scholarly journals Energetic ion depletions near Europa and Io: the effect of plumes and atmospheric charge exchange

2020 ◽  
Author(s):  
Hans Huybrighs ◽  
Christiaan van Buchem ◽  
Aljona Blöcker ◽  
Elias Roussos ◽  
Norbert Krupp ◽  
...  
Keyword(s):  
Charge Exchange ◽  
Energetic Particle ◽  
Depletion Region ◽  
The Moon ◽  
Particle Detector ◽  
Particle Tracing ◽  
Energetic Ions ◽  
Galilean Moons ◽  
Upper Limits ◽  
Inert Body

<p><strong>Introduction</strong></p><p>The flux of energetic ions (protons, oxygen and sulfur) near the Galilean moons were measured by the Energetic Particle Detector (EPD) on the Galileo mission (1995 - 2003). Near Galilean moons (such as Io and Europa) depletions of the energetic ion flux, of several orders of magnitude, were identified.</p><p>Such energetic ion depletions can be caused by the absorption of these particles onto the moon’s surfaces or by the loss due to charge exchange with neutral molecules in the atmospheres or potential plumes. To interpret the depletion features in the EPD data, a Monte Carlo particle tracing simulation has been conducted. The expected fluxes of the energetic ions are simulated under different scenarios including those with and without an atmosphere or plume. By comparing the simulated flux [YF1] to the EPD data, we investigate the cause of the depletion features with particular focuses on Europa and Io flybys.</p><p><strong>Results</strong></p><p>For Europa we report the following findings:</p><ul><li>For flyby E12 we find that a global atmosphere should produce a depletion region along the trajectory that is symmetrical to the closest approach, for energetic protons in the energy range of 80-220 keV. No such feature is visible in the data. Upper limits of the atmosphere are consistent with surface densities (⩽ 10<sup>8 </sup>cm<sup>-3</sup>) and scale heights (50-350 km) of previous studies. We find that a depletion of energetic protons (80-220 keV) occurring before closest approach is consistent with the field perturbations associated with a plume. This plume features coincides in time with the plume reported by Jia et al., 2018.</li> <li>For flyby E26 we find that the depletions of energetic protons (80-220 keV) are consistent with a simulation that takes into account the perturbations of the fields as calculated by an MHD simulation and atmospheric charge exchange. Furthermore, a depletion feature occurring shortly after closest approach is consistent with the field perturbations associated with a plume, located near the plume reported by Arnold et al., 2019.</li> <li>From these investigations, we confirm, independently from previous reports, that the Galileo spacecraft could have passed near plumes.</li> </ul><p>For Io we report the following results:</p><ul><li>We identify regions of proton (80-220 keV) depletions during Io flybys I24, I27 and I31 extending beyond one Io radius. The depletions features are not consistent with Io as an inert body. We investigate atmospheric charge exchange as a cause for the depletions.</li> </ul>

scholarly journals Titan's exosphere and its interaction with Saturn's magnetosphere

2008 ◽  
Vol 367 (1889) ◽  
pp. 743-752 ◽  
Author(s):  
Iannis Dandouras ◽  
Philippe Garnier ◽  
Donald G Mitchell ◽  
Edmond C Roelof ◽  
Pontus C Brandt ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Remote Sensing ◽  
Charge Exchange ◽  
Mass Spectrometer ◽  
Upper Atmosphere ◽  
Neutral Atoms ◽  
Energetic Ions ◽  
Imaging Instrument ◽  
Singly Charged

Titan's nitrogen-rich atmosphere is directly bombarded by energetic ions, due to its lack of a significant intrinsic magnetic field. Singly charged energetic ions from Saturn's magnetosphere undergo charge-exchange collisions with neutral atoms in Titan's upper atmosphere, or exosphere, being transformed into energetic neutral atoms (ENAs). The ion and neutral camera, one of the three sensors that comprise the magnetosphere imaging instrument (MIMI) on the Cassini/Huygens mission to Saturn and Titan, images these ENAs like photons, and measures their fluxes and energies. These remote-sensing measurements, combined with the in situ measurements performed in the upper thermosphere and in the exosphere by the ion and neutral mass spectrometer instrument, provide a powerful diagnostic of Titan's exosphere and its interaction with the Kronian magnetosphere. These observations are analysed and some of the exospheric features they reveal are modelled.

Ground-based observations of the [SII] 6731 Å emission lines of the Io plasma torus

2016 ◽  
Vol 12 (S328) ◽  
pp. 227-229
Author(s):  
P. Magalhães Fabíola ◽  
Walter Gonzalez ◽  
Ezequiel Echer ◽  
Mariza P. Souza-Echer ◽  
Rosaly Lopes ◽  
...  
Keyword(s):  
Charged Particles ◽  
Emission Lines ◽  
Solar Telescope ◽  
The Moon ◽  
Active Object ◽  
Oxygen Ions ◽  
Galilean Moons ◽  
Plasma Torus ◽  
Io Plasma Torus ◽  
Galilean Moons Of Jupiter

AbstractThe Io Plasma Torus (IPT) is a doughnut-shaped structure of charged particles, composed mainly of sulfur and oxygen ions. The main source of the IPT is the moon Io, the most volcanically active object in the Solar System. Io is the innermost of the Galilean moons of Jupiter, the main source of the magnetospheric plasma and responsible for injecting nearly 1 ton/s of ions into Jupiter's magnetosphere. In this work ground-based observations of the [SII] 6731 Å emission lines are observed, obtained at the MacMath-Pierce Solar Telescope. The results shown here were obtained in late 1997 and occurred shortly after a period of important eruptions observed by the Galileo mission (1996-2003). Several outbursts were observed and periods of intense volcanic activity are important to correlate with periods of brightness enhancements observed at the IPT. The time of response between an eruption and enhancement at IPT is still not well understood.

