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16 results on '"Nenon, Q."'

1. Properties of electrons accelerated by the Ganymede-magnetosphere interaction: survey of Juno high-latitude observations

Author

Rabia, J., Hue, V., Andre, N., Nenon, Q., Szalay, J. R., Allegrini, F., Sulaiman, A. H., Louis, C. K., Greathouse, T. K., Sarkango, Y., Santos-Costa, D., Blanc, M., Penou, E., Louarn, P., Ebert, R. W., Gladstone, G. R., Mura, A., Connerney, J. E. P., and Bolton, S. J.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The encounter between the Jovian co-rotating plasma and Ganymede gives rise to electromagnetic waves that propagate along the magnetic field lines and accelerate particles by resonant or non-resonant wave-particle interaction. They ultimately precipitate into Jupiter's atmosphere and trigger auroral emissions. In this study, we use Juno/JADE, Juno/UVS data, and magnetic field line tracing to characterize the properties of electrons accelerated by the Ganymede-magnetosphere interaction in the far-field region. We show that the precipitating energy flux exhibits an exponential decay as a function of downtail distance from the moon, with an e-folding value of 29{\deg}, consistent with previous UV observations from the Hubble Space Telescope (HST). We characterize the electron energy distributions and show that two distributions exist. Electrons creating the Main Alfv\'en Wing (MAW) spot and the auroral tail always have broadband distribution and a mean characteristic energy of 2.2 keV while in the region connected to the Transhemispheric Electron Beam (TEB) spot the electrons are distributed non-monotonically, with a higher characteristic energy above 10 keV. Based on the observation of bidirectional electron beams, we suggest that Juno was located within the acceleration region during the 11 observations reported. We thus estimate that the acceleration region is extended, at least, between an altitude of 0.5 and 1.3 Jupiter radius above the 1-bar surface. Finally, we estimate the size of the interaction region in the Ganymede orbital plane using far-field measurements. These observations provide important insights for the study of particle acceleration processes involved in moon-magnetosphere interactions., Comment: Accepted for publication in JGR: Space Physics

Published
2024

2. Exploring Fundamental Particle Acceleration and Loss Processes in Heliophysics through an Orbiting X-ray Instrument in the Jovian System

Author

Dunn, W., Berland, G., Roussos, E., Clark, G., Kollmann, P., Turner, D., Feldman, C., Stallard, T., Branduardi-Raymont, G., Woodfield, E. E., Rae, I. J., Ray, L. C., Carter, J. A., Lindsay, S. T., Yao, Z., Marshall, R., A., A. N. Jaynes, Ezoe, Y., Numazawa, M., Hospodarsky, G. B., Wu, X., Weigt, D. M., Jackman, C. M., Mori, K., Nénon, Q., Desai, R. T, Blum, L. W., Nordheim, T. A., Ness, J. U., Bodewits, D., Kimura, T., Li, W., Smith, H. T., Millas, D., Wibisono, A. D., Achilleos, N., Koutroumpa, D., McEntee, S. C., Collier, H., Bhardwaj, A., Martindale, A., Wolk, S. J., Badman, S. V., and Kraft, R. P.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Physics - Space Physics
Abstract

Jupiter's magnetosphere is considered to be the most powerful particle accelerator in the Solar System, accelerating electrons from eV to 70 MeV and ions to GeV energies. How electromagnetic processes drive energy and particle flows, producing and removing energetic particles, is at the heart of Heliophysics. Particularly, the 2013 Decadal Strategy for Solar and Space Physics was to "Discover and characterize fundamental processes that occur both within the heliosphere and throughout the universe". The Jovian system offers an ideal natural laboratory to investigate all of the universal processes highlighted in the previous Decadal. The X-ray waveband has been widely used to remotely study plasma across astrophysical systems. The majority of astrophysical emissions can be grouped into 5 X-ray processes: fluorescence, thermal/coronal, scattering, charge exchange and particle acceleration. The Jovian system offers perhaps the only system that presents a rich catalog of all of these X-ray emission processes and can also be visited in-situ, affording the special possibility to directly link fundamental plasma processes with their resulting X-ray signatures. This offers invaluable ground-truths for astrophysical objects beyond the reach of in-situ exploration (e.g. brown dwarfs, magnetars or galaxy clusters that map the cosmos). Here, we show how coupling in-situ measurements with in-orbit X-ray observations of Jupiter's radiation belts, Galilean satellites, Io Torus, and atmosphere addresses fundamental heliophysics questions with wide-reaching impact across helio- and astrophysics. New developments like miniaturized X-ray optics and radiation-tolerant detectors, provide compact, lightweight, wide-field X-ray instruments perfectly suited to the Jupiter system, enabling this exciting new possibility., Comment: A White Paper for the 2024-2033 Solar and Space Physics (Heliophysics) Decadal Survey

