The Dual Sources of Io's Sodium Clouds

Wilson, J. K.; Mendillo, M.; Baumgardner, Jeffrey; Schneider, Nicholas M.; Trauger, John T.; Flynn, Brian

doi:10.1006/icar.2002.6821

Cited by 55 publications

(63 citation statements)

References 52 publications

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“…To date the focus has been on the ions formed and accelerated in the corona. However, the ions dragged out of the atmosphere, often called "ionospheric outflow" (e.g., Fox 1997;Ma and Nagy 2007) are critically important to atmospheric loss and heating at Io (Wilson et al 2002;Mendillo et al 2007) and, likely, at Titan (Johnson 2008). Ions that are swept down the tail of the interaction region are an important atmospheric loss process.…”

Section: Energy Deposition Of Pick-up Ionsmentioning

confidence: 99%

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

2008

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We discuss here the energy deposition of solar FUV, EUV and X-ray photons, energetic auroral particles, and pickup ions. Photons and the photoelectrons that they produce may interact with thermospheric neutral species producing dissociation, ionization, excitation, and heating. The interaction of X-rays or keV electrons with atmospheric neutrals may produce core-ionized species, which may decay by the production of characteristic X-rays or Auger electrons. Energetic particles may precipitate into the atmosphere, and their collisions with atmospheric particles also produce ionization, excitation, and heating, and auroral emissions. Auroral energetic particles, like photoelectrons, interact with the atmospheric species through discrete collisions that produce ionization, excitation, and heating of the ambient electron population. Auroral particles are, however, not restricted to the sunlit regions. They originate outside the atmosphere and are more energetic than photoelectrons, especially at magnetized planets. The spectroscopic analysis of auroral emissions is discussed here, along with its relevance to precipitating particle diagnostics. Atmospheres can also be modified by the energy deposited by the incident pickup ions with energies of eV's to MeV's; these particles may be of solar wind origin, or from a magnetospheric plasma. When the modeling of the energy deposition of the plasma is calculated, the subsequent modeling of the atmospheric processes, such as chemistry, emission, and the fate of hot recoil particles produced is roughly independent of the exciting radiation. However, calculating the spatial distribution of the energy deposition versus depth into the atmosphere produced by an incident plasma is much more complex than is the calculation of the solar excitation profile. Here, the nature of the energy deposition processes by the incident plasma are described as is the fate of the hot recoil particles produced by exothermic chemistry and by knock-on collisions by the incident ions.

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Section: Energy Deposition Of Pick-up Ionsmentioning

confidence: 99%

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

2008

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“…It is worth noting that, in order to significantly affect the light-induced asymmetry in the line profile, the absolute value |δ 4 | of detuning must be larger than the natural linewidth Γ, i.e., according to Equation (9), it is necessary that Ω 3 exceeds the saturation threshold:…”

Section: Cyclic Transitions Treatment: Modeling and Discussionmentioning

confidence: 99%

“…The investigation of these sodium clouds is needed for better understanding of the interaction between Io's atmosphere and Jovian magnetosphere [9] and of processes in the Jovian environment [10].…”

Section: Introductionmentioning

confidence: 99%

Nonlinear Spectroscopy of Alkali Atoms in Cold Medium of Astrophysical Relevance

Efimov

Bruvelis

Безуглов

et al. 2017

Atoms

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Abstract:The time-dependent population dynamics of hyperfine (HF) sublevels of n 2 p 3/2 atomic states upon laser excitation in a cold medium of alkali atoms is examined. We demonstrate some peculiarities of the absorption HF multiplet formation in D2-line resulting from a long interaction time (∼200 µs) interaction between light and Na (n = 3) and Cs (n = 6) atoms in a cold and slow sub-thermal (T ∼ 1K) beam. We analytically describe a number of D2-line-shape effects that are of interest in spectroscopic studies of cold dusty white dwarfs: broadening by optical pumping, intensity redistribution within components of D2-line HF multiplet for partially closed transitions and asymmetry of absorption lines induced by AC Stark shifts for cyclic transitions.

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“…The material interior to Io's orbit, which has a Keplerian orbital velocity larger than Io's, moves ahead of Io forming the predominantly leading cloud; the trailing cloud does not form since the sodium moving slower from Io was ionized by the plasma. Neutralization of Na + pick-up ions created in Io's atmosphere is revealed through a jet of sodium escaping from the near surface-atmosphere (Burger et al 1999;Wilson et al 2002). The escape of molecular sodium-bearing ions from Io is revealed through the "stream" feature, a long narrow cloud of neutral Na formed from the dissociative recombination of ions in the Io plasma torus (Schneider et al 1991b).…”

Section: Characteristics Of Io's Atmospherementioning

confidence: 98%

Atmospheric/Exospheric Characteristics of Icy Satellites

et al. 2010

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The atmospheres/exospheres of icy satellites greatly vary from one to the next in terms of density, composition, structure or steadiness. Titan is the only icy satellite with a dense atmosphere comparable in many ways to that of the Earth's atmosphere. Titan's atmosphere prevents the surface from direct interaction with the plasma environment, but gives rise to Earth-like exchanges of energy, matter and momentum. The atmospheres of other satellites are tenuous. Enceladus' atmosphere manifests itself in a large water vapor plume emanating from surface cracks near the south pole. Io's SO 2 atmosphere originates from volcanoes. Europa's tenuous O 2 atmosphere is produced by intense radiation bombardment. This chapter reviews the characteristics of the atmospheres of Titan, Enceladus, Io and Europa based on observations. A. Coustenis ( ) LESIA, Observatoire de Paris-Meudon, 5, pl. Jules Janssen,

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The Dual Sources of Io's Sodium Clouds

Cited by 55 publications

References 52 publications

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

Nonlinear Spectroscopy of Alkali Atoms in Cold Medium of Astrophysical Relevance

Atmospheric/Exospheric Characteristics of Icy Satellites

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