@article{discovery120191,
          number = {14},
            year = {2005},
           month = {June},
         journal = {Geophysical Research Letters},
       publisher = {AMER GEOPHYSICAL UNION},
          volume = {32},
           title = {Evidence for rotationally driven plasma transport in Saturn's magnetosphere},
            note = {Copyright 2005 by the American Geophysical Union},
          author = {Hill, TW and Rymer, AM and Burch, JL and Crary, FJ and Young, DT and Thomsen, MF and Delapp, D and Andre, N and Coates, AJ and Lewis, GR},
             url = {http://dx.doi.org/10.1029/2005GL022620},
            issn = {0094-8276},
        keywords = {Io torus, Jovian magnetosphere, Jupiters inner, Interchange, Corotation, Signatures},
        abstract = {{{[}} 1] Radial convective transport of plasma in a rotation-dominated magnetosphere implies alternating longitudinal sectors of cooler, denser plasma moving outward and hotter, more tenuous plasma moving inward. The Cassini Plasma Spectrometer ( CAPS) has provided dramatic new evidence of this process operating in the magnetosphere of Saturn. The inward transport of hot plasma is accompanied by adiabatic gradient and curvature drift, producing a V-shaped dispersion signature on a linear energy-time plot. Of the many (similar to 100) such signatures evident during the first two Cassini orbits, we analyze a subset ( 48) that are sufficiently isolated to allow determination of their ages, widths, and injection locations. Ages are typically {\ensuremath{<}} 10.8 hr ( Saturn's rotation period) but range up to several rotation periods. Widths are typically {\ensuremath{<}} 1 RS ( Saturn's radius) but range up to several RS. Injection locations are randomly distributed in local time and in Saturnian longitude. The apex of the V sometimes coincides with a localized density cavity in the cooler background plasma, and usually coincides with a localized diamagnetic depression of the magnetic field strength. These signatures are fully consistent with the convective motions that are expected to result from the centrifugal interchange instability.}
}