Published
2023

3. Moonraker -- Enceladus Multiple Flyby Mission

Author

Mousis, O., Bouquet, A., Langevin, Y., André, N., Boithias, H., Durry, G., Faye, F., Hartogh, P., Helbert, J., Iess, L., Kempf, S., Masters, A., Postberg, F., Renard, J. -B., Vernazza, P., Vorburger, A., Wurz, P., Atkinson, D. H., Barabash, S., Berthomier, M., Brucato, J., Cable, M., Carter, J., Cazaux, S., Coustenis, A., Danger, G., Dehant, V., Fornaro, T., Garnier, P., Gautier, T., Groussin, O., Hadid, L. Z., Ize, J. -C., Kolmasova, I., Lebreton, J. -P., Maistre, S. Le, Lellouch, E., Lunine, J. I., Mandt, K. E., Martins, Z., Mimoun, D., Nenon, Q., Caro, G. M. Munõz, Rannou, P., Rauer, H., Schmitt-Kopplin, P., Schneeberger, A., Simons, M., Stephan, K., Van Hoolst, T., Vaverka, J., Wieser, M., and Wörner, L.

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

Enceladus, an icy moon of Saturn, possesses an internal water ocean and jets expelling ocean material into space. Cassini investigations indicated that the subsurface ocean could be a habitable environment having a complex interaction with the rocky core. Further investigation of the composition of the plume formed by the jets is necessary to fully understand the ocean, its potential habitability, and what it tells us about Enceladus' origin. Moonraker has been proposed as an ESA M-class mission designed to orbit Saturn and perform multiple flybys of Enceladus, focusing on traversals of the plume. The proposed Moonraker mission consists of an ESA-provided platform, with strong heritage from JUICE and Mars Sample Return, and carrying a suite of instruments dedicated to plume and surface analysis. The nominal Moonraker mission has a duration of 13.5 years. It includes a 23-flyby segment with 189 days allocated for the science phase, and can be expanded with additional segments if resources allow. The mission concept consists in investigating: i) the habitability conditions of present-day Enceladus and its internal ocean, ii) the mechanisms at play for the communication between the internal ocean and the surface of the South Polar Terrain, and iii) the formation conditions of the moon. Moonraker, thanks to state-of-the-art instruments representing a significant improvement over Cassini's payload, would quantify the abundance of key species in the plume, isotopic ratios, and physical parameters of the plume and the surface. Such a mission would pave the way for a possible future landed mission., Comment: Accepted for publication in The Planetary Science Journal

Published
2022

4. Imaging Jupiter's radiation belts down to 127 MHz with LOFAR

Author

Girard, J. N., Zarka, P., Tasse, C., Hess, S., de Pater, I., Santos-Costa, D., Nenon, Q., Sicard, A., Bourdarie, S., Anderson, J., Asgekar, A., Bell, M. E., van Bemmel, I., Bentum, M. J., Bernardi, G., Best, P., Bonafede, A., Breitling, F., Breton, R. P., Broderick, J. W., Brouw, W. N., Brüggen, M., Ciardi, B., Corbel, S., Corstanje, A., de Gasperin, F., de Geus, E., Deller, A., Duscha, S., Eislöffel, J., Falcke, H., Frieswijk, W., Garrett, M. A., Grießmeier, J., Gunst, A. W., Hessels, J. W. T., Hoeft, M., Hörandel, J., Iacobelli, M., Juette, E., Kondratiev, V. I., Kuniyoshi, M., Kuper, G., van Leeuwen, J., Loose, M., Maat, P., Mann, G., Markov, S., McFadden, R., McKay-Bukowski, D., Moldon, J., Munk, H., Nelles, A., Norden, M. J., Orru, E., Paas, H., Pandey-Pommier, M., Pizzo, R., Polatidis, A. G., Reich, W., Röttgering, H., Rowlinson, A., Schwarz, D., Smirnov, O., Steinmetz, M., Swinbank, J., Tagger, M., Thoudam, S., Toribio, M. C., Vermeulen, R., Vocks, C., van Weeren, R. J., Wijers, R. A. M. J., and Wucknitz, O.

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

Context. Observing Jupiter's synchrotron emission from the Earth remains today the sole method to scrutinize the distribution and dynamical behavior of the ultra energetic electrons magnetically trapped around the planet (because in-situ particle data are limited in the inner magnetosphere). Aims. We perform the first resolved and low-frequency imaging of the synchrotron emission with LOFAR at 127 MHz. The radiation comes from low energy electrons (~1-30 MeV) which map a broad region of Jupiter's inner magnetosphere. Methods (see article for complete abstract) Results. The first resolved images of Jupiter's radiation belts at 127-172 MHz are obtained along with total integrated flux densities. They are compared with previous observations at higher frequencies and show a larger extent of the synchrotron emission source (>=4 $R_J$). The asymmetry and the dynamic of east-west emission peaks are measured and the presence of a hot spot at lambda_III=230 {\deg} $\pm$ 25 {\deg}. Spectral flux density measurements are on the low side of previous (unresolved) ones, suggesting a low-frequency turnover and/or time variations of the emission spectrum. Conclusions. LOFAR is a powerful and flexible planetary imager. The observations at 127 MHz depict an extended emission up to ~4-5 planetary radii. The similarities with high frequency results reinforce the conclusion that: i) the magnetic field morphology primarily shapes the brightness distribution of the emission and ii) the radiating electrons are likely radially and latitudinally distributed inside about 2 $R_J$. Nonetheless, the larger extent of the brightness combined with the overall lower flux density, yields new information on Jupiter's electron distribution, that may shed light on the origin and mode of transport of these particles., Comment: 10 pages, 12 figures, accepted for publication in A&A (27/11/2015) - abstract edited because of limited characters

