DOCSLIB.ORG

A Survey of Small-Scale Waves and Wave-Like Phenomena in Jupiter's

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
A Survey of Small-Scale Waves and Wave-Like Phenomena in Jupiter's EPSC Abstracts Vol. 14, EPSC2020-26, 2020 https://doi.org/10.5194/epsc2020-26 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. A Survey of Small-Scale Waves and Wave-Like Phenomena in Jupiter’s Atmosphere Glenn Orton1, Fachreddin Tabataba-Vakili1, John Rogers3, Candice Hansen4, and the JunoCam Waves Investigation Team* 1Jet Propulsion Laboratory, MS 183-501, Pasadena, United States of America ([email protected]) 3British Astronomical Association, London, UK 4Planetary Science Institute, Tucson, Arizona, USA *A full list of authors appears at the end of the abstract Abstract In the first 20 orbits of the Juno mission, over 150 waves and wave-like features have been detected by the JunoCam public-outreach camera. A wide variety of wave morphologies were detected over a wide latitude range, but the great majority were found near Jupiter’s equator. By analogy with previous studies of waves in Jupiter’s atmosphere, most of the waves detected are likely to be inertia-gravity waves. The Juno mission’s JunoCam instrument [1], has detected very small-scale waves. Our survey of JunoCam images revealed a surprising variety of features with wave-like morphologies. They are presented in terms of differences in visual morphology, without implication that this differentiation arises from the associated responsible dynamics. Long wave packets with short, dark wave fronts represent 79% of the types of waves in our inventory, especially in the Equatorial Zone (EZ) that were also detected in previous studies. These include wave trains with orthogonal wave crests. Even more commonly, we detected wave packets with tilted fronts that are not oriented orthogonally to the wave packet direction. Both the meridional extent and wavelength of these waves are much shorter than the Rossby deformation radius, so it is logical to assume that they are formed by and interact with small-scale turbulence, and thereby propagate the waves in all directions (Fig. 1). Sometimes the short wavefronts are aligned in curved wave packets, all associated with larger features, and located outside the EZ. Short wave packets with wide wave fronts were also detected. In the Earth’s atmosphere, such waves are often associated with thunderstorms producing a brief impulse period with radiating waves. Wave packets with bright features appear bright on a dark background rather than dark on a lighter background, like the waves described above. Differences between darker and brighter wave crests could be the composition of the material affected. Lee waves, stationary waves generated by the vertical deflection of winds over an obstacle, were also detected. Jupiter’s atmosphere no doubt possesses the dynamical equivalent of an obstacle (Fig. 2). Waves associated with large vortices include compact cyclonic and anticyclonic features with extended radial wavefronts, resembling structures in terrestrial cyclonic hurricanes (Fig. 3). Long, parallel dark streaks are seen both with a non-uniform patterns and in regularly spaced parallel bands. Their orientation suggests that they are tracing out the direction of flow on streamlines. Figure 4 plots the distribution of mean wavelengths for different types of waves and wave-like features as a function of latitude, co-plotted with mean zonal wind velocity. The minimum distance between crests is 29.1 km. The variability of wavelengths within a single packet is typically no greater than 20-30%. The equatorial waves with long packets and short crests in the EZ have wavelengths that are clustered between 30 km and 320 km, with most between 80 and 230 km in size. No waves are found at latitudes associated with retrograde zonal flow unless associated with a larger atmospheric feature. JunoCam, detected 157 waves or wave-like features in its first 20 perijove passes. Of these, 100 are waves with long, linear packets and short crests. Another 25were detected with short packets and long crests. They are all likely to be truly