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1. Characteristic scales of magnetic switchback patches near the Sun and their possible association with solar supergranulation and granulation

Author

Fargette, Naïs, Lavraud, Benoit, Rouillard, Alexis, Réville, Victor, De Wit, Thierry Dudok, Froment, Clara, Halekas, Jasper S., Phan, Tai, Malaspina, David, Bale, Stuart D., Kasper, Justin, Louarn, Philippe, Case, Anthony W., Korreck, Kelly E., Larson, Davin E., Pulupa, Marc, Stevens, Michael L., Whittlesey, Phyllis L., and Berthomier, Matthieu

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Parker Solar Probe (PSP) data recorded within a heliocentric radial distance of 0.3 AU have revealed a magnetic field dominated by Alfv\'enic structures that undergo large local variations or even reversals of the radial magnetic field. They are called magnetic switchbacks, they are consistent with folds in magnetic field lines within a same magnetic sector, and are associated with velocity spikes during an otherwise calmer background. They are thought to originate either in the low solar atmosphere through magnetic reconnection processes, or result from the evolution of turbulence or velocity shears in the expanding solar wind. In this work, we investigate the temporal and spatial characteristic scales of magnetic switchback patches. We define switchbacks as a deviation from the nominal Parker spiral direction and detect them automatically for PSP encounters 1, 2, 4 and 5. We focus in particular on a 5.1-day interval dominated by switchbacks during E5. We perform a wavelet transform of the solid angle between the magnetic field and the Parker spiral and find periodic spatial modulations with two distinct wavelengths, respectively consistent with solar granulation and supergranulation scales. In addition we find that switchback occurrence and spectral properties seem to depend on the source region of the solar wind rather than on the radial distance of PSP. These results suggest that switchbacks are formed in the low corona and modulated by the solar surface convection pattern., Comment: 12 pages, 7 figures

Published
2021
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2. Whistler instability driven by the sunward electron deficit in the solar wind

Author

Berčič, Laura, Verscharen, Daniel, Owen, Christopher J., Colomban, Lucas, Kretzschmar, Matthieu, Chust, Thomas, Maksimović, Milan, Kataria, Dhiren, Behar, Etienne, Berthomier, Matthieu, Bruno, Roberto, Fortunato, Vito, Kelly, Christopher W., Khotyaintsev, Yuri. V., Lewis, Gethyn R., Livi, Stefano, Louarn, Philippe, Mele, Gennaro, Nicolaou, Georgios, Watson, Gillian, and Wicks, Robert T.

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

Solar wind electrons play an important role in the energy balance of the solar wind acceleration by carrying energy into interplanetary space in the form of electron heat flux. The heat flux is stored in the complex electron velocity distribution functions (VDFs) shaped by expansion, Coulomb collisions, and field-particle interactions. We investigate how the suprathermal electron deficit in the anti-strahl direction, which was recently discovered in the near-Sun solar wind, drives a kinetic instability and creates whistler waves with wave vectors that are quasi-parallel to the direction of the background magnetic field. We combine high-cadence measurements of electron pitch-angle distribution functions and electromagnetic waves provided by Solar Orbiter during its first orbit. Our case study is based on a burst-mode data interval from the Electrostatic Analyser System (SWA-EAS) at a distance of 112 $R_S$ (0.52 au) from the Sun, during which several whistler wave packets were detected by Solar Orbiter's Radio and Plasma Waves (RPW) instrument. The sunward deficit creates kinetic conditions under which the quasi-parallel whistler wave is driven unstable. We directly test our predictions for the existence of these waves through solar wind observations. We find whistler waves that are quasi-parallel and almost circularly polarised, propagating away from the Sun, coinciding with a pronounced sunward deficit in the electron VDF. The cyclotron-resonance condition is fulfilled for electrons moving in the direction opposite to the direction of wave propagation, with energies corresponding to those associated with the sunward deficit.

