HR: 1340h
AN: SH13A-1103    [Abstracts]
TI: Technique of Measuring Taylor Microscale
AU: * Chuychai, P
EM: paeng@bartol.udel.edu
AF: Bartol Research Institute, Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, United States
AU: Weygand, J M
EM: jweygand@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095, United States
AU: Matthaeus, W H
EM: whm@udel.edu
AF: Bartol Research Institute, Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, United States
AU: Dasso, S
EM: sdasso@iafe.uba.ar
AF: Instituto de Astronomia y Fisica del Espacio and Departamento de Fisica, Universidad de Buenos Aires, Buenos Aires, 1428, Argentina
AU: Smith, C W
EM: Charles.Smith@unh.edu
AF: Institute for Earth, Oceans and Space, University of New Hamshire, Durham, NH 03824, United States
AU: Kivelson, M
EM: mkivelson@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095, United States
AB: We present the method to measure Taylor microscale from the discrete data which is useful for the data from the spacecraft. To study how well the method works, we construct the discrete data from known power spectrum. We model the power spectrum as the frequency in inertial range is proportional to -5/3 slope and the power law index q at dissipation range can be varied. From the data, we compute the second order structure function and correlation function. To obtain the Taylor microscale, we use the technique of the Richardson extrapolation from parabolic fitting of the correlation function. We found that the error of Taylor microscale depend on the steepening at the dissipation range and the resolution of the data. Since in this study we can compute the solution of the Taylor microscale from each spectrum, we produce the correction ratio to help correcting the Taylor microscale from extrapolation method. Finally, we apply this technique to the magnetic field data from the spacecraft in the solar wind.
DE: 7594 Instruments and techniques
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting