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On the Dynamical Evolution of Alfvenic Turbulence in the Inner Heliosphere
On the Dynamical Evolution of Alfvenic Turbulence in the Inner Heliosphere
상세정보
- 자료유형
- 학위논문 서양
- 최종처리일시
- 20250211152010
- ISBN
- 9798382829760
- DDC
- 523
- 서명/저자
- On the Dynamical Evolution of Alfvenic Turbulence in the Inner Heliosphere
- 발행사항
- [Sl] : University of California, Los Angeles, 2024
- 발행사항
- Ann Arbor : ProQuest Dissertations & Theses, 2024
- 형태사항
- 317 p
- 주기사항
- Source: Dissertations Abstracts International, Volume: 85-12, Section: B.
- 주기사항
- Advisor: Velli, Marco C. M.
- 학위논문주기
- Thesis (Ph.D.)--University of California, Los Angeles, 2024.
- 초록/해제
- 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.
- 일반주제명
- Astrophysics
- 일반주제명
- Plasma physics
- 일반주제명
- Statistical physics
- 일반주제명
- Astronomy
- 키워드
- Alfven waves
- 키워드
- MHD turbulence
- 키워드
- Solar wind
- 키워드
- Space physics
- 기타저자
- University of California, Los Angeles Geophysics & Space Physics 0406
- 기본자료저록
- Dissertations Abstracts International. 85-12B.
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
008250123s2024 us c eng d■001000017162418
■00520250211152010
■006m o d
■007cr#unu||||||||
■020 ▼a9798382829760
■035 ▼a(MiAaPQ)AAI31331039
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aSioulas, Nikolaos.
■24510▼aOn the Dynamical Evolution of Alfvenic Turbulence in the Inner Heliosphere
■260 ▼a[Sl]▼bUniversity of California, Los Angeles▼c2024
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2024
■300 ▼a317 p
■500 ▼aSource: Dissertations Abstracts International, Volume: 85-12, Section: B.
■500 ▼aAdvisor: Velli, Marco C. M.
■5021 ▼aThesis (Ph.D.)--University of California, Los Angeles, 2024.
■520 ▼aAs 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.
■590 ▼aSchool code: 0031.
■650 4▼aAstrophysics
■650 4▼aPlasma physics
■650 4▼aStatistical physics
■650 4▼aAstronomy
■653 ▼aAlfven waves
■653 ▼aMHD turbulence
■653 ▼aSolar wind
■653 ▼aSpace physics
■653 ▼aPlasma turbulence
■690 ▼a0596
■690 ▼a0759
■690 ▼a0217
■690 ▼a0606
■71020▼aUniversity of California, Los Angeles▼bGeophysics & Space Physics 0406.
■7730 ▼tDissertations Abstracts International▼g85-12B.
■790 ▼a0031
■791 ▼aPh.D.
■792 ▼a2024
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T17162418▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