Published
2015
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8. Moonraker: Enceladus Multiple Flyby Mission

Author

Mousis, O., primary, Bouquet, A., additional, Langevin, Y., additional, André, N., additional, Boithias, H., additional, Durry, G., additional, Faye, F., additional, Hartogh, P., additional, Helbert, J., additional, Iess, L., additional, Kempf, S., additional, Masters, A., additional, Postberg, F., additional, Renard, J.-B., additional, Vernazza, P., additional, Vorburger, A., additional, Wurz, P., additional, Atkinson, D. H., additional, Barabash, S., additional, Berthomier, M., additional, Brucato, J., additional, Cable, M., additional, Carter, J., additional, Cazaux, S., additional, Coustenis, A., additional, Danger, G., additional, Dehant, V., additional, Fornaro, T., additional, Garnier, P., additional, Gautier, T., additional, Groussin, O., additional, Hadid, L. Z., additional, Ize, J.-C., additional, Kolmasova, I., additional, Lebreton, J.-P., additional, Maistre, S. Le, additional, Lellouch, E., additional, Lunine, J. I., additional, Mandt, K. E., additional, Martins, Z., additional, Mimoun, D., additional, Nenon, Q., additional, Caro, G. M. Muñoz, additional, Rannou, P., additional, Rauer, H., additional, Schmitt-Kopplin, P., additional, Schneeberger, A., additional, Simons, M., additional, Stephan, K., additional, Hoolst, T. Van, additional, Vaverka, J., additional, Wieser, M., additional, and Wörner, L., additional

Published
2022
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9. Moonraker: Enceladus Multiple Flyby Mission

Author

UCL - SST/ELI/ELIC - Earth & Climate, Mousis, O., Bouquet, A., Langevin, Y., André, N., Boithias, H., Durry, G., Faye, F., Hartogh, P., Helbert, J., Iess, L., Kempf, S., Masters, A., Postberg, F., Renard, J.-B., Vernazza, P., Vorburger, A., Wurz, P., Atkinson, D. H., Barabash, S., Berthomier, M., Brucato, J., Cable, M., Carter, J., Cazaux, S., Coustenis, A., Danger, G., Dehant, Véronique, Fornaro, T., Garnier, P., Gautier, T., Groussin, O., Hadid, L. Z., Ize, J.-C., Kolmasova, I., Lebreton, J.-P., Maistre, S. Le, Lellouch, E., Lunine, J. I., Mandt, K. E., Martins, Z., Mimoun, D., Nenon, Q., Caro, G. M. Muñoz, Rannou, P., Rauer, H., Schmitt-Kopplin, P., Schneeberger, A., Simons, M., Stephan, K., Hoolst, T. Van, Vaverka, J., Wieser, M., Wörner, L., UCL - SST/ELI/ELIC - Earth & Climate, Mousis, O., Bouquet, A., Langevin, Y., André, N., Boithias, H., Durry, G., Faye, F., Hartogh, P., Helbert, J., Iess, L., Kempf, S., Masters, A., Postberg, F., Renard, J.-B., Vernazza, P., Vorburger, A., Wurz, P., Atkinson, D. H., Barabash, S., Berthomier, M., Brucato, J., Cable, M., Carter, J., Cazaux, S., Coustenis, A., Danger, G., Dehant, Véronique, Fornaro, T., Garnier, P., Gautier, T., Groussin, O., Hadid, L. Z., Ize, J.-C., Kolmasova, I., Lebreton, J.-P., Maistre, S. Le, Lellouch, E., Lunine, J. I., Mandt, K. E., Martins, Z., Mimoun, D., Nenon, Q., Caro, G. M. Muñoz, Rannou, P., Rauer, H., Schmitt-Kopplin, P., Schneeberger, A., Simons, M., Stephan, K., Hoolst, T. Van, Vaverka, J., Wieser, M., and Wörner, L.

