TY - GEN
T1 - Data-Driven Representations of Ion-Kinetic Distribution Functions
AU - Bowen, Trevor A.
AU - Chandran, Benjamin D.G.
AU - Klein, Kristopher G.
AU - Mallet, Alfred
AU - Bale, Stuart D.
AU - Squire, Jonathan
AU - Verniero, Jaye
N1 - Publisher Copyright:
© 2023 International Union of Radio Science.
PY - 2023
Y1 - 2023
N2 - Collisionless processes, such as wave particle interactions, are key to understanding the energy transfer in plasma environments. While collisional interactions are known to result in a distribution of particle velocities close to a thermal Maxwell-Boltzmann distribution, wave-particle interactions produce distribution functions that may diverge significantly from thermal equilibrium. Correct measurement and representation of non-thermal features is key to understanding the collisionless wave-particle interactions and how they shape plasma distributions. Here, we present and expand on methods (Polynomial interpolation, radial basis functions) used to approximate ion distribution functions observed by Parker Solar Probe. These non-parametric representations of the observed distributions can be used to understand instability growth rates and resonant heating of the solar wind plasma.
AB - Collisionless processes, such as wave particle interactions, are key to understanding the energy transfer in plasma environments. While collisional interactions are known to result in a distribution of particle velocities close to a thermal Maxwell-Boltzmann distribution, wave-particle interactions produce distribution functions that may diverge significantly from thermal equilibrium. Correct measurement and representation of non-thermal features is key to understanding the collisionless wave-particle interactions and how they shape plasma distributions. Here, we present and expand on methods (Polynomial interpolation, radial basis functions) used to approximate ion distribution functions observed by Parker Solar Probe. These non-parametric representations of the observed distributions can be used to understand instability growth rates and resonant heating of the solar wind plasma.
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U2 - 10.23919/URSIGASS57860.2023.10265538
DO - 10.23919/URSIGASS57860.2023.10265538
M3 - Conference contribution
AN - SCOPUS:85175181132
T3 - 2023 35th General Assembly and Scientific Symposium of the International Union of Radio Science, URSI GASS 2023
BT - 2023 35th General Assembly and Scientific Symposium of the International Union of Radio Science, URSI GASS 2023
PB - Institute of Electrical and Electronics Engineers Inc.
T2 - 35th General Assembly and Scientific Symposium of the International Union of Radio Science, URSI GASS 2023
Y2 - 19 August 2023 through 26 August 2023
ER -