Published
2021
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3. Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au

Author

Nair, Raaman, primary, Halekas, Jasper S., additional, Whittlesey, Phyllis L., additional, Larson, Davin E., additional, Livi, Roberto, additional, Berthomier, Matthieu, additional, Kasper, Justin C., additional, Case, Anthony W., additional, Stevens, Michael L., additional, Bale, Stuart D., additional, MacDowall, Robert J., additional, and Pulupa, Marc P., additional

Published
2022
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4. ICARUS : in-situ studies of the solar corona beyond Parker Solar Probe and Solar Orbiter

Author

Krasnoselskikh, Vladimir, Tsurutani, Bruce T., Dudok de Wit, Thierry, Walker, Simon, Balikhin, Michael, Balat-Pichelin, Marianne, Velli, Marco, Bale, Stuart D., Maksimovic, Milan, Agapitov, Oleksiy, Baumjohann, Wolfgang, Berthomier, Matthieu, Bruno, Roberto, Cranmer, Steven R., de Pontieu, Bart, Meneses, Domingos de Sousa, Eastwood, Jonathan, Erdelyi, Robertus, Ergun, Robert, Fedun, Viktor, Ganushkina, Natalia, Greco, Antonella, Harra, Louise, Henri, Pierre, Horbury, Timothy, Hudson, Hugh, Kasper, Justin, Khotyaintsev, Yuri, Kretzschmar, Matthieu, Krucker, Säm, Kucharek, Harald, Langevin, Yves, Lavraud, Benoit, Lebreton, Jean-Pierre, Lepri, Susan, Liemohn, Michael, Louarn, Philippe, Moebius, Eberhard, Mozer, Forrest, Nemecek, Zdenek, Panasenco, Olga, Retino, Alessandro, Safrankova, Jana, Scudder, Jack, Servidio, Sergio, Sorriso-Valvo, Luca, Soucek, Jan, Szabo, Adam, Vaivads, Andris, Vekstein, Grigory, Vörös, Zoltan, Zaqarashvili, Teimuraz, Zimbardo, Gaetano, Fedorov, Andrei, Krasnoselskikh, Vladimir, Tsurutani, Bruce T., Dudok de Wit, Thierry, Walker, Simon, Balikhin, Michael, Balat-Pichelin, Marianne, Velli, Marco, Bale, Stuart D., Maksimovic, Milan, Agapitov, Oleksiy, Baumjohann, Wolfgang, Berthomier, Matthieu, Bruno, Roberto, Cranmer, Steven R., de Pontieu, Bart, Meneses, Domingos de Sousa, Eastwood, Jonathan, Erdelyi, Robertus, Ergun, Robert, Fedun, Viktor, Ganushkina, Natalia, Greco, Antonella, Harra, Louise, Henri, Pierre, Horbury, Timothy, Hudson, Hugh, Kasper, Justin, Khotyaintsev, Yuri, Kretzschmar, Matthieu, Krucker, Säm, Kucharek, Harald, Langevin, Yves, Lavraud, Benoit, Lebreton, Jean-Pierre, Lepri, Susan, Liemohn, Michael, Louarn, Philippe, Moebius, Eberhard, Mozer, Forrest, Nemecek, Zdenek, Panasenco, Olga, Retino, Alessandro, Safrankova, Jana, Scudder, Jack, Servidio, Sergio, Sorriso-Valvo, Luca, Soucek, Jan, Szabo, Adam, Vaivads, Andris, Vekstein, Grigory, Vörös, Zoltan, Zaqarashvili, Teimuraz, Zimbardo, Gaetano, and Fedorov, Andrei

Abstract

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

Published
2022
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5. Characteristic Scales of Magnetic Switchback Patches Near the Sun and Their Possible Association With Solar Supergranulation and Granulation

