Jupiter: The Planet, Satellites and Magnetosphere

By R. Beebe. 2005

389 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/25c670ae8502e141783088b2b39a4aa49637267c

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In Astronomy and Astrophysics

Citations in the corpus

Formation of Jets and Equatorial Superrotation on Jupiter (2008, background): “The zonal flow in Jupiter’s upper troposphere has been inferred by tracking cloud features, which move with the horizontal flow in the layer between about 0.5 and 1 bar atmospheric pressure (Ingersoll et al. 2004; West et al. 2004; Vasavada and Showman 2005).”
High-Resolution Submillimeter Constraints on Circumstellar Disk Structure (2006, background): “…Udry et al. 2007) and their host stars (Santos et al. 2001; Fischer &Valenti 2005), as well as via the internal structure and composition of the giant planets (Lunine et al. 2004; Guillot 2005) and various aspects of the populations of smaller bodies (e.g., Luu & Jewitt 2002) in the solar system.”
Response of Jupiter's and Saturn's auroral activity to the solar wind (2009, background): “…compared with auroral emissions from the magnetic footprints of the satellites and theoretical modeling have demonstrated that the main auroral oval maps along the field to a distance about 20–30 Jovian radii (RJ), in the middle magnetosphere far from the solar wind boundary [Clarke et al., 2004].”
Constraints on Deep-seated Zonal Winds Inside Jupiter and Saturn (2007, background): “Hydrogen cannot undergo a phase change at that radius (Guillot et al. 2004).”
The Interior Structure, Composition, and Evolution of Giant Planets (2009, background): “We note that if the H/He envelope were wholly 10× solar in metallicity, the increased molecular weight of the H/He-dominated envelope would entirely negate this high-opacity effect (Hansen & Barman 2007; Guillot 2008).”
The escape of heavy atoms from the ionosphere of HD209458b. I. A photochemical–dynamical model of the thermosphere (2012, background): “General dependency433 We note that the thermal structure in the upper atmospheres of the giant434 planets in the solar system is not very well understood despite modeling and435 observations that are far more extensive than those available for extrasolar436 planets (e.g., Yelle and Miller, 2004).”
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, background): “However, there are several tens of Earth masses of “metals” (molecules heavier than H and He) in Jupiter (Guillot, 2005) and it is possible that part or even most of its primordial core has been eroded and dissolved into the atmosphere (Guillot et al., 2004; Wilson and Militzer, 2012).”
Mass-Radius Relationships for Solid Exoplanets (2007, methodology): “We define water planets to be solid planets with > 25% H2O by mass. Jupiter’s moons Ganymede and Callisto would be water planets by this definition10.”
Plasma interactions of exoplanets with their parent star and associated radio emissions (2006, background): “5/d 2 × (1 + (f − 1)/d) Bφ = Br × Ωd/V Btot = (B 2 r + B 2 φ) 1/2 (11)”
Energetic ion acceleration in Saturn's magnetotail: Substorms at Saturn? (2005, background): “, McPherron, 1995], while the dynamics of Jupiter’s magnetosphere is dominated by internal energy sources, primarily the rotational energy of Jupiter’s very strong magnetic field and the dense plasma contained by it [Bagenal et al., 2004]. Energetic particles are suddenly accelerated and/or heated i”
Dusty plasma effects in Saturn's magnetosphere (2004, background): “…populations: impact-generated dust clouds surrounding the Galilean satellites and tenuous dust populations between moons, as well as captured interplanetary RG4002 Horányi et al.: DUSTY PLASMAS AT SATURN 8 of 20 RG4002 dust particles (discussed in section 4.2) [Krüger et al., 2003a, 2003b, 2004].”