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Journal articles on the topic 'Ganymedes'

Author: Grafiati

Published: 4 June 2021

Last updated: 17 February 2022

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1

Eden, P. T. "Two Notes on Euripides." Classical Quarterly 38, no. 2 (December 1988): 560–61. http://dx.doi.org/10.1017/s0009838800037204.

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Students of the Orestes are fortunate to have two excellent commentaries at their disposal, by C. W. Willink (Oxford, 1986) and M. L. West (Warminster, 1987). Neither will help them to understand this line, which is ‘the only allusion to Ganymede's horsemanship’ (Willink ad loc), because ‘no story of riding by Ganymede is known’ (West ad loc). But we are repeatedly reminded that the scene with the Phrygian (1369ff.) has far fewer affinities with tragedy than with comedy, and εύριπιδαριστοφαíζεται Comedy provides the clue, specifically at Ar. Vesp. 50If. and Lys. 676ff. The reference is to the variety of equestrianism for which Ganymede is far from unknown (he was too young to have established an association with any other kind). For Innoavvr) here describes a σχῆμα ἐρωτικóν and the line means Ganymedes concubinus, Iovis supini inguini insidens et equitans, sc. inter causas fuit malorum propter Iunonis invidiam Troianis immissorum.

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2

Stevens, J. Timothy. "Ganymedes, Persephone, and Mei: The Child as Object of Desire." Dutch Crossing 13, no. 38 (August 1989): 96–109. http://dx.doi.org/10.1080/03096564.1989.11783916.

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3

Прокофьев, А. М. "Новый полорыл Coelorinchus ganymedes sp. nova из вод Полинезии (Macrouridae)." Вопросы ихтиологии 61, no. 2 (2021): 127–33. http://dx.doi.org/10.31857/s0042875221020193.

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4

Chaudhary, Zahid. "Controlling the Ganymedes: The colonial gaze in J. R. Ackerley'sHindoo holiday." South Asia: Journal of South Asian Studies 24, sup001 (January 2001): 47–57. http://dx.doi.org/10.1080/00856400108723435.

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Folgar Brea, María José. "Cuando Apolo mató a Ganymedes. El “texte .liij.” de la Epistre Othea." Medievalia 53, no. 1 (May 19, 2021): 5–23. http://dx.doi.org/10.19130/medievalia.2021.53.1.25621.

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Christine de Pizan's Epistre Othea aims to show a variety of models about what does it mean to be a perfect knight. In her book she bases on several sources, among which the Ovide moralisé is one of the most important. Thus, it´s surprising that one of the used exempla conspicuously departs from the content of this work (and others that she knew) by introducing an episode in which Apollo kills Ganymede, not only in the text itself but also in the iconographic program that accompanies it in the manuscripts. This article tries to draw attention to this unique feature in order to seek some possible explanation.

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Prokofiev, A. M. "New grenadier Coelorinchus ganymedes sp. nova from the Waters of Polynesia (Macrouridae)." Journal of Ichthyology 61, no. 2 (March 2021): 175–81. http://dx.doi.org/10.1134/s0032945221020156.

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7

Jara-Orué, H. M., and B. L. A. Vermeersen. "Tides on Jupiter's moon Ganymede and their relation to its internal structure." Netherlands Journal of Geosciences - Geologie en Mijnbouw 95, no. 2 (March 16, 2016): 191–201. http://dx.doi.org/10.1017/njg.2015.23.

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AbstractOne of the major scientific objectives of ESA's JUICE (JUpiter ICy moons Explorer) mission, which is scheduled for launch in 2022 and planned to arrive at the Jovian system in 2030, is to characterise the internal water ocean and overlying ice shell of Jupiter's largest moon Ganymede. As part of the strategy developed to realise this objective, the tidal response of Ganymede's interior will be constrained by JUICE's measurements of surface displacements (by the Ganymede Laser Altimeter (GALA) instrument) and variations in the gravitational potential (by the 3GM radio science package) due to the acting diurnal tides. Here we calculate the tidal response at the surface of Ganymede for several plausible internal configurations in order to analyse the relation between the tidal response and the geophysical parameters that characterise Ganymede's interior. Similarly to the case of Jupiter's smallest icy satellite Europa, the tidal response of Ganymede in the presence of a subsurface ocean, which could be as large as about 3.5 m in terms of the induced radial deformation, mostly depends on the structural (thickness, density) and rheological (rigidity, viscosity) properties of the ice-I shell. Nevertheless, the dependence of the tidal response on several geophysical parameters of the interior, in particular on the thickness and rigidity of the ice-I shell, does not allow for the unambiguous determination of the shell thickness from tidal measurements alone. Additional constraints could be provided by the measurement of forced longitudinal librations at the surface, as their amplitude is more sensitive to the rigidity than to the thickness of the shell.