propagating waves, which form the vast majority of features detected, concentrated in a latitude range between 5ºS and 7ºN. Few of these appear to be associated with other features except for waves that appear to be oriented in lines of local flow. There were fewer waves in the EZ between the equator and 1ºN than there were immediately north and south of this band, which was different from the waves detected by Voyager imaging in 1979 that were more equally distributed. Other waves outside the EZ are influenced by other features. These include waves associated with an anticyclonic or cyclonic eddies, lee waves some 10 km above the surrounding cloud deck. Several features appeared within or emanating from vortices. Two sets of extremely long, curved features were detected near the edges of a southwestern extension of a region associated with high 5-µm radiances at the southern edge of the NEB. No waves were detected south of 7ºS that were not associated with larger vortices, such as the GRS. No waves or wave-like features were detected in regions of retrograde mean zonal flow that were not associated with larger features, similar to the waves detected by Voyager imaging. Acknowledgements The primary support for this research was provided by NASA, a portion of which was distributed to the Jet Propulsion Laboratory, California Institute of Technology. References [1] Hansen et al. Junocam: Juno’s outreach camera. Space Sci. Rev. 217, 475-506. 2017. [2] Wong et al. High-resolution UV/optical/IR imaging of Jupiter in 2016–2019. Space Sci. Rev. 247, 58. 2020. JunoCam Waves Investigation Team: Andrew P. Ingersoll (California Institute of Technology, Pasadena, California, USA), Shawn Brueshaber (Western Michigan University, Kalamazoo, Michigan, USA), Michael H. Wog (University of California Berkeley, California, USA; SETI Institute, Mountain View, Caiifornia, USA), Amy Simon (NASA Goddard Space Flight Center, Greenbelt, Maryland, USA), Michael Ravine & Michael Caplinger (Malin Space Science Systems, San Diego, California, USA), Dakota Smith (National Center for Atmospheric Research, Boulder, Colorado, USA), Scott Bolton (Southwest Research Institute, San Antonio, Texas, USA), Chloe Thepenier (Glendale Community College, Glendale, California, USA), Hamish Nicholson (Harvard College, Cambridge, Massachusetts, USA), Abigail Anthony (Golden West College, Huntington Beach, California, USA) Powered by TCPDF (www.tcpdf.org).
Load more

Recommended publications
  • Lessons Learned from the Juno Project
    Lessons Learned from the Juno Project Presented by: William McAlpine Insoo Jun EJSM Instrument Workshop January 18‐20, 2010 © 2010 All rights reserved. Pre‐decisional, For Planning and Discussion Purposes Only Y‐1 Topics Covered • Radiation environment • Radiation control program • Radiation control program lessons learned Pre‐decisional, For Planning and Discussion Purposes Only Y‐2 Juno Radiation Environments Pre‐decisional, For Planning and Discussion Purposes Only Y‐3 Radiation Environment Comparison • Juno TID environment is about a factor of 5 less than JEO • Juno peak flux rate is about a factor of 3 above JEO Pre‐decisional, For Planning and Discussion Purposes Only Y‐4 Approach for Mitigating Radiation (1) • Assign a radiation control manager to act as a focal point for radiation related activities and issues across the Project early in the lifecycle – Requirements, EEE parts, materials, environments, and verification • Establish a radiation advisory board to address challenging radiation control issues • Hold external reviews for challenging radiation control issues • Establish a radiation control process that defines environments, defines requirements, and radiation requirements verification documentation • Design the mission trajectory to minimize the radiation exposure Pre‐decisional, For Planning and Discussion Purposes Only Y‐5 Approach for Mitigating Radiation (2) • Optimize shielding design to accommodate cumulative total ionizing dose and displacement damage dose and instantaneous charged particle fluxes near Perijove
    [Show full text]
  • 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.