Abstract

Enceladus, an icy moon of Saturn, possesses an internal water ocean and jets expelling ocean material into space. Cassini investigations indicated that the subsurface ocean could be a habitable environment having a complex interaction with the rocky core. Further investigation of the composition of the plume formed by the jets is necessary to fully understand the ocean, its potential habitability, and what it tells us about Enceladus's origin. Moonraker has been proposed as an ESA M-class mission designed to orbit Saturn and perform multiple flybys of Enceladus, focusing on traversals of the plume. The proposed Moonraker mission consists of an ESA-provided platform with strong heritage from JUICE and Mars Sample Return and carrying a suite of instruments dedicated to plume and surface analysis. The nominal Moonraker mission has a duration of ∼13.5 yr. It includes a 23-flyby segment with 189 days allocated for the science phase and can be expanded with additional segments if resources allow. The mission concept consists of investigating (i) the habitability conditions of present-day Enceladus and its internal ocean, (ii) the mechanisms at play for the communication between the internal ocean and the surface of the South Polar Terrain, and (iii) the formation conditions of the moon. Moonraker, thanks to state-of-the-art instruments representing a significant improvement over Cassini's payload, would quantify the abundance of key species in the plume, isotopic ratios, and the physical parameters of the plume and the surface. Such a mission would pave the way for a possible future landed mission.

Published
2022

10. The in-situ exploration of Jupiter's radiation belts

Author

Roussos, E., Allanson, O., Andre, N., Bertucci, B., Branduardi-Raymont, G., Clark, G., Dialynas, K., Dandouras, I., Desai, R.T., Futaana, Y., Gkioulidou, M., Jones, G.H., Kollmann, P., Kotova, A., Kronberg, E.A., Krupp, N., Murakami, G., Nenon, Q., Nordheim, T., Palmaerts, B., Plainaki, C., Rae, J., Santos-Costa, D., Sarris, T., Shprits, Y., Sulaiman, A., Woodfield, E., Wu, X., Yao, Z.H., Roussos, E., Allanson, O., Andre, N., Bertucci, B., Branduardi-Raymont, G., Clark, G., Dialynas, K., Dandouras, I., Desai, R.T., Futaana, Y., Gkioulidou, M., Jones, G.H., Kollmann, P., Kotova, A., Kronberg, E.A., Krupp, N., Murakami, G., Nenon, Q., Nordheim, T., Palmaerts, B., Plainaki, C., Rae, J., Santos-Costa, D., Sarris, T., Shprits, Y., Sulaiman, A., Woodfield, E., Wu, X., and Yao, Z.H.

Abstract

Jupiter has the most complex and energetic radiation belts in our Solar System and one of the most challenging space environments to measure and characterize in-depth. Their hazardous environment is also a reason why so many spacecraft avoid flying directly through their most intense regions, thus explaining how Jupiter's radiation belts have kept many of their secrets so well hidden, despite having been studied for decades. In this paper we argue why these secrets are worth unveiling. Jupiter's radiation belts and the vast magnetosphere that encloses them constitute an unprecedented physical laboratory, suitable for interdisciplinary and novel scientific investigations: from studying fundamental high energy plasma physics processes which operate throughout the Universe, such as adiabatic charged particle acceleration and nonlinear wave-particle interactions, to exploiting the astrobiological consequences of energetic particle radiation. The in-situ exploration of the uninviting environment of Jupiter's radiation belts presents us with many challenges in mission design, science planning, instrumentation, and technology. We address these challenges by reviewing the different options that exist for direct and indirect observations of this unique system. We stress the need for new instruments, the value of synergistic Earth and Jupiter-based remote sensing and in-situ investigations, and the vital importance of multi-spacecraft in-situ measurements. While simultaneous, multi-point in-situ observations have long become the standard for exploring electromagnetic interactions in the inner Solar System, they have never taken place at Jupiter or any strongly magnetized planet besides Earth. We conclude that a dedicated multi-spacecraft mission to Jupiter is an essential and obvious way forward for exploring the planet's radiation belts. Besides guaranteeing numerous discoveries and huge leaps in our understanding of radiation belt systems, such a mission would also enable u

Published
2022

11. Magnetospheric Studies: A requirement for addressing interdisciplinary mysteries in the Ice Giant systems [White Paper]

Author

Kollmann, P., Allegini, F., Allen, R., André, N., Azari, A., Bagenal, F., Beddingfield, C., Brain, D., Brandt, P., Cao, X., Cartwright, R., Clark, G., Cohen, I., Cooper, J., Crary, F., Leonard, E., Paty, C., Pater, I., Desai, R., DiBraccio, G., Dietrich, W., Dong, C., Ebert, R., Felici, M., Filwett, R., Fischer, G., Gershman, D., Gkioulidou, M., Greathouse, T., Griton, L., Gritsevich, M., Hibbitts, K., Hospodarsky, G., Hue, V., Hunt, G., Huybrighs, H., Imai, M., Jackman, C., Jasinski, J., Jia, X., Jun, I., Kotova, A., Kurth, W., Lamy, L., Lazio, J., Lejosne, S., Louis, C., Masters, A., Mauk, B., Madanian, H., Mandt, K., McNutt, R., Melin, H., Miller, S., Moore, L., Nenon, Q., Neubauer, F., Nordheim, T., Palmaerts, B., Paranicas, C., Phipps, P., Regoli, L., Retherford, K., Roth, L., Roussos, E., Runyon, K., Rymer, A., Saur, J., Santos-Costa, D., SHPRITS, Y., Spilker, L., Stallard, T., Smirnov, A., Soderlund, K., Stanley, S., Sulaiman, A., Szalay, J., Turner, D., Vines, S., Wang, L., Weiss, B., Wicht, J., Wilson, R., and Woodfield, E.