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8

Lehmer, Owen R., David C. Catling, and Kevin J. Zahnle. "The Longevity of Water Ice on Ganymedes and Europas around Migrated Giant Planets." Astrophysical Journal 839, no. 1 (April 11, 2017): 32. http://dx.doi.org/10.3847/1538-4357/aa67ea.

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9

Downey, Brynna G., Francis Nimmo, and Isamu Matsuyama. "Inclination damping on Callisto." Monthly Notices of the Royal Astronomical Society 499, no. 1 (September 14, 2020): 40–51. http://dx.doi.org/10.1093/mnras/staa2802.

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ABSTRACT Callisto is thought to possess a subsurface ocean, which will dissipate energy due to obliquity tides. This dissipation should have damped any primordial inclination within 1 Gyr – and yet Callisto retains a present-day inclination. We argue that Callisto’s inclination and eccentricity were both excited in the relatively recent past (∼0.3 Gyr). This excitation occurred as Callisto migrated outwards according to the ‘resonance-locking’ model and passed through a 2:1 mean-motion resonance with Ganymede. Ganymede’s orbital elements were likewise excited by the same event. To explain the present-day orbital elements, we deduce a solid-body tidal k2/Q ≈ 0.05 for Callisto and a significantly lower value for Ganymede.

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10

Steinbrügge, Gregor, Teresa Steinke, Robin Thor, Alexander Stark, and Hauke Hussmann. "Measuring Ganymede’s Librations with Laser Altimetry." Geosciences 9, no. 7 (July 20, 2019): 320. http://dx.doi.org/10.3390/geosciences9070320.

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Jupiter’s moon Ganymede might be in possession of a subsurface ocean located between two ice layers. However, from Galileo data it is not possible to unambiguously infer the thickness and densities of the individual layers. The upcoming icy satellite mission JUICE (JUpiter ICy moons Explorer) will have the possibility to perform more detailed investigations of Ganymede’s interior structure with the radio science experiment 3GM and the GAnymede Laser Altimeter (GALA). Here we investigate the possibility to derive the rotational state of the outer ice shell by using topography measured by laser altimetry. We discuss two different methods to invert synthetic laser altimetry data. Method 1 is based on a spherical harmonics expansion and Method 2 solves for B-splines on a rectangular grid. While Method 1 has significant limitations due to the omission of high degrees of the global expansion, Method 2 leads to stable results allowing for an estimate of the in-orbit measurement accuracy. We estimate that GALA can measure the amplitude of Ganymede’s librations with an accuracy of 2.5–6.6 μ rad (6.6–17.4 m at the equator). This allows for determining the thickness of an elastic ice shell, if decoupled from the deeper interior by a subsurface ocean, to about an accuracy of 24–65 km.

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11

Pigni, Natalia B., Segundo Ríos-Ruiz, F. Javier Luque, Francesc Viladomat, Carles Codina, and Jaume Bastida. "Wild daffodils of the section Ganymedes from the Iberian Peninsula as a source of mesembrane alkaloids." Phytochemistry 95 (November 2013): 384–93. http://dx.doi.org/10.1016/j.phytochem.2013.07.010.

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12

Strolonga, Polyxeni. "Variations on the Myth of the Abduction of Ganymede." Yearbook of Ancient Greek Epic Online 2, no. 1 (August 23, 2018): 190–217. http://dx.doi.org/10.1163/24688487-00201007.

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Abstract This article explores the verbal and the mythological intertextuality of the archaic Greek sources that relate the abduction of Ganymede and either omit or overemphasize the compensation of horses provided by Zeus to Ganymede’s father. By employing focalization, I trace the myth’s re-presentation in different narrative contexts and I investigate its reception by Hellanicus and Apollodorus. I argue that although the myth is tailored differently according to the narrative purposes of each work, its narratological function as a hortatory analepsis and a celebratory myth is consistent.

