Bulletin of the American Physical Society
64th Annual Meeting of the APS Division of Plasma Physics
Volume 67, Number 15
Monday–Friday, October 17–21, 2022; Spokane, Washington
Session NP11: Poster Session V: In-Person, Hall A (9:30-11:00am) and Virtual Poster Presentations (11:15am-12:30pm)
MFE: Stellerators
HED: High Energy Density
BEAMS: Short Pulse Laser Plasmas
HED: Short Pulse Laser Plasma
SPACE: Space Plasmas
9:30 AM - 12:30 PM
Wednesday, October 19, 2022
Room: Exhibit Hall A and Online
Abstract: NP11.00147 : Heliospheric Magnetic Fields Generated by Solar Wind Current Fluctuations.*
Presenter:
Charles F Driscoll
(University of California, San Diego)
Author:
Charles F Driscoll
(University of California, San Diego)
1) Variable-duration spectral analyses clearly show that there is no persistent magnetic "spiral" at 1AU, merely the statistical fluctuations of "random walk" dynamics. Similarly, spectral components B(f) above f≅50μHz clearly show the √N scaling of random noise.
2) Pervasive dynamical "arc" events are observed on time-scales 10^3< τ < 10^5 sec, presumably related to spiky "switchbacks" observed by PSP at 0.1AU. The dynamics appears as Bθ-Bz, Br-Bz, and Br-Bθ temporal arcs, with occurrence rates differing by direction. The observed dynamics is modeled by finite-duration "pinched" +/- current filaments, representing charge non-neutrality of 10^-5 in the e-/p+ flux over distances d≅10^3Mm and times τ≅2000s.
3) The Br and Bθ (but not Bz) spectral components at the solar rotation frequency frot are exceptional, varying between 0% and 30% (average 17%) of the total Brms^2 magnetic energy. In only these variable components (arising from variable surface emission) is there a Br-Bθ anti-correlation, which is traditionally mis-interpreted as the magnetic spiral. NNP.ucsd.edu/Solar/
*Supported by UCSD and AFOSR
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