SOLAR wind, SOLAR energetic particles, SOLAR corona, HELIOSPHERE, SOLAR magnetic fields, MAGNETIC field measurements, OBSERVATORIES
Abstract

Context. The launch of Parker Solar Probe (PSP) in 2018, followed by Solar Orbiter (SO) in February 2020, has opened a new window in the exploration of solar magnetic activity and the origin of the heliosphere. These missions, together with other space observatories dedicated to solar observations, such as the Solar Dynamics Observatory, Hinode, IRIS, STEREO, and SOHO, with complementary in situ observations from WIND and ACE, and ground based multi-wavelength observations including the DKIST observatory that has just seen first light, promise to revolutionize our understanding of the solar atmosphere and of solar activity, from the generation and emergence of the Sun's magnetic field to the creation of the solar wind and the acceleration of solar energetic particles. Aims. Here we describe the scientific objectives of the PSP and SO missions, and highlight the potential for discovery arising from synergistic observations. Here we put particular emphasis on how the combined remote sensing and in situ observations of SO, that bracket the outer coronal and inner heliospheric observations by PSP, may provide a reconstruction of the solar wind and magnetic field expansion from the Sun out to beyond the orbit of Mercury in the first phases of the mission. In the later, out-of-ecliptic portions of the SO mission, the solar surface magnetic field measurements from SO and the multi-point white-light observations from both PSP and SO will shed light on the dynamic, intermittent solar wind escaping from helmet streamers, pseudo-streamers, and the confined coronal plasma, and on solar energetic particle transport. Methods. Joint measurements during PSP–SO alignments, and magnetic connections along the same flux tube complemented by alignments with Earth, dual PSP–Earth, and SO-Earth, as well as with STEREO-A, SOHO, and BepiColumbo will allow a better understanding of the in situ evolution of solar-wind plasma flows and the full three-dimensional distribution of the solar wind from a purely observational point of view. Spectroscopic observations of the corona, and optical and radio observations, combined with direct in situ observations of the accelerating solar wind will provide a new foundation for understanding the fundamental physical processes leading to the energy transformations from solar photospheric flows and magnetic fields into the hot coronal plasma and magnetic fields and finally into the bulk kinetic energy of the solar wind and solar energetic particles. Results. We discuss the initial PSP observations, which already provide a compelling rationale for new measurement campaigns by SO, along with ground- and space-based assets within the synergistic context described above. [ABSTRACT FROM AUTHOR]

Published
2020
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6. The Solar Orbiter EUI instrument: The Extreme Ultraviolet Imager.

Author

Rochus, P., Auchère, F., Berghmans, D., Harra, L., Schmutz, W., Schühle, U., Addison, P., Appourchaux, T., Aznar Cuadrado, R., Baker, D., Barbay, J., Bates, D., BenMoussa, A., Bergmann, M., Beurthe, C., Borgo, B., Bonte, K., Bouzit, M., Bradley, L., and Büchel, V.

Subjects
OPTICAL instruments, OPTICAL elements, SOLAR activity, ELECTRONIC systems, SOLAR atmosphere, THERMAL shielding, SOLAR chromosphere, TELEMETRY
Abstract

Context. The Extreme Ultraviolet Imager (EUI) is part of the remote sensing instrument package of the ESA/NASA Solar Orbiter mission that will explore the inner heliosphere and observe the Sun from vantage points close to the Sun and out of the ecliptic. Solar Orbiter will advance the "connection science" between solar activity and the heliosphere. Aims. With EUI we aim to improve our understanding of the structure and dynamics of the solar atmosphere, globally as well as at high resolution, and from high solar latitude perspectives. Methods. The EUI consists of three telescopes, the Full Sun Imager and two High Resolution Imagers, which are optimised to image in Lyman-α and EUV (17.4 nm, 30.4 nm) to provide a coverage from chromosphere up to corona. The EUI is designed to cope with the strong constraints imposed by the Solar Orbiter mission characteristics. Limited telemetry availability is compensated by state-of-the-art image compression, onboard image processing, and event selection. The imposed power limitations and potentially harsh radiation environment necessitate the use of novel CMOS sensors. As the unobstructed field of view of the telescopes needs to protrude through the spacecraft's heat shield, the apertures have been kept as small as possible, without compromising optical performance. This led to a systematic effort to optimise the throughput of every optical element and the reduction of noise levels in the sensor. Results. In this paper we review the design of the two elements of the EUI instrument: the Optical Bench System and the Common Electronic Box. Particular attention is also given to the onboard software, the intended operations, the ground software, and the foreseen data products. Conclusions. The EUI will bring unique science opportunities thanks to its specific design, its viewpoint, and to the planned synergies with the other Solar Orbiter instruments. In particular, we highlight science opportunities brought by the out-of-ecliptic vantage point of the solar poles, the high-resolution imaging of the high chromosphere and corona, and the connection to the outer corona as observed by coronagraphs. [ABSTRACT FROM AUTHOR]

Published
2020
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7. Models and data analysis tools for the Solar Orbiter mission.