    [Show full text]
  • Juno Spacecraft Description
    Juno Spacecraft Description By Bill Kurth 2012-06-01 Juno Spacecraft (ID=JNO) Description The majority of the text in this file was extracted from the Juno Mission Plan Document, S. Stephens, 29 March 2012. [JPL D-35556] Overview For most Juno experiments, data were collected by instruments on the spacecraft then relayed via the orbiter telemetry system to stations of the NASA Deep Space Network (DSN). Radio Science required the DSN for its data acquisition on the ground. The following sections provide an overview, first of the orbiter, then the science instruments, and finally the DSN ground system. Juno launched on 5 August 2011. The spacecraft uses a deltaV-EGA trajectory consisting of a two-part deep space maneuver on 30 August and 14 September 2012 followed by an Earth gravity assist on 9 October 2013 at an altitude of 559 km. Jupiter arrival is on 5 July 2016 using two 53.5-day capture orbits prior to commencing operations for a 1.3-(Earth) year-long prime mission comprising 32 high inclination, high eccentricity orbits of Jupiter. The orbit is polar (90 degree inclination) with a periapsis altitude of 4200-8000 km and a semi-major axis of 23.4 RJ (Jovian radius) giving an orbital period of 13.965 days. The primary science is acquired for approximately 6 hours centered on each periapsis although fields and particles data are acquired at low rates for the remaining apoapsis portion of each orbit. Juno is a spin-stabilized spacecraft equipped for 8 diverse science investigations plus a camera included for education and public outreach.
    [Show full text]
  • Juno Magnetometer (MAG) Standard Product Data Record and Archive Volume Software Interface Specification
    Juno Magnetometer Juno Magnetometer (MAG) Standard Product Data Record and Archive Volume Software Interface Specification Preliminary March 6, 2018 Prepared by: Jack Connerney and Patricia Lawton Juno Magnetometer MAG Standard Product Data Record and Archive Volume Software Interface Specification Preliminary March 6, 2018 Approved: John E. P. Connerney Date MAG Principal Investigator Raymond J. Walker Date PDS PPI Node Manager Concurrence: Patricia J. Lawton Date MAG Ground Data System Staff 2 Table of Contents 1 Introduction ............................................................................................................................. 1 1.1 Distribution list ................................................................................................................... 1 1.2 Document change log ......................................................................................................... 2 1.3 TBD items ........................................................................................................................... 3 1.4 Abbreviations ...................................................................................................................... 4 1.5 Glossary .............................................................................................................................. 6 1.6 Juno Mission Overview ...................................................................................................... 7 1.7 Software Interface Specification Content Overview .........................................................
    [Show full text]
  • Dynamics of the J Avian Magnetosphere
    25 Dynamics of the J avian Magnetosphere N. Krupp, V. M. Vasyliunas, J. Woch, A. Lagg Max-Planck-Institut fur Sonnensystemforschung, Katlenburg-Lindau K. K. Khurana, M. G. Kivelson IGPP and Dept. Earth & Space Sciences, University of California, Los Angeles B. H. Mauk, E. C. Roelof, D. J. Williams, S. M. Krimigis The Johns Hopkins University Applied Physics Laboratory W. S. Kurth, L. A. Frank, W. R. Paterson Dept. of Physics & As.tronomy, University of Iowa 25.1 INTRODUCTION around Jupiter for almost 8 years (1995-2003), Galileo has collected in situ data of the jovian system over an extended Understanding the dynamic processes in the largest magne­ duration and has for the first time made possible the study tosphere of our solar system is one of the outstanding goals of Jupiter on timescales of weeks, months, and even years, of magnetospheric physics. These processes are associated using the same instrumentation. New regions of the jovian with temporal and/ or spatial variations of the global config­ magnetosphere have been explored, especially the jovian uration. Their timescales range from several tens of minutes magnetotail which was not visited by any of the previous to sizeable fractions of the planetary rotation period to long­ spacecraft (except, to a very minor extent, by Voyager 2). term variations which take several days to develop. They oc­ Additional inputs have become available from ground-based cur on both local and global spatial scales, out to dimensions and Earth-orbit-based measurements and from advanced representing a large fraction of the magnetosphere. global magneto hydrodynamic (MHD) simulations of the jo­ Early indications of a "living", varying jovian magneto­ vian magnetosphere.
