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Modeling the Mars-Solar Wind Interaction with Enhanced Multi-Species MHD: Proton Origin and Ion-Electron Temperature Separation
Modeling the Mars-Solar Wind Interaction with Enhanced Multi-Species MHD: Proton Origin and Ion-Electron Temperature Separation
상세정보
- 자료유형
- 학위논문 서양
- 최종처리일시
- 20260202105252
- ISBN
- 9798297637580
- DDC
- 550
- 저자명
- Sun, Wenyi.
- 서명/저자
- Modeling the Mars-Solar Wind Interaction with Enhanced Multi-Species MHD: Proton Origin and Ion-Electron Temperature Separation
- 발행사항
- [Sl] : University of California, Los Angeles, 2025
- 발행사항
- Ann Arbor : ProQuest Dissertations & Theses, 2025
- 형태사항
- 118 p
- 주기사항
- Source: Dissertations Abstracts International, Volume: 87-04, Section: B.
- 주기사항
- Advisor: Ma, Yingjuan Y.;Russell, Christopher C. T.
- 학위논문주기
- Thesis (Ph.D.)--University of California, Los Angeles, 2025.
- 초록/해제
- 요약Mars, lacking a global magnetic field, experiences direct interaction between the solar wind and its upper atmosphere and ionosphere, leading to ion escape that has played a major role in long-term atmospheric loss and climate evolution. Understanding this interaction is critical for understanding the planet's history and planetary habitability.This dissertation advances our understanding of the Martian plasma environment with detailed analysis of proton behaviors, system-wide responses to upstream variability, and ion-electron energetics, through advanced multi-species magnetohydrodynamic (MHD) modeling. In the model, we introduce two key improvements: the separation of planetary and solar wind protons, which allows their distinct distributions and fluxes to be tracked, and the inclusion of an electron pressure equation with variable photoelectron heating, which improves the treatment of ionospheric energetics.With separated proton origins, our simulations reveal the distinct distributions and behaviors of planetary protons and solar wind protons. Planetary proton escape rates generally exceed those of heavy ions under both solar minimum and maximum conditions, though they remain one to two orders of magnitude lower than the neutral hydrogen escape rate. Solar wind precipitations are strongly influenced by the crustal magnetic fields. These results also underscore the importance of ion chemistry, such as charge exchange and impact ionization. Starting from these steady-state solutions, the dissertation also examines how the Martian plasma system reacts to short-term solar wind dynamic pressure enhancements, which drive a sequence of response phases: initial compression, sustained compression, rapid expansion, and gradual recovery, governed by a combination of upstream variability and intrinsic system dynamics. To further explore the validity of the results, a comprehensive comparison between two independent multi-species MHD codes is conducted, demonstrating a high degree of consistency in global structures and escape rates. Sensitivity experiments within this comparison also reveal that assumptions about ion-electron temperature separation and photoelectron heating can significantly affect ionospheric structure and escape rate predictions.Our studies provide new insights into the drivers of ion escape and the dynamics of the present-day Martian plasma environment, clarifying the roles of proton behaviors, transient solar wind conditions, and temperature decoupling. Furthermore, this dissertation demonstrates how advanced global modeling, when carefully validated, can serve as a framework for exploring atmospheric loss under extreme solar conditions and across other planetary systems.
- 일반주제명
- Geophysics
- 일반주제명
- Plasma physics
- 일반주제명
- Astrophysics
- 키워드
- Mars
- 키워드
- Space plasma
- 기타저자
- University of California, Los Angeles Geophysics & Space Physics 0406
- 기본자료저록
- Dissertations Abstracts International. 87-04B.
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
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■00520260202105252
■006m o d
■007cr#unu||||||||
■020 ▼a9798297637580
■035 ▼a(MiAaPQ)AAI32277226
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a550
■1001 ▼aSun, Wenyi.
■24510▼aModeling the Mars-Solar Wind Interaction with Enhanced Multi-Species MHD: Proton Origin and Ion-Electron Temperature Separation
■260 ▼a[Sl]▼bUniversity of California, Los Angeles▼c2025
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2025
■300 ▼a118 p
■500 ▼aSource: Dissertations Abstracts International, Volume: 87-04, Section: B.
■500 ▼aAdvisor: Ma, Yingjuan Y.;Russell, Christopher C. T.
■5021 ▼aThesis (Ph.D.)--University of California, Los Angeles, 2025.
■520 ▼aMars, lacking a global magnetic field, experiences direct interaction between the solar wind and its upper atmosphere and ionosphere, leading to ion escape that has played a major role in long-term atmospheric loss and climate evolution. Understanding this interaction is critical for understanding the planet's history and planetary habitability.This dissertation advances our understanding of the Martian plasma environment with detailed analysis of proton behaviors, system-wide responses to upstream variability, and ion-electron energetics, through advanced multi-species magnetohydrodynamic (MHD) modeling. In the model, we introduce two key improvements: the separation of planetary and solar wind protons, which allows their distinct distributions and fluxes to be tracked, and the inclusion of an electron pressure equation with variable photoelectron heating, which improves the treatment of ionospheric energetics.With separated proton origins, our simulations reveal the distinct distributions and behaviors of planetary protons and solar wind protons. Planetary proton escape rates generally exceed those of heavy ions under both solar minimum and maximum conditions, though they remain one to two orders of magnitude lower than the neutral hydrogen escape rate. Solar wind precipitations are strongly influenced by the crustal magnetic fields. These results also underscore the importance of ion chemistry, such as charge exchange and impact ionization. Starting from these steady-state solutions, the dissertation also examines how the Martian plasma system reacts to short-term solar wind dynamic pressure enhancements, which drive a sequence of response phases: initial compression, sustained compression, rapid expansion, and gradual recovery, governed by a combination of upstream variability and intrinsic system dynamics. To further explore the validity of the results, a comprehensive comparison between two independent multi-species MHD codes is conducted, demonstrating a high degree of consistency in global structures and escape rates. Sensitivity experiments within this comparison also reveal that assumptions about ion-electron temperature separation and photoelectron heating can significantly affect ionospheric structure and escape rate predictions.Our studies provide new insights into the drivers of ion escape and the dynamics of the present-day Martian plasma environment, clarifying the roles of proton behaviors, transient solar wind conditions, and temperature decoupling. Furthermore, this dissertation demonstrates how advanced global modeling, when carefully validated, can serve as a framework for exploring atmospheric loss under extreme solar conditions and across other planetary systems.
■590 ▼aSchool code: 0031.
■650 4▼aGeophysics
■650 4▼aPlasma physics
■650 4▼aAstrophysics
■653 ▼aMagnetohydrodynamics
■653 ▼aMars
■653 ▼aSolar-planteary interaction
■653 ▼aSpace plasma
■690 ▼a0373
■690 ▼a0759
■690 ▼a0596
■690 ▼a0467
■71020▼aUniversity of California, Los Angeles▼bGeophysics & Space Physics 0406.
■7730 ▼tDissertations Abstracts International▼g87-04B.
■790 ▼a0031
■791 ▼aPh.D.
■792 ▼a2025
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T17360023▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