Author

Rouillard, A. P., Pinto, R. F., Vourlidas, A., De Groof, A., Thompson, W. T., Bemporad, A., Dolei, S., Indurain, M., Buchlin, E., Sasso, C., Spadaro, D., Dalmasse, K., Hirzberger, J., Zouganelis, I., Strugarek, A., Brun, A. S., Alexandre, M., Berghmans, D., Raouafi, N. E., and Wiegelmann, T.

Subjects
SOLAR wind, DATA analysis, DATA modeling, CORONAL mass ejections, SOLAR corona, SOLAR magnetic fields, SOLAR atmosphere, HELIOSPHERE
Abstract

Context. The Solar Orbiter spacecraft will be equipped with a wide range of remote-sensing (RS) and in situ (IS) instruments to record novel and unprecedented measurements of the solar atmosphere and the inner heliosphere. To take full advantage of these new datasets, tools and techniques must be developed to ease multi-instrument and multi-spacecraft studies. In particular the currently inaccessible low solar corona below two solar radii can only be observed remotely. Furthermore techniques must be used to retrieve coronal plasma properties in time and in three dimensional (3D) space. Solar Orbiter will run complex observation campaigns that provide interesting opportunities to maximise the likelihood of linking IS data to their source region near the Sun. Several RS instruments can be directed to specific targets situated on the solar disk just days before data acquisition. To compare IS and RS, data we must improve our understanding of how heliospheric probes magnetically connect to the solar disk. Aims. The aim of the present paper is to briefly review how the current modelling of the Sun and its atmosphere can support Solar Orbiter science. We describe the results of a community-led effort by European Space Agency's Modelling and Data Analysis Working Group (MADAWG) to develop different models, tools, and techniques deemed necessary to test different theories for the physical processes that may occur in the solar plasma. The focus here is on the large scales and little is described with regards to kinetic processes. To exploit future IS and RS data fully, many techniques have been adapted to model the evolving 3D solar magneto-plasma from the solar interior to the solar wind. A particular focus in the paper is placed on techniques that can estimate how Solar Orbiter will connect magnetically through the complex coronal magnetic fields to various photospheric and coronal features in support of spacecraft operations and future scientific studies. Methods. Recent missions such as STEREO, provided great opportunities for RS, IS, and multi-spacecraft studies. We summarise the achievements and highlight the challenges faced during these investigations, many of which motivated the Solar Orbiter mission. We present the new tools and techniques developed by the MADAWG to support the science operations and the analysis of the data from the many instruments on Solar Orbiter. Results. This article reviews current modelling and tool developments that ease the comparison of model results with RS and IS data made available by current and upcoming missions. It also describes the modelling strategy to support the science operations and subsequent exploitation of Solar Orbiter data in order to maximise the scientific output of the mission. Conclusions. The on-going community effort presented in this paper has provided new models and tools necessary to support mission operations as well as the science exploitation of the Solar Orbiter data. The tools and techniques will no doubt evolve significantly as we refine our procedure and methodology during the first year of operations of this highly promising mission. [ABSTRACT FROM AUTHOR]

Published
2020
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8. LYRA OBSERVATIONS OF TWO OSCILLATION MODES IN A SINGLE FLARE.

Author

VAN DOORSSELAERE, T., DE GROOF, A., ZENDER, J., BERGHMANS, D., and GOOSSENS, M.

