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Ganymede–Induced Decametric Radio Emission: In-Situ

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Ganymede–Induced Decametric Radio Emission: In-Situ manuscript submitted to Geophysical Research Letters 1 Ganymede{induced decametric radio emission: in-situ 2 observations and measurements by Juno 1 1 2;3 4 5 3 C. K. Louis , P. Louarn , F. Allegrini , W. S. Kurth , J. R. Szalay 1 4 IRAP, Universit´ede Toulouse, CNRS, CNES, UPS, (Toulouse), France 2 5 Southwest Research Institute, San Antonio, Texas, USA 3 6 Department of Physics and Astronomy, University of Texas at San Antonio, San Antonio, Texas, USA 4 7 Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA 5 8 Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey, USA 9 Key Points: 10 • First detailed wave/particle investigation of a Ganymede-induced decametric ra- 11 dio source using Juno/Waves and Juno/JADE instruments 12 • Confirmation that the emission is produced by a loss-cone-driven Cyclotron Maser 13 Instability 14 • Ganymede-induced radio emission is produced by electrons of ∼ 4-15 keV, at a ◦ ◦ 15 beaming angle [76 -83 ], and a frequency 1:005 − 1:021 × fce Corresponding author: C. K. Louis, [email protected] {1{ manuscript submitted to Geophysical Research Letters 16 Abstract 17 At Jupiter, part of the auroral radio emissions are induced by the Galilean moons 18 Io, Europa and Ganymede. Until now, they have been remotely detected, using ground- 19 based radio-telescopes or electric antennas aboard spacecraft. The polar trajectory of 20 the Juno orbiter allows the spacecraft to cross the magnetic flux tubes connected to these 21 moons, or their tail, and gives a direct measure of the characteristics of these decamet- 22 ric moon{induced radio emissions. In this study, we focus on the detection of a radio emis- 23 sion during the crossing of magnetic field lines connected to Ganymede's tail. Us- 24 ing electromagnetic waves (Juno/Waves) and in-situ electron measurements (Juno/JADE- 25 E), we estimate the radio source size of ∼ 250 km, a radio emission growth rate −4 26 > 3 × 10 , an resonant electron population of energy E = 4 − 15 keV and an emis- ◦ ◦ 27 sion beaming angle of θ = 76 −83 , at a frequency ∼ 1:005−1:021×fce. We also con- 28 firmed that radio emission is associated with Ganymede's down-tail far-ultraviolet emis- 29 sion. 30 Plain Language Summary 31 The Juno spacecraft crossed magnetic field lines connected to Ganymede's auro- 32 ral signature in Jupiter's atmosphere. At the same time, Juno also crossed a decamet- 33 ric radio source. By measuring the electrons during this radio source crossing, we deter- 34 mine that this emission is produced by the cyclotron maser instability driven by upgo- 35 ing electrons, at a frequency 0:5 to 2:1% above the cyclotron electronic frequency with 36 electrons of energy 4-15 keV. 37 1 Introduction 38 With the arrival of Juno at Jupiter in July 2016, the probe passes above the poles 39 once per orbit, every 53 days, and acquires high-resolution measurements in the auro- 40 ral regions (Bagenal et al., 2017). In particular the instruments Waves (radio and plasma 41 waves, Kurth et al., 2017), JADE-E (Jovian Auroral Distributions Experiment - Elec- 42 trons, McComas et al., 2017) and MAG (Magnetometer , Connerney et al., 2017) offer 43 a unique opportunity to investigate in-situ the Jovian radio emissions produced in these 44 polar regions. These instruments enable constraints on the position of the sources (Louis 45 et al., 2019; Imai et al., 2017, 2019) and the mechanism producing these emissions (Louarn {2{ manuscript submitted to Geophysical Research Letters 46 et al., 2017, 2018), the Cyclotron Maser Instability (CMI), which is also responsible for 47 the production of the auroral kilometric radiation at Earth and Saturn (Treumann, 2006; 48 Wu, 1985; Wu & Lee, 1979; Le Queau et al., 1984b, 1984a; Pritchett, 1986a). 49 This instability produces emissions very close to the electron cyclotron frequency 50 fce, and requires two primary conditions: (i) a magnetized plasma, where the electron 51 plasma frequency fpe (proportional to the square root of the electron plasma density ne) 52 is much lower than the electron cyclotron frequency fce (proportional to the magnetic 53 field amplitude B); and (ii) a weakly relativistic electron population previously accel- 54 erated along high-latitude magnetic field lines at typical energies of a few keV. The first 55 orbits of Jupiter allowed Louarn et al. (2017, 2018) to study in-situ the radio emission 56 during source crossings and determine that the auroral hectometric/decametric radio emis- 57 sions are driven by the CMI with a loss cone distribution function, i.e. triggered by a 58 lack in the up-going electron population. 