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13

Williams, D. J., B. H. Mauk, R. W. McEntire, E. C. Roelof, T. P. Armstrong, B. Wilken, J. G. Roederer, et al. "Energetic particle signatures at Ganymede: Implications for Ganymede's magnetic field." Geophysical Research Letters 24, no. 17 (September 1, 1997): 2163–66. http://dx.doi.org/10.1029/97gl01931.

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14

Kivelson, Margaret G., Xianzhe Jia, and Krishan K. Khurana. "Medicean Moons Sailing Through Plasma Seas: Challenges in Establishing Magnetic Properties." Proceedings of the International Astronomical Union 6, S269 (January 2010): 58–70. http://dx.doi.org/10.1017/s1743921310007271.

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AbstractJupiter's moons, embedded in the magnetized, flowing plasma of Jupiter's magnetosphere, the plasma seas of the title, are fluids whose highly non-linear interactions imply complex behavior. In a plasma, magnetic fields couple widely separated regions; consequently plasma interactions are exceptionally sensitive to boundary conditions (often ill-specified). Perturbation fields arising from plasma currents greatly limit our ability to establish more than the dominant internal magnetic field of a moon. With a focus on Ganymede and a nod to Io, this paper discusses the complexity of plasma-moon interactions, explains how computer simulations have helped characterize the system and presents improved fits to Ganymede's internal field.

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15

Prokopowicz, Anna J., Sonja Rueckert, Brian S. Leander, Josée Michaud, and Louis Fortier. "Parasitic infection of the hyperiid amphipod Themisto libellula in the Canadian Beaufort Sea (Arctic Ocean), with a description of Ganymedes themistos sp. n. (Apicomplexa, Eugregarinorida)." Polar Biology 33, no. 10 (May 20, 2010): 1339–50. http://dx.doi.org/10.1007/s00300-010-0821-0.

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16

Bland, Michael T., and William B. McKinnon. "Forming Ganymede’s grooves at smaller strain: Toward a self-consistent local and global strain history for Ganymede." Icarus 245 (January 2015): 247–62. http://dx.doi.org/10.1016/j.icarus.2014.09.008.

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17

Carlson, R. W., W. D. Smythe, D. L. Matson, R. Lopes-Gautier, J. Hui, M. Segura, A. C. Ocampo, et al. "Surface Composition of the Galilean Satellites from Galileo Near-Infrared Mapping Spectroscopy." Highlights of Astronomy 11, no. 2 (1998): 1078–81. http://dx.doi.org/10.1017/s1539299600019638.

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AbstractThe Galileo Near Infrared Mapping Spectrometer (NIMS) is currently obtaining spectral maps of Jupiter’s moons to determine the composition and spatial distribution of minerals on the satellite surfaces. Sulfur dioxide, as a frost or ice, covers much of Io’s surface, except in hot volcanic areas. A weak spectral feature at 3.15 μm suggests the presence of an OH containing surface compound (hydroxide, hydrate, or water) and a broad absorption above 1 μm is reasonably attributed to iron-containing minerals, such as feldspars and pyrite. Water is the dominant molecule covering Europa’s surface, occurring as ice but also as a hydrate. The trailing side shows high concentrations of these hydrous minerals, whose identifications are not yet established. Ganymede’s surface exhibits water absorption bands, largely due to ice but hydrates are also present. A dark component is present, but with a smaller proportion compared to Callisto. Some of the non-ice features seen on Ganymede are similar to those found in Callisto’s spectra (see below). Among the icy Galilean satellites, Callisto shows the least amount of water ice, covering about 10% of the surface in patchy concentrations. Most of the surface is covered with unidentified (as yet) dark minerals. The exposed ice is often associated with impact craters, implying that the darker material exists as a blanket over more pure ice. Non-ice spectral features at 3.88, 4.03, 4.25, and 4.57 μm are present in Callisto’s spectra (and some of these appear in Ganymede’s spectra), each with different spatial distributions. Laboratory spectra suggest that the 4.25-μm feature is due to carbon dioxide which is trapped in the surface grains. The band at 4.03 μm may be due to sulfur dioxide, which probably originated from Io. Molecules containing CN, SH, SiH, and perhaps deuterated constituents are candidates for the other features, some of which could be derived from shock-heated and modified material from impacts, perhaps of carbonaceous composition. There is evidence for the presence of hydrated minerals on Callisto, based on water band shifts and shapes.