Published
2021

12. The in-situ exploration of Jupiter's radiation belts

Author

Roussos, E., Allanson, O., Andre, N., Bertucci, B., Branduardi-Raymont, G., Clark, G., Dialynas, K., Dandouras, I., Desai, R.T., Futaana, Y., Gkioulidou, M., Jones, G.H., Kollmann, P., Kotova, A., Kronberg, E.A., Krupp, N., Murakami, G., Nenon, Q., Nordheim, T., Palmaerts, B., Plainaki, C., Rae, J., Santos-Costa, D., Sarris, T., Shprits, Y., Sulaiman, A., Woodfield, E., Wu, X., Yao, Z.H., Roussos, E., Allanson, O., Andre, N., Bertucci, B., Branduardi-Raymont, G., Clark, G., Dialynas, K., Dandouras, I., Desai, R.T., Futaana, Y., Gkioulidou, M., Jones, G.H., Kollmann, P., Kotova, A., Kronberg, E.A., Krupp, N., Murakami, G., Nenon, Q., Nordheim, T., Palmaerts, B., Plainaki, C., Rae, J., Santos-Costa, D., Sarris, T., Shprits, Y., Sulaiman, A., Woodfield, E., Wu, X., and Yao, Z.H.

Abstract

Jupiter has the most complex and energetic radiation belts in our Solar System and one of the most challenging space environments to measure and characterize in-depth. Their hazardous environment is also a reason why so many spacecraft avoid flying directly through their most intense regions, thus explaining how Jupiter's radiation belts have kept many of their secrets so well hidden, despite having been studied for decades. In this paper we argue why these secrets are worth unveiling. Jupiter's radiation belts and the vast magnetosphere that encloses them constitute an unprecedented physical laboratory, suitable for interdisciplinary and novel scientific investigations: from studying fundamental high energy plasma physics processes which operate throughout the Universe, such as adiabatic charged particle acceleration and nonlinear wave-particle interactions, to exploiting the astrobiological consequences of energetic particle radiation. The in-situ exploration of the uninviting environment of Jupiter's radiation belts presents us with many challenges in mission design, science planning, instrumentation, and technology. We address these challenges by reviewing the different options that exist for direct and indirect observations of this unique system. We stress the need for new instruments, the value of synergistic Earth and Jupiter-based remote sensing and in-situ investigations, and the vital importance of multi-spacecraft in-situ measurements. While simultaneous, multi-point in-situ observations have long become the standard for exploring electromagnetic interactions in the inner Solar System, they have never taken place at Jupiter or any strongly magnetized planet besides Earth. We conclude that a dedicated multi-spacecraft mission to Jupiter is an essential and obvious way forward for exploring the planet's radiation belts. Besides guaranteeing numerous discoveries and huge leaps in our understanding of radiation belt systems, such a mission would also enable u

Published
2021

13. Magnetospheric Studies: A requirement for addressing interdisciplinary mysteries in the Ice Giant systems

Author

Kollmann, Peter, primary, Allegini, F., additional, Allen, R. C., additional, André, N., additional, Azari, A. R., additional, Bagenal, F., additional, Beddingfield, C. B., additional, Brain, D., additional, Brandt, P., additional, Cao, X., additional, Cartwright, R. J., additional, Clark, G., additional, Cohen, I., additional, Cooper, J. F., additional, Crary, F., additional, Leonard, E. J., additional, Paty, C., additional, Pater, I. de, additional, Desai, R. T., additional, DiBraccio, G. A., additional, Dietrich, W., additional, Dong, C., additional, Ebert, R. W., additional, Felici, M., additional, Filwett, R. J., additional, Fischer, G., additional, Gershman, D. J., additional, Gkioulidou, M., additional, Greathouse, T. K., additional, Griton, L., additional, Gritsevich, M., additional, Hibbitts, K., additional, Hospodarsky, G., additional, Hue, V., additional, Hunt, G., additional, Huybrighs, H. L. F., additional, Imai, M., additional, Jackman, C. M., additional, Jasinski, J. M., additional, Jia, X., additional, Jun, I., additional, Kotova, A., additional, Kurth, W. S., additional, Lamy, L., additional, Lazio, J., additional, Lejosne, S., additional, Louis, C., additional, Masters, A., additional, Mauk, B., additional, Madanian, H., additional, Mandt, K. E., additional, Jr., R. McNutt,, additional, Melin, H., additional, Miller, S., additional, Moore, L., additional, Nenon, Q., additional, Neubauer, F. M., additional, Nordheim, T., additional, Palmaerts, B., additional, Paranicas, C., additional, Phipps, P., additional, Regoli, L., additional, Retherford, K., additional, Roth, L., additional, Roussos, E., additional, Runyon, K. D., additional, Rymer, A., additional, Saur, J., additional, Santos-Costa, D., additional, Shprits, Y. Y., additional, Spilker, L. J., additional, Stallard, T., additional, Smirnov, A. G., additional, Soderlund, K., additional, Stanley, S., additional, Sulaiman, A. H., additional, Szalay, J. R., additional, Turner, D. L., additional, Vines, S., additional, Wang, L., additional, Weiss, B., additional, Wicht, J., additional, Wilson, R. J., additional, and Woodfield, E., additional

