자료유형  

 학위논문

Control Number  

0017162418

International Standard Book Number  

9798382829760

Dewey Decimal Classification Number  

523

Main Entry-Personal Name  

Sioulas, Nikolaos.

Publication, Distribution, etc. (Imprint  

[S.l.] : University of California, Los Angeles., 2024

Publication, Distribution, etc. (Imprint  

Ann Arbor : ProQuest Dissertations & Theses, 2024

Physical Description  

317 p.

General Note  

Source: Dissertations Abstracts International, Volume: 85-12, Section: B.

General Note  

Advisor: Velli, Marco C. M.

Dissertation Note  

Thesis (Ph.D.)--University of California, Los Angeles, 2024.

Summary, Etc.  

요약As the solar wind expands into the interplanetary medium, its turbulent nature changes dramatically. The synergy of the Parker Solar Probe, Solar Orbiter, and WIND missions is enabling hitherto impossible studies of plasma turbulence throughout the inner heliosphere, ranging from within the Alfven region out to Earth's orbit at 1 astronomical unit (AU). Understanding the dynamic evolution and transport of turbulent fluctuations from the corona into the heliosphere is fundamental to heliospheric science and can offer insights into several important unresolved problems in the field, including the coronal heating mechanism, the acceleration and non-adiabatic expansion of the solar wind, and the scattering and acceleration of energetic particles by turbulent fluctuations. The principal scientific aim of this thesis is to harness these observations and provide robust observational constraints on theoretical models and numerical simulations of Alfvenic turbulence by offering insights into the statistical signatures of 3-D anisotropic MHD turbulence in the solar wind. Emphasis is placed on testing homogeneous phenomenological models of MHD turbulence informed by the principles of critical balance and dynamic alignment and assessing the extent to which the conjectures and predictions made by these models align with in-situ observations. By comparing our observations with the model predictions, we aim to understand how effects not accounted for in these models, but present in the solar wind-namely, inhomogeneity induced by the radial expansion, imbalance in the fluxes of counterpropagating wave packets, compressibility, and the spherically polarized nature of the magnetic field fluctuations-can affect the statistical properties of MHD turbulence. In parallel, our study dissects the dynamics and radial evolution of coherent magnetic structures, elucidating their role in magnetic energy dissipation and the ensuing heating of the solar wind.

Subject Added Entry-Topical Term  

Astrophysics.

Subject Added Entry-Topical Term  

Plasma physics.

Subject Added Entry-Topical Term  

Statistical physics.

Subject Added Entry-Topical Term  

Astronomy.

Index Term-Uncontrolled  

Alfven waves

Index Term-Uncontrolled  

MHD turbulence

Index Term-Uncontrolled  

Solar wind

Index Term-Uncontrolled  

Space physics

Index Term-Uncontrolled  

Plasma turbulence

Added Entry-Corporate Name  

University of California, Los Angeles Geophysics & Space Physics 0406

Host Item Entry  

Dissertations Abstracts International. 85-12B.

Electronic Location and Access  

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Control Number  

joongbu:658455