    [Show full text]
  • Juno Observations of Large-Scale Compressions of Jupiter's Dawnside
    PUBLICATIONS Geophysical Research Letters RESEARCH LETTER Juno observations of large-scale compressions 10.1002/2017GL073132 of Jupiter’s dawnside magnetopause Special Section: Daniel J. Gershman1,2 , Gina A. DiBraccio2,3 , John E. P. Connerney2,4 , George Hospodarsky5 , Early Results: Juno at Jupiter William S. Kurth5 , Robert W. Ebert6 , Jamey R. Szalay6 , Robert J. Wilson7 , Frederic Allegrini6,7 , Phil Valek6,7 , David J. McComas6,8,9 , Fran Bagenal10 , Key Points: Steve Levin11 , and Scott J. Bolton6 • Jupiter’s dawnside magnetosphere is highly compressible and subject to 1Department of Astronomy, University of Maryland, College Park, College Park, Maryland, USA, 2NASA Goddard Spaceflight strong Alfvén-magnetosonic mode Center, Greenbelt, Maryland, USA, 3Universities Space Research Association, Columbia, Maryland, USA, 4Space Research coupling 5 • Magnetospheric compressions may Corporation, Annapolis, Maryland, USA, Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA, 6 7 enhance reconnection rates and Southwest Research Institute, San Antonio, Texas, USA, Department of Physics and Astronomy, University of Texas at San increase mass transport across the Antonio, San Antonio, Texas, USA, 8Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey, USA, magnetopause 9Office of the VP for the Princeton Plasma Physics Laboratory, Princeton University, Princeton, New Jersey, USA, • Total pressure increases inside the 10Laboratory for Atmospheric and Space Physics, University of Colorado
    [Show full text]
  • EGU2018-10209, 2018 EGU General Assembly 2018 © Author(S) 2018
    Geophysical Research Abstracts Vol. 20, EGU2018-10209, 2018 EGU General Assembly 2018 © Author(s) 2018. CC Attribution 4.0 license. Jupiter’s auroras in radio and ultraviolet wavelengths as seen from Juno Masafumi Imai (1), G. Randall Gladstone (2), William S. Kurth (1), Thomas K. Greathouse (2), George B. Hospodarsky (1), Scott J. Bolton (2), John E. P. Connerney (3), and Steven M. Levin (4) (1) University of Iowa, Iowa City, Iowa, United States ([email protected]), (2) Southwest Research Institute, San Antonio, Texas, United States, (3) NASA Goddard Space Flight Center, Greenbelt, Maryland, United States, (4) Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, United States Jupiter is the strongest auroral radio source in our solar system, producing low-frequency radio emissions in a broad frequency range from 10 kHz to 40 MHz from both north and south polar regions of the planet. These sporadic nonthermal bursts and ultraviolet (UV) auroras have been monitored with the radio and plasma wave instrument (Waves) and the ultraviolet spectrograph instrument (Juno-UVS) aboard the spinning Juno spacecraft in polar orbit about Jupiter since July 5, 2016. Waves is capable of recording the electric fields of waves from 50 Hz to 41 MHz with one electric dipole antenna and the magnetic fields of waves from 50 Hz to 20 kHz with one magnetic search coil sensor. Juno-UVS is designed to image and obtain spectra in a wavelength range from 70 to 205 nm with a 4 cm by 4 cm aperture. The Juno spacecraft rotates with a period of 30 s, which modulates the Waves spectral intensity sensed with the dipole antenna.