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Chela-Flores, J., A. Cicuttin, M. L. Crespo, and C. Tuniz. "Biogeochemical fingerprints of life: earlier analogies with polar ecosystems suggest feasible instrumentation for probing the Galilean moons." International Journal of Astrobiology 14, no. 3 (October 10, 2014): 427–34. http://dx.doi.org/10.1017/s1473550414000391.

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AbstractWe base our search for the right instrumentation for detecting biosignatures on Europa on the analogy suggested by the recent work on polar ecosystems in the Canadian Arctic at Ellesmere Island. In that location sulphur patches (analogous to the Europan patches) are accumulating on glacial ice lying over saline springs rich in sulphate and sulphide. Their work reinforces earlier analogies in Antarctic ecosystems that are appropriate models for possible habitats that will be explored by the European Space Agency JUpiter ICy Moons Explorer (JUICE) mission to the Jovian System. Its Jupiter Ganymede Orbiter (JGO) will include orbits around Europa and Ganymede. The Galileo orbital mission discovered surficial patches of non-ice elements on Europa that were widespread and, in some cases possibly endogenous. This suggests the possibility that the observed chemical elements in the exoatmosphere may be from the subsurface ocean. Spatial resolution calculations of Cassidy and co-workers are available, suggesting that the atmospheric S content can be mapped by a neutral mass spectrometer, now included among the selected JUICE instruments. In some cases, large S-fractionations are due to microbial reduction and disproportionation (although sometimes providing a test for ecosystem fingerprints, even though with Sim – Bosak – Ono we maintain that microbial sulphate reduction large sulphur isotope fractionation does not require disproportionation. We address the question of the possible role of oxygen in the Europan ocean. Instrument issues are discussed for measuring stable S-isotope fractionations up to the known limits in natural populations of δ34 ≈ −70‰. We state the hypothesis of a Europa anaerobic oceanic population of sulphate reducers and disproportionators that would have the effect of fractionating the sulphate that reaches the low-albedo surficial regions. This hypothesis is compatible with the time-honoured expectation of Kaplan and co-workers (going back to the 1960s) that the distribution range of 32S/34S in analysed extra-terrestrial material appears to be narrower than the isotopic ratio of H, C or N and may be the most reliable for estimating biological effects. In addition, we discuss the necessary instruments that can test our biogenic hypothesis. First of all we hasten to clarify that the last-generation miniaturized mass spectrometer we discuss in the present paper are capable of reaching the required accuracy of ‰ for the all-important measurements with JGO of the thin atmospheres of the icy satellites. To implement the measurements, we single out miniature laser ablation time-of-flight mass spectrometers that are ideal for the forthcoming JUICE probing of the exoatmospheres, ionospheres and, indirectly, surficial low-albedo regions. Ganymede's surface, besides having ancient dark terrains covering about one-third of the total surface, has bright terrains of more recent origin, possibly due to some internal processes, not excluding biological ones. The geochemical test could identify bioindicators on Europa and exclude them on its large neighbour by probing relatively recent bright terrains on Ganymede's Polar Regions.

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19

Prockter, Louise M. "Icing Ganymede." Nature 410, no. 6824 (March 2001): 25–27. http://dx.doi.org/10.1038/35065183.

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Orgel, S. "GANYMEDE AGONISTES." GLQ: A Journal of Lesbian and Gay Studies 10, no. 3 (January 1, 2004): 485–501. http://dx.doi.org/10.1215/10642684-10-3-485.

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21

Maltagliati, Luca. "Global Ganymede." Nature Astronomy 3, no. 8 (July 29, 2019): 686. http://dx.doi.org/10.1038/s41550-019-0870-4.

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22

Pommier, Anne. "Experimental investigation of the effect of nickel on the electrical resistivity of Fe-Ni and Fe-Ni-S alloys under pressure." American Mineralogist 105, no. 7 (July 1, 2020): 1069–77. http://dx.doi.org/10.2138/am-2020-7301.