Subjects
SOLAR flares, SOLAR oscillations, LIGHT curves, CORONAL holes, SPECTRAL irradiance
Abstract

We analyze light curves from the LYRA irradiance experiment on board PROBA2 during the flare of 2010 February 8. We see both long- and short-period oscillations during the flare. The long-period oscillation is interpreted in terms of standing slow sausage modes; the short-period oscillation is thought to be a standing fast sausage mode. The simultaneous presence of two oscillation modes in the same flaring structure allows for new coronal seismological applications. The periods are used to find seismological estimates of the plasma-β and the density contrast of the flaring loop. Also the wave mode number is estimated from the observed periods. [ABSTRACT FROM AUTHOR]

Published
2011
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9. SWAP onboard PROBA 2, a new EUV imager for solar monitoring

Author

Berghmans, D., Hochedez, J.F., Defise, J.M., Lecat, J.H., Nicula, B., Slemzin, V., Lawrence, G., Katsyiannis, A.C., der Linden, R. Van, Zhukov, A., Clette, F., Rochus, P., Mazy, E., Thibert, T., Nicolosi, P., Pelizzo, M-G., and Schühle, U.

Subjects
*SUN observations, *SOLAR flares, *CORONAL mass ejections, *SPACE environment
Abstract

Abstract: SWAP (Sun Watcher using Active Pixel system detector and image processing) is a solar imager in the extreme ultraviolet (EUV) that has been selected to fly in 2007 on the PROBA 2 technological platform, an ESA program. SWAP will use an off-axis Ritchey Chrétien telescope equipped with an EUV enhanced active pixel sensor detector (coated APS). This type of detector has advantages that promise to be very profitable for solar EUV imaging. SWAP will provide solar coronal images at a 1-min cadence in a bandpass centered on 17.5nm. Observations with this specific wavelength allow detecting phenomena, such as solar flares or EIT-waves, associated with the early phase of coronal mass ejections. Image processing software will be developed that automatically detects these phenomena and sends out space weather warnings. Together with its sister instrument LYRA, also onboard PROBA 2, SWAP will serve as a high performance solar monitoring tool to be used in operational space weather forecasting. The SWAP data will complement the solar observations provided by instruments like SOHO-EIT, and STEREO-SECCHI. [Copyright &y& Elsevier]

Published
2006
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10. Objective CME detection over the solar cycle: A first attempt

Author

Robbrecht, E., Berghmans, D., and Van der Linden, R.A.M.

Subjects
*SOLAR corona, *IMAGE processing, *INFORMATION processing, *INTEGRATED software
Abstract

Abstract: We recently developed a software package to autonomously detect coronal mass ejections (CMEs) in image sequences from large angle spectrometric coronagraph (LASCO). The detection is not done in the original images, instead we detect bright ridges in (time, height) plots using a modified version of the Hough transform. Experimental results on real-time data have shown that the developed technique can achieve excellent results in measuring starting time and principal angle and good results for the angular width and velocity measurement compared to the CMEs listed in the manually assembled catalog. The real-time output of the software can be found online at www.sidc.oma.be/cactus. With the present paper, we report on the first large scale application of the software to the LASCO archive. In an ongoing work, we have applied the software on a first sample of 29 months selected from archive data in the period July 1997 to December 2002. The results in this paper show that relevant characteristics of CMEs over the solar cycle are successfully recovered with the automated procedure. This proves that a completely automatically produced CME catalog is within reach. [Copyright &y& Elsevier]

Published
2006
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11. LUCI onboard Lagrange, the next generation of EUV space weather monitoring

Author

West Matthew J., Kintziger Christian, Haberreiter Margit, Gyo Manfred, Berghmans David, Gissot Samuel, Büchel Valeria, Golub Leon, Shestov Sergei, and Davies Jackie A.

Subjects
instrumentation: detectors, space vehicles: instruments, telescopes, sun: corona, sun: uv radiation, Meteorology. Climatology, QC851-999
Abstract

Lagrange eUv Coronal Imager (LUCI) is a solar imager in the Extreme UltraViolet (EUV) that is being developed as part of the Lagrange mission, a mission designed to be positioned at the L5 Lagrangian point to monitor space weather from its source on the Sun, through the heliosphere, to the Earth. LUCI will use an off-axis two mirror design equipped with an EUV enhanced active pixel sensor. This type of detector has advantages that promise to be very beneficial for monitoring the source of space weather in the EUV. LUCI will also have a novel off-axis wide field-of-view, designed to observe the solar disk, the lower corona, and the extended solar atmosphere close to the Sun–Earth line. LUCI will provide solar coronal images at a 2–3 min cadence in a pass-band centred on 19.5. Observations made through this pass-band allow for the detection and monitoring of semi-static coronal structures such as coronal holes, prominences, and active regions; as well as transient phenomena such as solar flares, limb coronal mass ejections (CMEs), EUV waves, and coronal dimmings. The LUCI data will complement EUV solar observations provided by instruments located along the Sun–Earth line such as PROBA2-SWAP, SUVI-GOES and SDO-AIA, as well as provide unique observations to improve space weather forecasts. Together with a suite of other remote-sensing and in-situ instruments onboard Lagrange, LUCI will provide science quality operational observations for space weather monitoring.