    [Show full text]
  • Radiation: Lessons Learned
    Radiation:Radiation: LessonsLessons LearnedLearned Scott Bolton Southwest Research Institute Insoo Jun Jet Propulsion Laboratory This document has been reviewed for export control and it does NOT contain controlled technical data. Juno Science Objectives • Origin – Determine O/H ratio (water abundance) and constrain core mass to decide among alternative theories of origin. • Interior – Understand Jupiter's interior structure and dynamical properties by mapping its gravitational and magnetic fields. • Atmosphere – Map variations in atmospheric composition, temperature, cloud opacity and dynamics to depths greater than 100 bars. • Polar Magnetosphere – Explore the three-dimensional structure of Jupiter's polar magnetosphere and aurorae. Juno Juno Payload Gravity Science (JPL/Italy) Magnetometer— MAG (GSFC) Microwave Radiometer— MWR (JPL) Energetic Particles —JEDI (APL) Plasma ions and electrons — JADE (SwRI) Plasma waves/radio — Waves (U of Iowa) Ultra Violet Imager — UVS (SwRI) Visible Camera – Juno Cam (Malin) InfraRed Imager – JIRAM (Italy) Radiation Lessons Learned 3 Juno Juno Mission Design Launch: August 2011 5 year cruise Baseline mission: 32 polar orbits Perijove ~5000 km 11 day period Spinner Solar-powered Orbit is designed to avoid radiation from the inner belts of Jupiter. Dips inside inner belt at perijove and goes above belts (Juno is in polar orbit). Radiation Lessons Learned 4 Juno Orbit 4: Juno Gravity Science 5 days 4 days 6-hour Jupiter science pass 3 days 2 days 1 day Opportunities for 0 communication 11 with Earth 10
    [Show full text]
  • The Pulsating Magnetosphere at Jupiter
    EGU2020-3651 https://doi.org/10.5194/egusphere-egu2020-3651 EGU General Assembly 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. The Pulsating Magnetosphere at Jupiter Harry Manners and Adam Masters Space and Atmospheric Physics Group, Blackett Laboratory, Imperial College London, London, UK ([email protected]) The magnetosphere of Jupiter is the largest planetary magnetosphere in the solar system, and plays host to internal dynamics that remain, in many ways, mysterious. Prominent among these mysteries are the ultra-low-frequency (ULF) pulses ubiquitous in this system. Pulsations in the electromagnetic emissions, magnetic field and flux of energetic particles have been observed for decades, with little to indicate the source mechanism. While ULF waves have been observed in the magnetospheres of all the magnetized planets, the magnetospheric environment at Jupiter seems particularly conducive to the emergence of ULF waves over a wide range of periods (1-100+ minutes). This is mainly due to the high variability of the system on a global scale: internal plasma sources and a powerful intrinsic magnetic field produce a highly-compressible magnetospheric cavity, which can be reduced to a size significantly smaller than its nominal expanded state by variations in the dynamic pressure of the solar wind. Compressive fronts in the solar wind, turbulent surface interactions on the magnetopause and internal plasma processes can also all lead to ULF wave activity inside the magnetosphere. To gain the first comprehensive view of ULF waves in the Jovian system, we have performed a heritage survey of magnetic field data measured by six spacecraft that visited the magnetosphere (Galileo, Ulysses, Voyager 1 & 2 and Pioneer 10 & 11).
    [Show full text]
  • First Observations Near Jupiter by the Juno Waves Investigation
    FIRST OBSERVATIONS NEAR JUPITER BY THE JUNO WAVES INVESTIGATION W. S. Kurth∗,M.Imai∗, G. B. Hospodarsky∗, D. A. Gurnett∗, S. S. Tetrick∗, S.–Y. Ye∗, S. J. Bolton†,J.E.P.Connerney‡, andS.M.Levin§ Abstract The Juno spacecraft successfully entered Jupiter orbit on 5 July 2016. One of Juno’s primary objectives is to explore Jupiter’s polar magnetosphere for the first time. An obvious major aspect of this exploration includes remote and in-situ observations of Jupiter’s auroras and the processes responsible for them. To this end, Juno carries a suite of particle, field, and remote sensing instruments. One of these instruments is a radio and plasma wave instrument called Waves, designed to detect one electric field component of waves in the frequency range of 50 Hz to 41 MHz and one magnetic field component of waves in the range of 50 Hz to 20 kHz. Juno’s first perijove pass with science observations occurred on 27 August 2016. This paper presents some of the first observations of the Juno Waves instrument made during that first perijove. Among radio emissions, kilometric, hectometric, and decametric emissions were observed. From a vantage point at high latitudes, many of Jupiter’s auroral radio emissions appear as V-shaped emissions in frequency–time space with vertices near the electron cyclotron frequency where the emissions intensify. In fact, we present observations suggesting Juno flew through or close to as many as five or six sources of auroral radio emissions during its first perijove. Waves made in-situ observations of plasma waves on auroral field lines such as whistler–mode hiss, a common feature of terrestrial auroral regions.