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Abstract Electrical resistivity experiments were conducted on three alloys in the iron-rich side of the Fe-Ni(-S) system (Fe-5 wt% Ni, Fe-10 wt% Ni, Fe-10 wt% Ni-5 wt% S) at 4.5 and 8 GPa and up to 1900 K using the multi-anvil apparatus and the 4-electrode technique. For all samples, increasing temperature increases resistivity. At a specified temperature, Fe-Ni(-S) alloys are more resistive than Fe by a factor of about 3. Fe-Ni alloys containing 5 and 10 wt% Ni present comparable electrical resistivity values. The resistivity of Fe-Ni(-S) alloys is comparable to the one of Fe = 5 wt% S at 4.5 GPa and is about three times higher than the resistivity of Fe = 5 wt% S at 8 GPa, due to a different pressure dependence of electrical resistivity between Fe-Ni and Fe-S alloys. Based on these electrical results and experimentally determined thermal conductivity values from the literature, lower and upper bounds of thermal conductivity were calculated. For all Ni-bearing alloys, thermal conductivity estimates range between ~12 and 20 W/(m⋅K) over the considered pressure and temperature ranges. Adiabatic heat fluxes were computed for both Ganymede's core and the Lunar core, and heat flux values suggest a significant dependence to both core composition and the adiabatic temperature. Comparison with previous thermochemical models of the cores of Ganymede and the Moon suggests that some studies may have overestimated the thermal conductivity and hence, the heat flux along the adiabat in these planetary cores.

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23

Wirström, E. S., P. Bjerkeli, L. Rezac, C. Brinch, and P. Hartogh. "Effect of the 3D distribution on water observations made with the SWI." Astronomy & Astrophysics 637 (May 2020): A90. http://dx.doi.org/10.1051/0004-6361/202037609.

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Context. Characterising and understanding the atmospheres of Jovian icy moons is one of the key exploration goals of the Submillimetre Wave Instrument (SWI), which is to be flown on ESA’s Jupiter Icy Moons Explorer (JUICE) mission. Aims. The aim of this paper is to investigate how and under which conditions a 3D asymmetric distribution of the atmosphere may affect the SWI observations. In this work we target the role of phase angle for both nadir and limb geometries for unresolved and partially resolved disc observations from large distances. Methods. We adapted the LIME software package, a 3D non-local thermodynamical equilibrium radiative transfer model, to evaluate ortho-H2O populations and synthesise the simulated SWI beam spectra for different study cases of Ganymede’s atmosphere. The temperature and density vertical distributions were adopted from a previous work. The study cases presented here were selected according to the distance and operational scenarios of moon monitoring anticipated for SWI during the Jupiter phase of the JUICE mission. Results. We demonstrate that nadir and limb observations at different phase angles will modify the line amplitude and width. Unresolved observations where both absorption against surface continuum and limb emission contributes within the beam will lead to characteristic line wing emission, which may also appear in pure nadir geometry for specific phase angles. We also find that for Ganymede, the 3D non-local thermodynamical equilibrium populations are more highly excited in the upper atmosphere near the sub-solar region than they are in 1D spherically symmetric models. Finally, the 3D radiative transfer is better suited to properly simulate spectral lines for cases where density or population gradients exist along the line of sight.

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YUST, JASON. "Ganymede's Heavenly Descent." Music Analysis 39, no. 1 (March 2020): 50–84. http://dx.doi.org/10.1111/musa.12138.

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Zhan, X., and G. Schubert. "Powering Ganymede's dynamo." Journal of Geophysical Research: Planets 117, E8 (August 2012): n/a. http://dx.doi.org/10.1029/2012je004052.

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26

McGrath, Melissa A., Xianzhe Jia, Kurt Retherford, Paul D. Feldman, Darrell F. Strobel, and Joachim Saur. "Aurora on Ganymede." Journal of Geophysical Research: Space Physics 118, no. 5 (May 2013): 2043–54. http://dx.doi.org/10.1002/jgra.50122.

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27

Martinez, Juan. "Souvenirs from Ganymede." River Teeth: A Journal of Nonfiction Narrative 8, no. 2 (2007): 90–96. http://dx.doi.org/10.1353/rvt.2007.0012.

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28

Volwerk, M., X. Jia, C. Paranicas, W. S. Kurth, M. G. Kivelson, and K. K. Khurana. "ULF waves in Ganymede's upstream magnetosphere." Annales Geophysicae 31, no. 1 (January 7, 2013): 45–59. http://dx.doi.org/10.5194/angeo-31-45-2013.

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Abstract. Ganymede's mini-magnetosphere, embedded in Jupiter's larger one, sustains ULF (ultra-low frequency) waves that are analyzed here using data from two Galileo flybys that penetrate deeply into the upstream closed field line region. The magnetometer data are used to identify field line resonances, magnetopause waves and ion cyclotron waves. The plasma densities that are inferred from the interpretation of these waves are compared with the observations made by other plasma and wave experiments on Galileo and with numerical and theoretical models of Ganymede's magnetosphere.

