A Turbulent Heating Model Combining Diffusion and Advection Effects for Giant Planet Magnetospheres

  title={A Turbulent Heating Model Combining Diffusion and Advection Effects for Giant Planet Magnetospheres},
  author={C. S. Ng and Bishwa Neupane and Peter A. Delamere and Peter Damiano},
  journal={Geophysical Research Letters},
The ion temperature of the magnetospheres of Jupiter and Saturn was observed to increase substantially from about 10 to 30 planet radii. Different heating mechanisms have been proposed to explain such observations, including a heating model for Jupiter based on MHD turbulence with flux-tube diffusion. More recently, an MHD turbulent heating model based on advection was shown to also explain the temperature increase at Jupiter and Saturn. We further develop this turbulent heating model by… 

Figures from this paper


Radial Transport and Plasma Heating in Jupiter's Magnetodisc
The ion temperature of the magnetosphere of Jupiter derived from Galileo PLS data was observed to increase by about an order of magnitude from 10 to 40 Jupiter radii. This suggests the presence of
Magnetotail structure of the giant magnetospheres: Implications of the viscous interaction with the solar wind
[1] The internal sources of plasma in the giant magnetospheres of Jupiter and Saturn affect magnetospheric dynamics in terms of magnetosphere-ionosphere coupling and auroral current systems, as well
Turbulent Heating of Jupiter's Middle Magnetosphere
We give a possible explanation for the high ion temperatures of ~108 K measured in the middle magnetosphere of Jupiter. In the absence of a significant heat source, much lower temperatures are
Local time dependence of turbulent magnetic fields in Saturn's magnetodisc: SATURN'S TURBULENT MAGNETODISC
Net plasma transport in magnetodiscs around giant planets is outward. Observations of plasma temperature have shown that the expanding plasma is heating nonadiabatically during this process.
Survey of thermal plasma ions in Saturn's magnetosphere utilizing a forward model
The Cassini Plasma Spectrometer instrument gathered thermal ion data at Saturn from 2004 to 2012, predominantly observing water group ions and protons. Plasma parameters, with uncertainties, for
Flow of mass and energy in the magnetospheres of Jupiter and Saturn
[1] We present simple models of the plasma disks surrounding Jupiter and Saturn based on published measurements of plasma properties. We calculate radial profiles of the distribution of plasma mass,
Solar wind interaction with Jupiter's magnetosphere
[1] We present a review of observations and theories of the dynamics of Jupiter's magnetosphere from Pioneer to New Horizons. We suggest that Jupiter's solar wind–driven magnetospheric flows are due
Kolmogorov versus Iroshnikov-Kraichnan spectra: Consequences for ion heating in the solar wind
[1] Whether the phenomenology governing MHD turbulence is Kolmogorov or Iroshnikov-Kraichnan (IK) remains an open question, theoretically as well as observationally. The ion heating profile observed
A 1-D model of physical chemistry in Saturn's inner magnetosphere
[1] Water vapor spewed out of Enceladus' geysers spreads across the Saturn system through dissociation, charge exchange, and neutral-neutral collisions. The combined effects of impact ionization by