Published
2020
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12. The first coronal mass ejection observed in both visible-light and UV HI Ly-α channels of the Metis coronagraph on board Solar Orbiter

Author

V. Andretta, A. Bemporad, Y. De Leo, G. Jerse, F. Landini, M. Mierla, G. Naletto, M. Romoli, C. Sasso, A. Slemer, D. Spadaro, R. Susino, D.-C. Talpeanu, D. Telloni, L. Teriaca, M. Uslenghi, E. Antonucci, F. Auchère, D. Berghmans, A. Berlicki, G. Capobianco, G. E. Capuano, C. Casini, M. Casti, P. Chioetto, V. Da Deppo, M. Fabi, S. Fineschi, F. Frassati, F. Frassetto, S. Giordano, C. Grimani, P. Heinzel, A. Liberatore, E. Magli, G. Massone, M. Messerotti, D. Moses, G. Nicolini, M. Pancrazzi, M.-G. Pelizzo, P. Romano, U. Schühle, M. Stangalini, Th. Straus, C. A. Volpicelli, L. Zangrilli, P. Zuppella, L. Abbo, R. Aznar Cuadrado, R. Bruno, A. Ciaravella, R. D’Amicis, P. Lamy, A. Lanzafame, A. M. Malvezzi, P. Nicolosi, G. Nisticò, H. Peter, C. Plainaki, L. Poletto, F. Reale, S. K. Solanki, L. Strachan, G. Tondello, K. Tsinganos, M. Velli, R. Ventura, J.-C. Vial, J. Woch, G. Zimbardo, Andretta V., Bemporad A., De Leo Y., Jerse G., Landini F., Mierla M., Naletto G., Romoli M., Sasso C., Slemer A., Spadaro D., Susino R., Talpeanu D.-C., Telloni D., Teriaca L., Uslenghi M., Antonucci E., Auchere F., Berghmans D., Berlicki A., Capobianco G., Capuano G.E., Casini C., Casti M., Chioetto P., Da Deppo V., Fabi M., Fineschi S., Frassati F., Frassetto F., Giordano S., Grimani C., Heinzel P., Liberatore A., Magli E., Massone G., Messerotti M., Moses D., Nicolini G., Pancrazzi M., Pelizzo M.-G., Romano P., Schuhle U., Stangalini M., Straus T., Volpicelli C.A., Zangrilli L., Zuppella P., Abbo L., Aznar Cuadrado R., Bruno R., Ciaravella A., D'amicis R., Lamy P., Lanzafame A., Malvezzi A.M., Nicolosi P., Nistico G., Peter H., Plainaki C., Poletto L., Reale F., Solanki S.K., Strachan L., Tondello G., Tsinganos K., Velli M., Ventura R., Vial J.-C., Woch J., Zimbardo G., INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Torino (OATo), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Dipartamento di Fisica e Astronomia 'Ettore Majorana', Università degli studi di Catania [Catania], INAF - Osservatorio Astronomico di Trieste (OAT), Royal Observatory of Belgium [Brussels] (ROB), Institute of Geodynamics of the Romanian Academy, Romanian Academy, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), Dipartimento di Fisica e Astronomia [Firenze], Università degli Studi di Firenze = University of Florence [Firenze] (UNIFI), INAF - Osservatorio Astrofisico di Catania (OACT), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute [Wroclaw], University of Wrocław [Poland] (UWr), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Dipartimento di Scienze Pure et Applicate (DiSPea), Università degli Studi di Urbino 'Carlo Bo', Istituto Nazionale di Fisica Nucleare, Sezione di Firenze (INFN, Sezione di Firenze), Istituto Nazionale di Fisica Nucleare (INFN), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Università degli studi di Torino (UNITO), Dipartimento di Elettronica e Telecomunicazioni [Torino] (DET), Politecnico di Torino = Polytechnic of Turin (Polito), NASA Headquarters, Istituto di Elettronica e di Ingegneria dell'Informazione e delle Telecomunicazioni (IEIIT), Consiglio Nazionale delle Ricerche (CNR), Agenzia Spaziale Italiana (ASI), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), INAF - Osservatorio Astronomico di Palermo (OAPa), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Università di Pavia, Dipartimento di Fisica [Arcavacata di Rende], Università della Calabria [Arcavacata di Rende] (Unical), Dipartimento di Fisica e Chimica 'Emilio Segrè' (DiFC), Università degli studi di Palermo - University of Palermo, Naval Research Laboratory (NRL), Department of Physics [Athens], National and Kapodistrian University of Athens (NKUA), University of California [Los Angeles] (UCLA), and University of California