    [Show full text]
  • Plasma Waves in Jupiter's High Latitude Regions
    PLASMA WAVES IN JUPITER’S HIGH LATITUDE REGIONS: OBSERVATIONS FROM THE JUNO SPACECRAFT by Sadie Suzanne Tetrick A thesis submitted in partial fulfillment of the requirements for the Master of Science degree in Physics in the Graduate College of The University of Iowa December 2017 Thesis Supervisor: Professor Donald A. Gurnett Copyright by SADIE SUZANNE TETRICK 2017 All Rights Reserved Graduate College The University of Iowa Iowa City, Iowa CERTIFICATE OF APPROVAL ____________________________ MASTER'S THESIS _________________ This is to certify that the Master's thesis of Sadie Suzanne Tetrick has been approved by the Examining Committee for the thesis requirement for the Master of Science degree in Physics at the December 2017 graduation. Thesis Committee: Donald A. Gurnett, Thesis Supervisor Jasper S. Halekas, Committee Member Vincent G. J. Rodgers, Committee Member ACKNOWLEDGEMENTS A special thanks to Dr. Donald Gurnett and Dr. Bill Kurth for providing me the opportunity to work on Juno research and for their continued support during the completion of my Master of Science degree. I would also like to thank Masafumi Imai, Jeremy Faden, and Terry Averkamp for their help, feedback, and encouragement that has allowed me to successfully complete this research. A final thank you to my parents, Kelly and Paul Tetrick, my soon-to-be parents-in-law, Rose and Scott Elliott, and fiancé, Josh Elliott for their continued support throughout my educational journey. ii ABSTRACT The Juno Waves instrument detected new broadband plasma wave emissions on the first three successful passes over the low altitude polar regions of Jupiter on Days 240 and 346 of 2016 and Day 033 of 2017.
    [Show full text]
  • A Survey of Small-Scale Waves and Wave-Like Phenomena in Jupiter's Atmosphere Detected by Junocam
    1 A Survey of Small-Scale Waves and Wave-Like Phenomena in 2 Jupiter’s Atmosphere Detected by JunoCam 3 4 Glenn S. Orton1, Fachreddin Tabataba-Vakili1, Gerald Eichstädt2, John Rogers3, 5 Candice J. Hansen4, Thomas W. Momary1, Andrew P. Ingersoll5, Shawn Brueshaber 6, Michael 6 H. Wong7, Amy A. Simon8, Leigh N. Fletcher9, Michael Ravine10, Michael Caplinger10, Dakota 7 Smith11, Scott J. Bolton12, Stephen M. Levin1, James A. Sinclair1, Chloe Thepenier13, Hamish 8 Nicholson14, Abigail Anthony15 9 10 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA 11 2Independent scholar, Stuttgart, Germany 12 3British Astronomical Association, London, UK 13 4Planetary Science Institute, Tucson, Arizona, USA 14 5California Institute of Technology, Pasadena, California, USA 15 6Western Michigan University, Kalamazoo, Michigan, USA 16 7University of California, Berkeley, California, USA; SETI Institute, Mountain View, California, 17 USA 18 8NASA Goddard Space Flight Center, Greenbelt, Maryland, USA 19 9University of Leicester, Leicester, UK 20 10Malin Space Science Systems, San Diego, California, USA 21 11 National Center for Atmospheric Research, Boulder, Colorado, USA 22 12Southwest Research Institute, San Antonio, Texas, USA 23 13Glendale Community College, Glendale, California, USA† 24 14Harvard College, Cambridge, Massachusetts, USA 25 15Golden West College, Huntington Beach, California, USA†† 26 27 28 Corresponding author: Glenn Orton ([email protected]) 29 30 31 †currently at the University of California, Davis 32 ††currently at the University of California, Berkeley 33 34 Key Points: 35 -In the first 20 orbits of the Juno mission, over 150 waves and wave-like features have been 36 detected by the JunoCam public-outreach camera.
    [Show full text]