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29

Gibson, Craig A. "Two rhetorical exercises on Ganymede in John Doxapatres’ Homiliae in Aphthonium." Byzantine and Modern Greek Studies 43, no. 02 (September 10, 2019): 181–93. http://dx.doi.org/10.1017/byz.2019.11.

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A pair of anonymous rhetorical exercises in Greek, dating perhaps to the eleventh century, contain a refutation and a confirmation of the myth of Ganymede, in which the young Trojan shepherd is abducted by Zeus in the form of an eagle to live with him in heaven. This article analyses the opposing arguments about divinity and sexuality in the two exercises, argues that they contain a unique aetiological account of the violet, and situates them in the reception history of Ganymede.

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Tittemore, W. C. "Chaotic Motion of Europa and Ganymede and the Ganymede-Callisto Dichotomy." Science 250, no. 4978 (October 12, 1990): 263–67. http://dx.doi.org/10.1126/science.250.4978.263.

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Lari, Giacomo, Melaine Saillenfest, and Marco Fenucci. "Long-term evolution of the Galilean satellites: the capture of Callisto into resonance." Astronomy & Astrophysics 639 (July 2020): A40. http://dx.doi.org/10.1051/0004-6361/202037445.

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Context. The Galilean satellites have very complex orbital dynamics due to the mean-motion resonances and the tidal forces acting in the system. The strong dissipation in the couple Jupiter–Io is spread to all the moons involved in the so-called Laplace resonance (Io, Europa, and Ganymede), leading to a migration of their orbits. Aims. We aim to characterize the future behavior of the Galilean satellites over the Solar System lifetime and to quantify the stability of the Laplace resonance. Tidal dissipation permits the satellites to exit from the current resonances or be captured into new ones, causing large variation in the moons’ orbital elements. In particular, we want to investigate the possible capture of Callisto into resonance. Methods. We performed hundreds of propagations using an improved version of a recent semi-analytical model. As Ganymede moves outwards, it approaches the 2:1 resonance with Callisto, inducing a temporary chaotic motion in the system. For this reason, we draw a statistical picture of the outcome of the resonant encounter. Results. The system can settle into two distinct outcomes: (A) a chain of three 2:1 two-body resonances (Io–Europa, Europa–Ganymede, and Ganymede–Callisto), or (B) a resonant chain involving the 2:1 two-body resonance Io–Europa plus at least one pure 4:2:1 three-body resonance, most frequently between Europa, Ganymede, and Callisto. In case A (56% of the simulations), the Laplace resonance is always preserved and the eccentricities remain confined to small values below 0.01. In case B (44% of the simulations), the Laplace resonance is generally disrupted and the eccentricities of Ganymede and Callisto can increase up to about 0.1, making this configuration unstable and driving the system into new resonances. In all cases, Callisto starts to migrate outward, pushed by the resonant action of the other moons. Conclusions. From our results, the capture of Callisto into resonance appears to be extremely likely (100% of our simulations). The exact timing of its entrance into resonance depends on the precise rate of energy dissipation in the system. Assuming the most recent estimate of the dissipation between Io and Jupiter, the resonant encounter happens at about 1.5 Gyr from now. Therefore, the stability of the Laplace resonance as we know it today is guaranteed at least up to about 1.5 Gyr.

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32

Kivelson, M. G., J. Warnecke, L. Bennett, S. Joy, K. K. Khurana, J. A. Linker, C. T. Russell, R. J. Walker, and C. Polanskey. "Ganymede's magnetosphere: Magnetometer overview." Journal of Geophysical Research: Planets 103, E9 (August 1, 1998): 19963–72. http://dx.doi.org/10.1029/98je00227.

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33

Williams, D. J. "Ganymede's ionic radiation belts." Geophysical Research Letters 28, no. 19 (October 1, 2001): 3793–96. http://dx.doi.org/10.1029/2001gl013353.

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Cessateur, Gaël, Jean Lilensten, Mathieu Barthélémy, Thierry Dudok de Wit, Cyril Simon Wedlund, Guillaume Gronoff, Hélène Ménager, and Matthieu Kretzschmar. "Photoabsorption in Ganymede’s atmosphere." Icarus 218, no. 1 (March 2012): 308–19. http://dx.doi.org/10.1016/j.icarus.2011.11.025.