Subjects
Physics, 010504 meteorology & atmospheric sciences, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Sun: corona, Sun: coronal mass ejections (CMEs), Astronomy and Astrophysics, Astrophysics, Alpha (navigation), Sun: UV radiation, 01 natural sciences, law.invention, On board, Orbiter, Space and Planetary Science, law, 0103 physical sciences, Coronal mass ejection, Metis, 010303 astronomy & astrophysics, Coronagraph, Sun: atmosphere, 0105 earth and related environmental sciences, Visible spectrum, Sun: atmosphere – Sun: corona – Sun: UV radiation – Sun: coronal mass ejections (CMEs)
Abstract

Context.The Metis coronagraph on board Solar Orbiter offers a new view of coronal mass ejections (CMEs), observing them for the first time with simultaneous images acquired with a broad-band filter in the visible-light interval and with a narrow-band filter around the H ILy-αline at 121.567 nm, the so-called Metis UV channel.Aims.We show the first Metis observations of a CME, obtained on 16 and 17 January 2021. The event was also observed by the EUI/FSI imager on board Solar Orbiter, as well as by other space-based coronagraphs, such as STEREO-A/COR2 and SOHO/LASCO/C2, whose images are combined here with Metis data.Methods.Different images are analysed here to reconstruct the 3D orientation of the expanding CME flux rope using the graduated cylindrical shell model. This also allows us to identify the possible location of the source region. Measurements of the CME kinematics allow us to quantify the expected Doppler dimming in the Ly-αchannel.Results.Observations show that most CME features seen in the visible-light images are also seen in the Ly-αimages, although some features in the latter channel appear more structured than their visible-light counterparts. We estimated the expansion velocity of this event to be below 140 km s−1. Hence, these observations can be understood by assuming that Doppler dimming effects do not strongly reduce the Ly-αemission from the CME. These velocities are comparable with or smaller than the radial velocities inferred from the same data in a similar coronal structure on the east side of the Sun.Conclusions.The first observations by Metis of a CME demonstrate the capability of the instrument to provide valuable and novel information on the structure and dynamics of these coronal events. Considering also its diagnostics capabilities regarding the conditions of the ambient corona, Metis promises to significantly advance our knowledge of such phenomena.

Published
2021
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13. Models and data analysis tools for the Solar Orbiter mission