Author

Fargette, Naïs, primary, Lavraud, Benoit, additional, Rouillard, Alexis P., additional, Réville, Victor, additional, Dudok De Wit, Thierry, additional, Froment, Clara, additional, Halekas, Jasper S., additional, Phan, Tai D., additional, Malaspina, David M., additional, Bale, Stuart D., additional, Kasper, Justin C., additional, Louarn, Philippe, additional, Case, Anthony W., additional, Korreck, Kelly E., additional, Larson, Davin E., additional, Pulupa, Marc, additional, Stevens, Michael L., additional, Whittlesey, Phyllis L., additional, and Berthomier, Matthieu, additional

Published
2021
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6. Nonlinear radiation generation processes in the auroral acceleration region

Author

Pottelette, Raymond, Berthomier, Matthieu, 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)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and 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)

Subjects
lcsh:Geophysics. Cosmic physics, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], Physics::Space Physics, lcsh:QC801-809, lcsh:Q, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], lcsh:Science, lcsh:Physics, lcsh:QC1-999
Abstract

International audience; It is known from laboratory plasma experiments that double layers (DLs) radiate in the electromagnetic spectrum; but this is only known qualitatively. In these experiments, it was shown that the electron beam created on the high-potential side of a DL generates nonlinear structures which couple to electromagnetic waves and act as a sender antenna. In the Earth auroral region, observations performed by auroral spacecraft have shown that DLs occur naturally in the source region of intense radio emissions called auroral kilometric radiation (AKR). Very high time-, spatial-, and temporal-resolution measurements are needed in order to characterize waves and particle distributions in the vicinity of DLs, which are moving transient structures. We report observations from the FAST satellite of a localized large-amplitude parallel electric field (˜ 300 mV m-1) recorded at the edges of the auroral density cavity. In agreement with laboratory experiments, on the high-potential side of the DL, elementary radiation events are detected. They occur substantially above the local electron gyrofrequency and are associated with the presence of electron holes. The velocity of these nonlinear structures can be derived from the measurement of the Doppler-shifted AKR frequency spectrum above the electron gyrofrequency. The generated electron holes appear as the nonlinear evolution of electrostatic waves generated by the electron-electron two-stream instability because they propagate at about half the beam velocity. It is pointed out that, in the vicinity of a DL, the shape of the electron distribution gives rise to a significant power recorded in the left-hand polarized ordinary (LO) mode.