Published
2021
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14. Imaging Jupiter’s radiation belts down to 127 MHz with LOFAR

Author

Girard, J. N., Zarka, P., Tasse, C., Hess, S., de Pater, I., Santos-Costa, D., Nenon, Q., Sicard, A., Bourdarie, S., Anderson, J., Asgekar, A., Bell, M. E., van Bemmel, I., Bentum, M. J., Bernardi, G., Best, P., Bonafede, A., Breitling, F., Breton, R. P., Broderick, J. W., Brouw, W. N., Brüggen, M., Ciardi, B., Corbel, S., Corstanje, A., de Gasperin, F., de Geus, E., Deller, A., Duscha, S., Eislöffel, J., Falcke, H., Frieswijk, W., Garrett, M. A., Grießmeier, J., Gunst, A. W., Hessels, J. W. T., Hoeft, M., Hörandel, J., Iacobelli, M., Juette, E., Kondratiev, V. I., Kuniyoshi, M., Kuper, G., van Leeuwen, J., Loose, M., Maat, P., Mann, G., Markoff, S., McFadden, R., McKay-Bukowski, D., Moldon, J., Munk, H., Nelles, A., Norden, M. J., Orru, E., Paas, H., Pandey-Pommier, M., Pizzo, R., Polatidis, A. G., Reich, W., Röttgering, H., Rowlinson, A., Schwarz, D., Smirnov, O., Steinmetz, M., Swinbank, J., Tagger, M., Thoudam, Satyendra, Toribio, M. C., Vermeulen, R., Vocks, C., van Weeren, R. J., Wijers, R. A. M. J., Wucknitz, O., Girard, J. N., Zarka, P., Tasse, C., Hess, S., de Pater, I., Santos-Costa, D., Nenon, Q., Sicard, A., Bourdarie, S., Anderson, J., Asgekar, A., Bell, M. E., van Bemmel, I., Bentum, M. J., Bernardi, G., Best, P., Bonafede, A., Breitling, F., Breton, R. P., Broderick, J. W., Brouw, W. N., Brüggen, M., Ciardi, B., Corbel, S., Corstanje, A., de Gasperin, F., de Geus, E., Deller, A., Duscha, S., Eislöffel, J., Falcke, H., Frieswijk, W., Garrett, M. A., Grießmeier, J., Gunst, A. W., Hessels, J. W. T., Hoeft, M., Hörandel, J., Iacobelli, M., Juette, E., Kondratiev, V. I., Kuniyoshi, M., Kuper, G., van Leeuwen, J., Loose, M., Maat, P., Mann, G., Markoff, S., McFadden, R., McKay-Bukowski, D., Moldon, J., Munk, H., Nelles, A., Norden, M. J., Orru, E., Paas, H., Pandey-Pommier, M., Pizzo, R., Polatidis, A. G., Reich, W., Röttgering, H., Rowlinson, A., Schwarz, D., Smirnov, O., Steinmetz, M., Swinbank, J., Tagger, M., Thoudam, Satyendra, Toribio, M. C., Vermeulen, R., Vocks, C., van Weeren, R. J., Wijers, R. A. M. J., and Wucknitz, O.

Abstract

Context. With the limited amount of in situ particle data available for the innermost region of Jupiter’s magnetosphere, Earth-based observations of the giant planets synchrotron emission remain the sole method today of scrutinizing the distribution and dynamical behavior of the ultra energetic electrons magnetically trapped around the planet. Radio observations ultimately provide key information about the origin and control parameters of the harsh radiation environment. Aims. We perform the first resolved and low-frequency imaging of the synchrotron emission with LOFAR. At a frequency as low as 127 MHz, the radiation from electrons with energies of ~1–30 MeV are expected, for the first time, to be measured and mapped over a broad region of Jupiter’s inner magnetosphere. Methods. Measurements consist of interferometric visibilities taken during a single 10-hour rotation of the Jovian system. These visibilities were processed in a custom pipeline developed for planetary observations, combining flagging, calibration, wide-field imaging, direction-dependent calibration, and specific visibility correction for planetary targets. We produced spectral image cubes of Jupiter’s radiation belts at the various angular, temporal, and spectral resolutions from which flux densities were measured. Results. The first resolved images of Jupiter’s radiation belts at 127–172 MHz are obtained with a noise level ~20–25 mJy/beam, along with total integrated flux densities. They are compared with previous observations at higher frequencies. A greater extent of the synchrotron emission source (≥4 RJ) is measured in the LOFAR range, which is the signature – as at higher frequencies – of the superposition of a “pancake” and an isotropic electron distribution. Asymmetry of east-west emission peaks is measured, as well as the longitudinal dependence of the radial distance of the belts, and the presence of a hot spot at λIII = 230° ± 25°. Spectral flux density measurements are on the low side o