scholarly journals Energetic Particle Tracing of Interplanetary CMEs: ULYSSES/HI-SCALE and ACE/EPAM Results

2004 ◽  
Vol 2004 (IAUS226) ◽  
pp. 361-366
Author(s):  
Olga E. Malandraki ◽  
D. Lario ◽  
T.E. Sarris ◽  
N. Tsaggas ◽  
E.T. Sarris
Keyword(s):  
Energetic Particle ◽  
Particle Tracing

First Results from Solar Orbiter’s Energetic Particle Detector

2021 ◽  
Author(s):  
Javier Rodriguez-Pacheco ◽  
Keyword(s):  
Energetic Particle ◽  
Wide Energy Range ◽  
High Temporal Resolution ◽  
The Sun ◽  
Particle Detector ◽  
First Results ◽  
Wide Energy ◽  
Spatio Temporal ◽  
Inner Heliosphere

<p>In this presentation, we will show the first measurements performed by EPD since the end of the commissioning phase until the latest results obtained. During these months EPD has been scanning the inner heliosphere at different heliocentric distances and heliolongitues allowing - together with other spacecraft - to investigate the spatio-temporal behavior of the particle populations in the inner heliosphere during solar minimum conditions. Solar Orbiter was launched from Cape Canaveral on February 10th, 2020, thus beginning the journey to its encounter with the Sun. Solar Orbiter carries ten scientific instruments, six remote sensing and four in situ, that will allow the mission main goal: how the Sun creates and controls the heliosphere. Among the in situ instruments, the Energetic Particle Detector (EPD) measures electrons, protons and heavy ions with high temporal resolution over a wide energy range, from suprathermal energies up to several hundreds of MeV/nucleon.</p>

Energetic particle radiations measured by particle detector on board CBERS-1 satellite

2007 ◽  
Vol 52 (5) ◽  
pp. 665-670 ◽  
Author(s):  
YongQiang Hao ◽  
Zuo Xiao ◽  
Hong Zou ◽  
DongHe Zhang
Keyword(s):  
Energetic Particle ◽  
Particle Detector

A discussion on infared astronomy - A far infrared sky survey

1969 ◽  
Vol 264 (1150) ◽  
pp. 267-271 ◽  
Keyword(s):  
Milky Way ◽  
Angular Resolution ◽  
Thermal Emission ◽  
Far Infrared ◽  
The Moon ◽  
Sky Survey ◽  
Upper Limits ◽  
Celestial Sphere ◽  
Thick Source ◽  
Thin Source

A balloon-borne instrument for making far infrared sky surveys with 2° angular resolution is described. In two initial flights at a wavelength of 320 μm approximately half of the celestial sphere including most of the northern milky way was surveyed. The thermal emission of the moon was alone detected. The upper limit to the flux from other sources was 3 x 10-12 W cm-2 in the 300 to 360 μm band, or approximately 2 x 10-23 W cm-2 Hz-1. A blackbody (optically thick) source 2° or greater in diameter yielding this flux would have a temperature of 10 °K. A warmer, small or optically thin source providing this much radiation in the Rayleigh-Jeans tail of the Plank distribution would have a temperature averaged over the 2° beam of 0.6 °K. These observations can be used to set upper limits to the opacity and temperature of interstellar grains.

scholarly journals The Energetic Particle Detector (EPD) Investigation and the Energetic Ion Spectrometer (EIS) for the Magnetospheric Multiscale (MMS) Mission

2014 ◽  
Vol 199 (1-4) ◽  
pp. 471-514 ◽  
Author(s):  
B. H. Mauk ◽  
J. B. Blake ◽  
D. N. Baker ◽  
J. H. Clemmons ◽  
G. D. Reeves ◽  
...  
Keyword(s):  
Energetic Particle ◽  
Particle Detector ◽  
Magnetospheric Multiscale

scholarly journals Energetic particle acceleration and transport by Alfvén/acoustic waves in tokamak-like Solar flares

2010 ◽  
Vol 6 (S274) ◽  
pp. 162-164
Author(s):  
Martin Obergaulinger ◽  
Manuel García-Muñoz
Keyword(s):  
Solar Flares ◽  
Acoustic Waves ◽  
Energetic Particle ◽  
Fusion Plasmas ◽  
Experimental Phase ◽  
Astrophysical Plasmas ◽  
Energetic Ions ◽  
Laboratory Plasmas ◽  
Magnetically Confined ◽  
Particle Exchange

AbstractAlfven/acoustic waves are ubiquitous in astrophysical as well as in laboratory plasmas. Their interplay with energetic ions is of crucial importance to understanding the energy and particle exchange in astrophysical plasmas as well as to obtaining a viable energy source in magnetically confined fusion devices. In magnetically confined fusion plasmas, an experimental phase-space characterisation of convective and diffusive energetic particle losses induced by Alfven/acoustic waves allows for a better understanding of the underlying physics. The relevance of these results in the problem of the anomalous heating of the solar corona is checked by MHD simulations of Tokamak-like Solar flare tubes.

Sign in / Sign up

Export Citation Format

Share Document