Europa and Ganymede's Water-Product Exospheres

The curves all have the same general shape: the velocity of expansion slows down until the cavity reaches its maximum depth H max at a time T max , which both seem to increase with

Vapor-liquid equilibrium (VLE) data over a wide range of pressures, temperatures and concentrations of the various solvents used for acid gas removal are

The prob- lem described here directly relates to planetary sounding if we assume incident fields to be the radar sources and if we let ∂Ω conforms locally with the plan- etary

This model is presented in Section 2 and we show in Section 3 how the enhanced non-maxwellian tails in the electron VDF (simulated with Lorentzian VDFs) contribute to

A collisionless thermal plasma trapped in a di- pole magnetic field can be described as a superposi- tion of an exospheric distribution (ballistic and escaping

Our study uses the radio emission simulator ExPRES [Hess et al., 2008, section 2] which allows us to search for Jupiter decametric emissions controlled by Io, Europa, Ganymede,

in the source of the radio emission, 4 to 6 seconds, is lower than the time spent cross- ing the magnetic field lines connected to the Ganymede’s tail footprint (18 seconds, Sza- lay

The calculated values were predicted to decrease with increasing pressure, due to an increase of the total rate constant arising from more efficient complex