Published
2016
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15. Imaging Jupiter’s radiation belts down to 127 MHz with LOFAR

Author

Girard, J. N., primary, Zarka, P., additional, Tasse, C., additional, Hess, S., additional, de Pater, I., additional, Santos-Costa, D., additional, Nenon, Q., additional, Sicard, A., additional, Bourdarie, S., additional, Anderson, J., additional, Asgekar, A., additional, Bell, M. E., additional, van Bemmel, I., additional, Bentum, M. J., additional, Bernardi, G., additional, Best, P., additional, Bonafede, A., additional, Breitling, F., additional, Breton, R. P., additional, Broderick, J. W., additional, Brouw, W. N., additional, Brüggen, M., additional, Ciardi, B., additional, Corbel, S., additional, Corstanje, A., additional, de Gasperin, F., additional, de Geus, E., additional, Deller, A., additional, Duscha, S., additional, Eislöffel, J., additional, Falcke, H., additional, Frieswijk, W., additional, Garrett, M. A., additional, Grießmeier, J., additional, Gunst, A. W., additional, Hessels, J. W. T., additional, Hoeft, M., additional, Hörandel, J., additional, Iacobelli, M., additional, Juette, E., additional, Kondratiev, V. I., additional, Kuniyoshi, M., additional, Kuper, G., additional, van Leeuwen, J., additional, Loose, M., additional, Maat, P., additional, Mann, G., additional, Markoff, S., additional, McFadden, R., additional, McKay-Bukowski, D., additional, Moldon, J., additional, Munk, H., additional, Nelles, A., additional, Norden, M. J., additional, Orru, E., additional, Paas, H., additional, Pandey-Pommier, M., additional, Pizzo, R., additional, Polatidis, A. G., additional, Reich, W., additional, Röttgering, H., additional, Rowlinson, A., additional, Schwarz, D., additional, Smirnov, O., additional, Steinmetz, M., additional, Swinbank, J., additional, Tagger, M., additional, Thoudam, S., additional, Toribio, M. C., additional, Vermeulen, R., additional, Vocks, C., additional, van Weeren, R. J., additional, Wijers, R. A. M. J., additional, and Wucknitz, O., additional

Published
2016
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16. Imaging Jupiter's radiation belts down to 127 MHz with LOFAR