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35

Eviatar, Aharon, Vytenis M. Vasyliūnas, and Donald A. Gurnett. "The ionosphere of Ganymede." Planetary and Space Science 49, no. 3-4 (March 2001): 327–36. http://dx.doi.org/10.1016/s0032-0633(00)00154-9.

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36

Pappalardo, Robert T., and Geoffrey C. Collins. "Strained craters on Ganymede." Journal of Structural Geology 27, no. 5 (May 2005): 827–38. http://dx.doi.org/10.1016/j.jsg.2004.11.010.

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37

Putnam, Michael C. J. "Ganymede and Virgilian Ekphrasis." American Journal of Philology 116, no. 3 (1995): 419. http://dx.doi.org/10.2307/295330.

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38

Moore, Jeffrey M., and Michael C. Malin. "Dome craters on Ganymede." Geophysical Research Letters 15, no. 3 (March 1988): 225–28. http://dx.doi.org/10.1029/gl015i003p00225.

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39

Palguta, Jennifer, John D. Anderson, Gerald Schubert, and William B. Moore. "Mass anomalies on Ganymede." Icarus 180, no. 2 (February 2006): 428–41. http://dx.doi.org/10.1016/j.icarus.2005.08.020.

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40

Cousins, A. D. "Daphne Du Maurier's GANYMEDE." Explicator 71, no. 3 (July 2013): 218–20. http://dx.doi.org/10.1080/00144940.2013.811397.

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41

Grodent, Denis, Bertrand Bonfond, Aikaterini Radioti, Jean-Claude Gérard, Xianzhe Jia, Jonathan D. Nichols, and John T. Clarke. "Auroral footprint of Ganymede." Journal of Geophysical Research: Space Physics 114, A7 (July 2009): n/a. http://dx.doi.org/10.1029/2009ja014289.

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42

Stevenson, David J. "When Galileo met Ganymede." Nature 384, no. 6609 (December 1996): 511–12. http://dx.doi.org/10.1038/384511a0.

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43

Fatemi, S., A. R. Poppe, K. K. Khurana, M. Holmström, and G. T. Delory. "On the formation of Ganymede's surface brightness asymmetries: Kinetic simulations of Ganymede's magnetosphere." Geophysical Research Letters 43, no. 10 (May 20, 2016): 4745–54. http://dx.doi.org/10.1002/2016gl068363.

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44

Zarka, P., M. S. Marques, C. Louis, V. B. Ryabov, L. Lamy, E. Echer, and B. Cecconi. "Jupiter radio emission induced by Ganymede and consequences for the radio detection of exoplanets." Astronomy & Astrophysics 618 (October 2018): A84. http://dx.doi.org/10.1051/0004-6361/201833586.

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By analysing a database of 26 yr of observations of Jupiter with the Nançay Decameter Array, we unambiguously identify the radio emissions caused by the Ganymede–Jupiter interaction. We study the energetics of these emissions via the distributions of their intensities, duration, and power, and compare them to the energetics of the Io–Jupiter radio emissions. This allows us to demonstrate that the average emitted radio power is proportional to the Poynting flux from the rotating Jupiter’s magnetosphere intercepted by the obstacle. We then generalize this result to the radio-magnetic scaling law that appears to apply to all plasma interactions between a magnetized flow and an obstacle, magnetized or not. Extrapolating this scaling law to the parameter range corresponding to hot Jupiters, we predict large radio powers emitted by these objects, that should result in detectable radio flux with new-generation radiotelescopes. Comparing the distributions of the durations of Ganymede–Jupiter and Io–Jupiter emission events also suggests that while the latter results from quasi-permanent Alfvén wave excitation by Io, the former likely results from sporadic reconnection between magnetic fields Ganymede and Jupiter, controlled by Jupiter’s magnetic field geometry and modulated by its rotation.

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45

Tripathi, Arvind K., Rajendra P. Singhal, and Onkar N. Singh II. "The generation of Ganymede's diffuse aurora through pitch angle scattering." Annales Geophysicae 35, no. 2 (February 22, 2017): 239–52. http://dx.doi.org/10.5194/angeo-35-239-2017.