Author

Kamen Kozarev, Hardi Peter, X. Bonnin, Manolis K. Georgoulis, Alexis P. Rouillard, Daniele Spadaro, A. De Groof, Angels Aran, Raul Gomez-Herrero, M. Bouchemit, Alessandro Bemporad, R. A. Howard, A. S. Brun, F. Espinosa Lara, E. Budnik, S. I. Jones, N. E. Raouafi, Rita Ventura, J. C. del Toro Iniesta, David Pérez-Suárez, Silvano Fineschi, Miho Janvier, Jon A. Linker, Thomas Wiegelmann, Teresa Nieves-Chinchilla, Timothy S. Horbury, L. R. Bellot Rubio, A. Giunta, Nicolas Poirier, Bogdan Nicula, Andreas Lagg, Kévin Dalmasse, Jim M. Raines, Michael Lavarra, Carl J. Henney, Holly Gilbert, S. Parenti, D. Orozco Suárez, Mikel Indurain, David R. Williams, David Berghmans, L. Etesi, Andrzej Fludra, F. Auchère, Daniel Müller, Vincent Génot, Y. Wu, Jens Pomoell, Marco Romoli, N. Rich, A. Kouloumvakos, S. Caminade, Benoit Lavraud, Antoine Strugarek, G. Mann, Philippe Louarn, Arnaud Masson, J. Carlyle, L. Sanchez, I. Zouganelis, Baptiste Cecconi, Eric Buchlin, Javier Rodriguez-Pacheco, T. Amari, M. Haberreiter, Thomas Straus, C. Watson, Alexander Warmuth, Johann Hirzberger, Säm Krucker, Athanasios Papaioannou, Tino L. Riethmüller, Pedro Osuna, Cis Verbeeck, Shane A. Maloney, William T. Thompson, Luciano Rodriguez, Sami K. Solanki, H. Önel, Paolo Pagano, I. Cernuda, Andrei Fedorov, Luca Teriaca, E. Kraaikamp, Nicole Vilmer, Rui F. Pinto, S. Dolei, Simon Plunkett, Roberto Susino, Etienne Pariat, Andrew Walsh, Clementina Sasso, Vincenzo Andretta, Christopher J. Owen, Donald M. Hassler, S. Guest, O. C. St. Cyr, Anastasios Anastasiadis, Ester Antonucci, Angelos Vourlidas, Andrei Zhukov, Milan Maksimovic, C. N. Arge, Matthieu Alexandre, Joseph M. Davila, Centre de Physique Théorique [Palaiseau] (CPHT), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Space Physics Research Group, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Naval Research Laboratory (NRL), European Space Astronomy Centre (ESAC), European Space Agency (ESA), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Catania (OACT), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), National Center for Atmospheric Research [Boulder] (NCAR), Laboratoire de Physique des Plasmas (LPP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche sur la Fusion par confinement Magnétique (IRFM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Stéréochimie et Interactions Moléculaires (STIM), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Centre de Recherche en Transplantation et Immunologie (U1064 Inserm - CRTI), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), INAF - Osservatorio Astronomico di Capodimonte (OAC), Institut Jacques Monod (IJM (UMR_7592)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Solar-Terrestrial Centre of Excellence [Brussels] (STCE), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), NOVELTIS [Sté], Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], NASA Goddard Space Flight Center (GSFC), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Blackett Laboratory, Imperial College London, EADS Astrium SAS, Science Applications International Corporation (SAIC), Space Science and Applications, Los Alamos National Laboratory (LANL), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Trinity College Dublin, Leibniz-Institut für Astrophysik Potsdam (AIP), Laboratoire Francis PERRIN (LFP - URA 2453), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut d'Electronique du Solide et des Systèmes (InESS), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Centro de Investigacion Cientifica y de Education Superior de Ensenada [Mexico] (CICESE), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Ecosystèmes et paysages montagnards (UR EPGR), Centre national du machinisme agricole, du génie rural, des eaux et forêts (CEMAGREF), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (INFN, Sezione di Napoli), Istituto Nazionale di Fisica Nucleare (INFN), Max Planck Institute for Solar System Research (MPS), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Microbiology Department, St. Jame's Hospital, European Research Council, European Commission, Science and Technology Facilities Council (UK), Durham University, Centre National D'Etudes Spatiales (France), Helmholtz Association, German Centre for Air and Space Travel, Ministerio de Ciencia, Innovación y Universidades (España), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), ANR-17-CE31-0006,COROSHOCK,EVALUER LE ROLE DU CHOC COMME ACCELERATEUR DE PARTICULES SOLAIRES(2017), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Rouillard A.P., Pinto R.F., Vourlidas A., De Groof A., Thompson W.T., Bemporad A., Dolei S., Indurain M., Buchlin E., Sasso C., Spadaro D., Dalmasse K., Hirzberger J., Zouganelis I., Strugarek A., Brun A.S., Alexandre M., Berghmans D., Raouafi N.E., Wiegelmann T., Pagano P., Arge C.N., Nieves-Chinchilla T., Lavarra M., Poirier N., Amari T., Aran A., Andretta V., Antonucci E., Anastasiadis A., Auchere F., Bellot Rubio L., Nicula B., Bonnin X., Bouchemit M., Budnik E., Caminade S., Cecconi B., Carlyle J., Cernuda I., Davila J.M., Etesi L., Espinosa Lara F., Fedorov A., Fineschi S., Fludra A., Genot V., Georgoulis M.K., Gilbert H.R., Giunta A., Gomez-Herrero R., Guest S., Haberreiter M., Hassler D., Henney C.J., Howard R.A., Horbury T.S., Janvier M., Jones S.I., Kozarev K., Kraaikamp E., Kouloumvakos A., Krucker S., Lagg A., Linker J., Lavraud B., Louarn P., Maksimovic M., Maloney S., Mann G., Masson A., Muller D., Onel H., Osuna P., Orozco Suarez D., Owen C.J., Papaioannou A., Perez-Suarez D., Rodriguez-Pacheco J., Parenti S., Pariat E., Peter H., Plunkett S., Pomoell J., Raines J.M., Riethmuller T.L., Rich N., Rodriguez L., Romoli M., Sanchez L., Solanki S.K., St Cyr O.C., Straus T., Susino R., Teriaca L., Del Toro Iniesta J.C., Ventura R., Verbeeck C., Vilmer N., Warmuth A., Walsh A.P., Watson C., Williams D., Wu Y., Zhukov A.N., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), vilmer, nicole, and University of St Andrews. Applied Mathematics