Author

Gianni Bernardi, Jörg R. Hörandel, A. G. Polatidis, Ashish Asgekar, A. Nelles, Angélica Sicard, H. Munk, R. J. van Weeren, Jason W. T. Hessels, D. McKay-Bukowski, I. de Pater, Matthias Hoeft, Oleg Smirnov, A. W. Gunst, Frank Breitling, Arthur Corstanje, Sebastien Hess, Quentin Nénon, Mark J. Bentum, J. van Leeuwen, R. C. Vermeulen, M. Loose, P. Zarka, H. J. A. Röttgering, P. Maat, M. J. Norden, M. Tagger, J. Moldón, F. de Gasperin, S. Bourdarie, Rene P. Breton, Annalisa Bonafede, John D. Swinbank, I. van Bemmel, Stephane Corbel, Martin Bell, V. I. Kondratiev, M. Pandey-Pommier, M. Iacobelli, James M. Anderson, Roberto Pizzo, Marcus Brüggen, Satyendra Thoudam, M. C. Toribio, Gerard H. Kuper, Antonia Rowlinson, Jochen Eislöffel, S. Duscha, Rebecca McFadden, M. A. Garrett, Daniel Santos-Costa, Julien N. Girard, Matthias Steinmetz, B. Ciardi, O. Wucknitz, J.-M. Grießmeier, M. Kuniyoshi, Ralph A. M. J. Wijers, Wilfred Frieswijk, Heino Falcke, C. Tasse, W. N. Brouw, S. Markov, Emanuela Orrú, H. Paas, Adam Deller, W. Reich, Dominik J. Schwarz, J. W. Broderick, E. Juette, G. Mann, Philip Best, C. Vocks, E. de Geus, Girard, J.N., Zarka, P., Tasse, C., Hess, S., De Pater, I., Santos-Costa, D., Nenon, Q., Sicard, A., Bourdarie, S., Anderson, J., Asgekar, A., Bell, M.E., Van Bemmel, I., Bentum, M.J., Bernardi, G., Best, P., Bonafede, A., Breitling, F., Breton, R.P., Broderick, J.W., Brouw, W.N., Brüggen, M., Ciardi, B., Corbel, S., Corstanje, A., De Gasperin, F., De Geus, E., Deller, A., Duscha, S., Eislöffel, J., Falcke, H., Frieswijk, W., Garrett, M.A., Grießmeier, J., Gunst, A.W., Hessels, J.W.T., Hoeft, M., Hörandel, J., Iacobelli, M., Juette, E., Kondratiev, V.I., Kuniyoshi, M., Kuper, G., Van Leeuwen, J., Loose, M., Maat, P., Mann, G., Markoff, S., McFadden, R., McKay-Bukowski, D., Moldon, J., Munk, H., Nelles, A., Norden, M.J., Orru, E., Paas, H., Pandey-Pommier, M., Pizzo, R., Polatidis, A.G., Reich, W., Röttgering, H., Rowlinson, A., Schwarz, D., Smirnov, O., Steinmetz, M., Swinbank, J., Tagger, M., Thoudam, S., Toribio, M.C., Vermeulen, R., Vocks, C., Van Weeren, R.J., Wijers, R.A.M.J., Wucknitz, O., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, ONERA - The French Aerospace Lab [Toulouse], ONERA, Netherlands Institute for Radio Astronomy (ASTRON), University of Southampton, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Jacobs University [Bremen], Leibniz-Institut für Astrophysik Potsdam (AIP), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Max Planck Institute for Astrophysics, Max-Planck-Gesellschaft, Radboud University [Nijmegen], Hamburger Sternwarte/Hamburg Observatory, Universität Hamburg (UHH), Thüringer Landessternwarte Tautenburg (TLS), Leiden Observatory [Leiden], Universiteit Leiden, Unité Scientifique de la Station de Nançay (USN), 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), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Department of Pure Mathematics and Mathematical Statistics (DPMMS), Faculty of mathematics Centre for Mathematical Sciences [Cambridge] (CMS), University of Cambridge [UK] (CAM)-University of Cambridge [UK] (CAM), Ruhr-Universität Bochum [Bochum], Max-Planck-Institut für Radioastronomie (MPIFR), University of Oulu, University of Groningen [Groningen], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Universität Bielefeld, Rhodes University, Grahamstown, Leibniz-Institut DSMZ-Deutsche Sammlung von Mikroorganismen und Zellkulturen GmbH / Leibniz Institute DSMZ-German Collection of Microorganisms and Cell Cultures (DSMZ), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, ANR-11-IDEX-0005,USPC,Université Sorbonne Paris Cité(2011), European Project: 228261,EC:FP7:ERC,ERC-2008-AdG,SPARSEASTRO(2009), ITA, GBR, FRA, DEU, NLD, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Radboud university [Nijmegen], Universiteit Leiden [Leiden], 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), 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)-Institut national des sciences de l'Univers (INSU - CNRS), Harvard University [Cambridge]-Smithsonian Institution, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics, Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), DPMMS/CMS, University of Cambridge [UK] (CAM), ANR-11-IDEX-0005-02/10-LABX-0023,UnivEarthS,Earth - Planets - Universe: observation, modeling, transfer(2011), Astronomy, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Faculty of Science

Subjects
radio continuum: planetary systems, Brightness, 010504 meteorology & atmospheric sciences, radio continuum: planetary, EWI-27447, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, FOS: Physical sciences, Astrophysics, Electron, METIS-321662, 7. Clean energy, 01 natural sciences, Jupiter, symbols.namesake, 0103 physical sciences, Emission spectrum, IR-103183, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Radio continuum: planetary system, Planets and satellites: magnetic field, Astronomy and Astrophysics, LOFAR, Astronomy and Astrophysic, planets and satellites: magnetic fields, Spectral flux density, 13. Climate action, Space and Planetary Science, Van Allen radiation belt, Techniques: interferometric, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, systems, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Observing Jupiter's synchrotron emission from the Earth remains today the sole method to scrutinize the distribution and dynamical behavior of the ultra energetic electrons magnetically trapped around the planet (because in-situ particle data are limited in the inner magnetosphere). Aims. We perform the first resolved and low-frequency imaging of the synchrotron emission with LOFAR at 127 MHz. The radiation comes from low energy electrons (~1-30 MeV) which map a broad region of Jupiter's inner magnetosphere. Methods (see article for complete abstract) Results. The first resolved images of Jupiter's radiation belts at 127-172 MHz are obtained along with total integrated flux densities. They are compared with previous observations at higher frequencies and show a larger extent of the synchrotron emission source (>=4 $R_J$). The asymmetry and the dynamic of east-west emission peaks are measured and the presence of a hot spot at lambda_III=230 {\deg} $\pm$ 25 {\deg}. Spectral flux density measurements are on the low side of previous (unresolved) ones, suggesting a low-frequency turnover and/or time variations of the emission spectrum. Conclusions. LOFAR is a powerful and flexible planetary imager. The observations at 127 MHz depict an extended emission up to ~4-5 planetary radii. The similarities with high frequency results reinforce the conclusion that: i) the magnetic field morphology primarily shapes the brightness distribution of the emission and ii) the radiating electrons are likely radially and latitudinally distributed inside about 2 $R_J$. Nonetheless, the larger extent of the brightness combined with the overall lower flux density, yields new information on Jupiter's electron distribution, that may shed light on the origin and mode of transport of these particles., Comment: 10 pages, 12 figures, accepted for publication in A&A (27/11/2015) - abstract edited because of limited characters

Published
2015
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