59 The Jupiter auroral radio emission is split into three major components, depend- 60 ing on the emission wavelength, namely broadband kilometric, hectometric and deca- 61 metric. Part of the auroral radio emissions in the decametric range are induced by the 62 interaction between the jovian magnetosphere and the Galilean moons: the best known 63 case Io, discovered by Bigg (1964), Europa and Ganymede (Louis, Lamy, Zarka, Cec- 64 coni, & Hess, 2017; Zarka et al., 2018, 2017) and potentially Callisto (Menietti et 65 al., 2001; Higgins, 2007). These moons are also known to induce Far Ultraviolet (FUV) 66 aurora above Jupiter's atmosphere (Prang´eet al., 1996; Clarke, 1998; Clarke et 67 al., 2002; Bhattacharyya et al., 2018). 68 In the Io case, we know that FUV and radio auroral emission are produced by Alfv´enic 69 interactions, and that Io-induced radio emissions are produced on the magnetic field lines 70 connected to the main Alfv´enwing (MAW) and reflected Alfv´enwing (RAW) spots (Hess 71 et al., 2010). In the Europa and Ganymede case, FUV emissions have been observed 72 at the moon's footprint and along the moon's footprint tail (Bonfond, Gro- 73 dent, et al., 2017; Bonfond, Saur, et al., 2017), but no simultaneous observation 74 of FUV and radio emissions has yet been obtained. 75 In this study, we focus on Juno's crossing of field lines connected to Ganymede's 76 footprint tail, which took place on May 29, 2019, where simultaneous FUV (Szalay et 77 al., 2020a) and radio emission were observed (see Section 2). In Section 3 we present the {3{ manuscript submitted to Geophysical Research Letters 78 instability leading to radio emission and the calculation to determine the different pa- 79 rameters of the radio emission (growth rate, electron distribution function and energy, 80 opening of the emission cone). Finally in Section 4 we summarize and discuss the results. 81 2 Observations th th 82 On May 29 , 2019 between 07:37:14 and 07:37:32 (20 perijove) Juno crossed ◦ 83 the magnetic field lines connected to Ganymede's tail (∼ 8 downtail from Ganymede's 84 main auroral spot). The in-situ measurements of Juno/MAG and Juno/JADE for the 85 down-going electrons and the Juno/UVS images were used by Szalay et al. (2020a) to 86 show the presence of Alfv´enwave activity capable of accelerating electrons into the at- 87 mosphere and producing FUV emissions, observed at the footprint of the crossed mag- 88 netic field lines. Here we focus on the study of Juno/JADE for the up-going electrons 89 and the radio measurements of Juno/Waves. 90 Figure 1 displays Juno measurements around the Ganymede's tail flux tube en- 91 counter. Panel (a) presents the Juno/Waves measurements (low resolution mode) around 92 the twentieth perijove (∼ −2=+1 h). Panel (b) is a 5-minute zoom-in of panel (a) us- 93 ing the Juno/Waves high-resolution mode. The solid-white line represents fce while the 94 dashed-white line (panel b) represents 1:01×fce (typical frequency for a loss-cone-CMI- 95 driven emission with electron energy of ∼ 5 keV, see Louarn et al., 2017). Panels (c{ 96 f) display Juno/JADE-E (electrons) measurements: panel (c) presents the electron dif- 97 ferential energy flux; panels (d-e) display the electron distribution functions for energy 98 in range [2-21] keV for different pitch angle ranges, panel (e) showing a subset for 99 pitch angle corresponding to up-going electrons; panel (f) presents the par- 100 tial electron density, where all the low energy population (here < 0:050 keV) 101 is not accounted for. 102 Figure 1b displays an emission very close to fce, tangent to the 1:01×fce line, be- 103 tween ∼ 07:37:00 and ∼ 07:38:10. During this time interval, and more precisely between 104 ∼ 07:37:14 and ∼07:37:32 (during Ganymede's tail magnetic field lines crossing), we 105 observe an enhancement in the electron energy flux (panel c) at a few keV, a strong in- 106 tensification in the distribution function (panel d) and an increase of the electron den- 107 sity (panel f). {4{ manuscript submitted to Geophysical Research Letters 20 a Waves 3 5 dB above bacakgroun ) 3 0 15 2 5 2 0 Freq. (MHz 10 1 5 1 0 d 5 5 0 06:00 06:20 06:40 07:00 07:20 07:40 08:00 08:20 08:40 09:00 Waves 7.0 b 3 0 dB above bacakgroun 6.8 ) 2 5 6.6 2 0 Freq. (MHz 6.4 1 5 d 6.2 1 0 6.0 5 (sec 10 c -1 .cm (keV) 1 -2 .sr -1 Electron energy 0.1 ) d (deg) Pitch angle (s 3 .km e -6 ) (deg) Pitch angle f ) -3 (cm Electron density 07:35 07:36 07:37 07:38 07:39 07:40 RJ 1.53 1.51 1.49 1.47 1.45 1.43 LonIII 284.30 290.60 296.50 302.00 307.10 311.70 Lat 78.29 77.78 77.14 76.39 75.53 74.56 MLatJRM09 74.75 73.52 72.24 70.92 69.55 68.14 MLT 14.55 14.43 14.33 14.23 14.15 14.08 L 22.19 18.81 16.04 13.77 11.89 10.32 2019-05-29 (149) 7:35 to 7:40 Figure 1.
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