Subjects
010504 meteorology & atmospheric sciences, corona [Sun], Solar wind, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 7. Clean energy, 01 natural sciences, law.invention, Data acquisition, law, Coronal mass ejection, general [Sun], QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Sun: magnetic fields, QC, ComputingMilieux_MISCELLANEOUS, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 3rd-DAS, energetic particles, CORONAL MASS EJECTIONS, numerical modeling, magnetic fields [Sun], solar wind, Physics::Space Physics, Systems engineering, Astrophysics::Earth and Planetary Astrophysics, atmosphere [Sun], fundamental parameters [Sun], Sun: general, FORCE-FREE FIELD, Sun: fundamental parameters, Solar radius, Context (language use), STREAMER STRUCTURE, Orbiter, 0103 physical sciences, OPTIMIZATION APPROACH, [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], POLARIZATION MEASUREMENTS, Sun: Solar wind, 3-DIMENSIONAL STRUCTURE, 0105 earth and related environmental sciences, Spacecraft, business.industry, Sun: corona, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], solar corona, MAGNETIC-FLUX ROPES, Astronomy and Astrophysics, SHOCKS DRIVEN, 115 Astronomy, Space science, SPECTRAL-LINES, QC Physics, 13. Climate action, Space and Planetary Science, business, Heliosphere, Sun: atmosphere, ELECTRON-DENSITY
Abstract