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Abstract. Diffuse auroral intensities of neutral atomic oxygen OI λ1356 Å emission on Ganymede due to whistler mode waves are estimated. Pitch angle diffusion of magnetospheric electrons into the loss cone due to resonant wave–particle interaction of whistler mode waves is considered, and the resulting electron precipitation flux is calculated. The analytical yield spectrum approach is used for determining the energy deposition of electrons precipitating into the atmosphere of Ganymede. It is found that the intensities (4–30 R) calculated from the precipitation of magnetospheric electrons observed near Ganymede are inadequate to account for the observational intensities (≤ 100 R). This is in agreement with the conclusions reached in previous works. Some acceleration mechanism is required to energize the magnetospheric electrons. In the present work we consider the heating and acceleration of magnetospheric electrons by electrostatic waves. Two particle distribution functions (Maxwellian and kappa distribution) are used to simulate heating and acceleration of electrons. Precipitation of a Maxwellian distribution of electrons can produce about 70 R intensities of OI λ1356 Å emission for electron temperature of 150 eV. A kappa distribution can also yield a diffuse auroral intensity of similar magnitude for a characteristic energy of about 100 eV. The maximum contribution to the estimated intensity results from the dissociative excitation of O2. Contributions from the direct excitation of atomic oxygen and cascading in atomic oxygen are estimated to be only about 1 and 2 % of the total calculated intensity, respectively. The findings of this work are relevant for the present JUNO and future JUICE missions to Jupiter. These missions will provide new data on electron densities, electron temperature and whistler mode wave amplitudes in the magnetosphere of Jupiter near Ganymede.

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Mura, A., A. Adriani, J. E. P. Connerney, S. Bolton, F. Altieri, F. Bagenal, B. Bonfond, et al. "Juno observations of spot structures and a split tail in Io-induced aurorae on Jupiter." Science 361, no. 6404 (July 5, 2018): 774–77. http://dx.doi.org/10.1126/science.aat1450.

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Jupiter’s aurorae are produced in its upper atmosphere when incoming high-energy electrons precipitate along the planet’s magnetic field lines. A northern and a southern main auroral oval are visible, surrounded by small emission features associated with the Galilean moons. We present infrared observations, obtained with the Juno spacecraft, showing that in the case of Io, this emission exhibits a swirling pattern that is similar in appearance to a von Kármán vortex street. Well downstream of the main auroral spots, the extended tail is split in two. Both of Ganymede’s footprints also appear as a pair of emission features, which may provide a remote measure of Ganymede’s magnetosphere. These features suggest that the magnetohydrodynamic interaction between Jupiter and its moon is more complex than previously anticipated.

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Belgacem, Ines, Frédéric Schmidt, and Grégory Jonniaux. "Regional study of Ganymede’s photometry." Icarus 369 (November 2021): 114631. http://dx.doi.org/10.1016/j.icarus.2021.114631.

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Strobel, Darrell F. "Comparative Planetary Atmospheres of the Galilean Satellites." Highlights of Astronomy 13 (2005): 894–95. http://dx.doi.org/10.1017/s1539299600017433.

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We know that each of the Galilean satellites of Jupiter has a tenuous atmosphere by terrestrial standards. Io’s SO2 equatorial atmosphere and, perhaps, Callisto’s atmosphere inferred from its large ionospheric densities are measured in nanobars, whereas the atmospheres of Europa and Ganymede produced by ion sputtering of the water ice surfaces only reach picobar pressures and are comprised mostly of O2. Io’s polar atmosphere is probably an order of magnitude less dense than its equatorial atmosphere. Europa and Ganymede have O2 atmospheres with column densities in the range of (1-10)×1014cm−2. These atmospheres, on the basis of their inferred production and loss rates, are estimated to have short residence times of ~2-3 days.

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Pappalardo, Robert T. "Geology and Composition of the Icy Galilean Satellites." Highlights of Astronomy 12 (2002): 619–24. http://dx.doi.org/10.1017/s1539299600014416.

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AbstractAnalysis of data from the Galileo spacecraft continues to provide significant advances in our understanding of the geology and composition of Jupiter’s icy Galilean satellites Callisto, Ganymede, and Europa.

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Forni, O., P. Thomas, and G. P. Masson. "Geologie et tectonique de Ganymede." Bulletin de la Société Géologique de France III, no. 1 (January 1, 1987): 95–106. http://dx.doi.org/10.2113/gssgfbull.iii.1.95.

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