Magnetospheric {ULF} Activity as a Function of Solar Wind Conditions: Toward a Quantitative Model of Radial Diffusion in the Magnetosphere

Details Magnetospheric {ULF} Activity as a Function of Solar Wind Conditions: Toward a Quantitative Model of Radial Diffusion in the Magnetosphere Magnetospheric {ULF} Activity as a Function of Solar Wind Conditions: Toward a Quantitative Model of Radial Diffusion in the Magnetosphere

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm13e..06e&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM13E-06

Physics

7807 Charged Particle Motion And Acceleration, 7836 Mhd Waves And Instabilities (2149, 2752, 6050), 7845 Particle Acceleration, 7867 Wave/Particle Interactions (2483, 6984), 7984 Space Radiation Environment

Scientific paper

Magnetospheric ULF waves, with frequencies in the mHz range, are known to efficiently energize and transport relativistic electrons in the radiation belts through resonant interactions leading to enhanced rates of radial diffusion. However, the global occurrence and physical characteristics of the waves driving the transport, and the resulting rates of radial diffusion, are not well-characterized in terms of the solar wind conditions responsible for the ULF activity. In this effort we drive global MHD simulations of the magnetosphere using an idealized set of solar wind conditions, based on statistical characterizations of the solar wind pressure (and its variations) as a function of solar wind velocity. The simulated ULF wave distributions are analyzed as a function of radial position and global mode structure within the magnetosphere. By applying interpolation techniques to the resulting wave distributions, we create 'synthetic' maps of ULF activity as a function of solar wind velocity. We compare the synthetic rates of radial diffusion to commonly-used empirical diffusion coefficients, and to those derived from simulations driven by `real' solar wind conditions (observed by upstream solar wind monitors) representing CME- and CIR-driven storms. These comparisons are used to investigate the feasibility of using synthetic, solar wind-driven ULF maps to quantify rates of radial diffusion for real magnetospheric events.

Affiliated with

Also associated with

No associations

Rating

Magnetospheric {ULF} Activity as a Function of Solar Wind Conditions: Toward a Quantitative Model of Radial Diffusion in the Magnetosphere does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Magnetospheric {ULF} Activity as a Function of Solar Wind Conditions: Toward a Quantitative Model of Radial Diffusion in the Magnetosphere, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnetospheric {ULF} Activity as a Function of Solar Wind Conditions: Toward a Quantitative Model of Radial Diffusion in the Magnetosphere will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1421281