All authors: Rouillard, A. P.; Pinto, R. F.; Vourlidas, A.; De Groof, A.; Thompson, W. T.; Bemporad, A.; Dolei, S.; Indurain, M.; Buchlin, E.; Sasso, C.; Spadaro, D.; Dalmasse, K.; Hirzberger, J.; Zouganelis, I.; Strugarek, A.; Brun, A. S.; Alexandre, M.; Berghmans, D.; Raouafi, N. E.; Wiegelmann, T.; Pagano, P.; Arge, C. N.; Nieves-Chinchilla, T.; Lavarra, M.; Poirier, N.; Amari, T.; Aran, A.; Andretta, V.; Antonucci, E.; Anastasiadis, A.; Auchère, F.; Bellot Rubio, L.; Nicula, B.; Bonnin, X.; Bouchemit, M.; Budnik, E.; Caminade, S.; Cecconi, B.; Carlyle, J.; Cernuda, I.; Davila, J. M.; Etesi, L.; Espinosa Lara, F.; Fedorov, A.; Fineschi, S.; Fludra, A.; Génot, V.; Georgoulis, M. K.; Gilbert, H. R.; Giunta, A.; Gomez-Herrero, R.; Guest, S.; Haberreiter, M.; Hassler, D.; Henney, C. J.; Howard, R. A.; Horbury, T. S.; Janvier, M.; Jones, S. I.; Kozarev, K.; Kraaikamp, E.; Kouloumvakos, A.; Krucker, S.; Lagg, A.; Linker, J.; Lavraud, B.; Louarn, P.; Maksimovic, M.; Maloney, S.; Mann, G.; Masson, A.; Müller, D.; Önel, H.; Osuna, P.; Orozco Suarez, D.; Owen, C. J.; Papaioannou, A.; Pérez-Suárez, D.; Rodriguez-Pacheco, J.; Parenti, S.; Pariat, E.; Peter, H.; Plunkett, S.; Pomoell, J.; Raines, J. M.; Riethmüller, T. L.; Rich, N.; Rodriguez, L.; Romoli, M.; Sanchez, L.; Solanki, S. K.; St Cyr, O. C.; Straus, T.; Susino, R.; Teriaca, L.; del Toro Iniesta, J. C.; Ventura, R.; Verbeeck, C.; Vilmer, N.; Warmuth, A.; Walsh, A. P.; Watson, C.; Williams, D.; Wu, Y.; Zhukov, A. N.-- Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. The Solar Orbiter spacecraft will be equipped with a wide range of remote-sensing (RS) and in situ (IS) instruments to record novel and unprecedented measurements of the solar atmosphere and the inner heliosphere. To take full advantage of these new datasets, tools and techniques must be developed to ease multi-instrument and multi-spacecraft studies. In particular the currently inaccessible low solar corona below two solar radii can only be observed remotely. Furthermore techniques must be used to retrieve coronal plasma properties in time and in three dimensional (3D) space. Solar Orbiter will run complex observation campaigns that provide interesting opportunities to maximise the likelihood of linking IS data to their source region near the Sun. Several RS instruments can be directed to specific targets situated on the solar disk just days before data acquisition. To compare IS and RS, data we must improve our understanding of how heliospheric probes magnetically connect to the solar disk. Aims. The aim of the present paper is to briefly review how the current modelling of the Sun and its atmosphere can support Solar Orbiter science. We describe the results of a community-led effort by European Space Agency's Modelling and Data Analysis Working Group (MADAWG) to develop different models, tools, and techniques deemed necessary to test different theories for the physical processes that may occur in the solar plasma. The focus here is on the large scales and little is described with regards to kinetic processes. To exploit future IS and RS data fully, many techniques have been adapted to model the evolving 3D solar magneto-plasma from the solar interior to the solar wind. A particular focus in the paper is placed on techniques that can estimate how Solar Orbiter will connect magnetically through the complex coronal magnetic fields to various photospheric and coronal features in support of spacecraft operations and future scientific studies. Methods. Recent missions such as STEREO, provided great opportunities for RS, IS, and multi-spacecraft studies. We summarise the achievements and highlight the challenges faced during these investigations, many of which motivated the Solar Orbiter mission. We present the new tools and techniques developed by the MADAWG to support the science operations and the analysis of the data from the many instruments on Solar Orbiter. Results. This article reviews current modelling and tool developments that ease the comparison of model results with RS and IS data made available by current and upcoming missions. It also describes the modelling strategy to support the science operations and subsequent exploitation of Solar Orbiter data in order to maximise the scientific output of the mission. Conclusions. The on-going community effort presented in this paper has provided new models and tools necessary to support mission operations as well as the science exploitation of the Solar Orbiter data. The tools and techniques will no doubt evolve significantly as we refine our procedure and methodology during the first year of operations of this highly promising mission. © 2020 A. P. Rouillard et al., Solar Orbiter is a joint ESA and NASA mission. A. Vourlidas' Solar Orbiter effort is supported by NRL grant N00173-16-1-G029. P. Pagano would like to thank D. H. Mackay and S. L. Yardley for their valuable contributions, the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 647214), and the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (http://www.dirac.ac.uk).This equipment was funded by a BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/K00087X/1, DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. A. Rouillard, V. Genot, M. Janvier, Elie Soubrier, F. Auchere, E. Buchlin and E. Pariat acknowledge support from the French space agency (Centre National d'Etudes Spatiales; CNES; https://cnes.fr/fr) that funds activity in plasma physics data center (Centre de Donnees de la Physique des Plasmas; CDPP; http://cdpp.eu/) and the Multi Experiment Data and Operation Center (MEDOC; https://idoc.ias.u-psud.fr/MEDOC), and the space weather team in Toulouse (Solar-Terrestrial Observations and Modelling Service; STORMS; http://storms-service.irap.omp.eu/).This includes funding for Gaia-DEM, the data mining tools AMDA (http://amda.cdpp.eu/), CLWEB (clweb.cesr. fr/) and the propagation tool (http://propagationtool.cdpp.eu).R.Pinto, M. Lavarra, Y. Wu and A. Kouloumvakos acknowledge financial support from the ANR project SLOW_ SOURCE No. ANR-17-CE31-0006-01, ANR project COROSHOCK No. ANR-18-ERC1-0006-01 and FP7 HELCATS project https://www.helcats-fp7.eu/under the FP7 EU contract number 606692. A. Warmuth acknowledges the support by DLR under grant No. 50 QL 0001. The STEREO SECCHI data are produced by a consortium of RAL (UK), NRL (USA), LMSAL (USA), GSFC (USA), MPS (Germany), CSL (Belgium), IOTA (France) and IAS (France). The ACE data were obtained from the ACE science center. The WIND data were obtained from the Space Physics Data Facility. Javier Rodriguez-Pacheco acknowledges Spanish Project: FEDER/MCIU-AEI/Project ESP2017-88436-R.

Published
2020
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