Published
2017
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7. Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Belcher, John Winston, Lazarus, Alan J, Richardson, John D, Kasper, Justin C, Abiad, Robert, Austin, Gerry, Balat-Pichelin, Marianne, Bale, Stuart D, Berg, Peter, Bergner, Henry, Berthomier, Matthieu, Bookbinder, Jay, Brodu, Etienne, Caldwell, David, Case, Anthony W, Chandran, Benjamin D G, Cheimets, Peter, Cirtain, Jonathan W, Cranmer, Steven R, Curtis, David W, Daigneau, Peter, Dalton, Greg, Dasgupta, Brahmananda, DeTomaso, David, Diaz-Aguado, Millan, Djordjevic, Blagoje, Donaskowski, Bill, Effinger, Michael, Florinski, Vladimir, Fox, Nichola, Freeman, Mark, Gallagher, Dennis, Gary, S. P, Gauron, Tom, Gates, Richard, Goldstein, Melvin, Golub, Leon, Gordon, Dorothy A, Gurnee, Reid, Guth, Giora, Halekas, Jasper, Hatch, Ken, Heerikuisen, Jacob, Ho, George, Hu, Qiang, Johnson, Greg, Jordan, Steven P, Korreck, Kelly E, Larson, Davin, Li, Gang, Livi, Roberto, Ludlam, Michael, Maksimovic, Milan, McFadden, James P, Marchant, William, Maruca, Bennet A, McComas, David J, Messina, Luciana, Mercer, Tony, Park, Sang, Peddie, Andrew M, Pogorelov, Nikolai, Reinhart, Matthew J, Robinson, Miles, Rosen, Irene, Skoug, Ruth M, Slagle, Amanda, Steinberg, John T, Stevens, Michael L, Taylor, Ellen R, Tiu, Chris, Turin, Paul, Velli, Marco, Webb, Gary, Whittlesey, Phyllis, Wright, Ken, Wu, S. T, Zank, Gary, Szabo, Adam, 1965, Richardson, John D., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Belcher, John Winston, Lazarus, Alan J, Richardson, John D, Kasper, Justin C, Abiad, Robert, Austin, Gerry, Balat-Pichelin, Marianne, Bale, Stuart D, Berg, Peter, Bergner, Henry, Berthomier, Matthieu, Bookbinder, Jay, Brodu, Etienne, Caldwell, David, Case, Anthony W, Chandran, Benjamin D G, Cheimets, Peter, Cirtain, Jonathan W, Cranmer, Steven R, Curtis, David W, Daigneau, Peter, Dalton, Greg, Dasgupta, Brahmananda, DeTomaso, David, Diaz-Aguado, Millan, Djordjevic, Blagoje, Donaskowski, Bill, Effinger, Michael, Florinski, Vladimir, Fox, Nichola, Freeman, Mark, Gallagher, Dennis, Gary, S. P, Gauron, Tom, Gates, Richard, Goldstein, Melvin, Golub, Leon, Gordon, Dorothy A, Gurnee, Reid, Guth, Giora, Halekas, Jasper, Hatch, Ken, Heerikuisen, Jacob, Ho, George, Hu, Qiang, Johnson, Greg, Jordan, Steven P, Korreck, Kelly E, Larson, Davin, Li, Gang, Livi, Roberto, Ludlam, Michael, Maksimovic, Milan, McFadden, James P, Marchant, William, Maruca, Bennet A, McComas, David J, Messina, Luciana, Mercer, Tony, Park, Sang, Peddie, Andrew M, Pogorelov, Nikolai, Reinhart, Matthew J, Robinson, Miles, Rosen, Irene, Skoug, Ruth M, Slagle, Amanda, Steinberg, John T, Stevens, Michael L, Taylor, Ellen R, Tiu, Chris, Turin, Paul, Velli, Marco, Webb, Gary, Whittlesey, Phyllis, Wright, Ken, Wu, S. T, Zank, Gary, Szabo, Adam, 1965, and Richardson, John D.

Abstract

The Solar Wind Electrons Alphas and Protons (SWEAP) Investigation on Solar Probe Plus is a four sensor instrument suite that provides complete measurements of the electrons and ionized helium and hydrogen that constitute the bulk of solar wind and coronal plasma. SWEAP consists of the Solar Probe Cup (SPC) and the Solar Probe Analyzers (SPAN). SPC is a Faraday Cup that looks directly at the Sun and measures ion and electron fluxes and flow angles as a function of energy. SPAN consists of an ion and electron electrostatic analyzer (ESA) on the ram side of SPP (SPAN-A) and an electron ESA on the anti-ram side (SPAN-B). The SPAN-A ion ESA has a time of flight section that enables it to sort particles by their mass/charge ratio, permitting differentiation of ion species. SPAN-A and -B are rotated relative to one another so their broad fields of view combine like the seams on a baseball to view the entire sky except for the region obscured by the heat shield and covered by SPC. Observations by SPC and SPAN produce the combined field of view and measurement capabilities required to fulfill the science objectives of SWEAP and Solar Probe Plus. SWEAP measurements, in concert with magnetic and electric fields, energetic particles, and white light contextual imaging will enable discovery and understanding of solar wind acceleration and formation, coronal and solar wind heating, and particle acceleration in the inner heliosphere of the solar system. SPC and SPAN are managed by the SWEAP Electronics Module (SWEM), which distributes power, formats onboard data products, and serves as a single electrical interface to the spacecraft. SWEAP data products include ion and electron velocity distribution functions with high energy and angular resolution. Full resolution data are stored within the SWEM, enabling high resolution observations of structures such as shocks, reconnection events, and other transient structures to be selected for download after the fact. This paper describes t, United States. National Aeronautics and Space Administration (contract NNN06AA01C (Task NNN10AA08T))

Published
2017

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