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Reconnection-Driven Flares in Magnetized Astrophysical Plasmas: From the Solar Atmosphere to Sagittarius A*
Reconnection-Driven Flares in Magnetized Astrophysical Plasmas: From the Solar Atmosphere to Sagittarius A*
상세정보
- 자료유형
- 학위논문 서양
- 최종처리일시
- 20260202105145
- ISBN
- 9798265408013
- DDC
- 523
- 서명/저자
- Reconnection-Driven Flares in Magnetized Astrophysical Plasmas: From the Solar Atmosphere to Sagittarius A*
- 발행사항
- [Sl] : Harvard University, 2025
- 발행사항
- Ann Arbor : ProQuest Dissertations & Theses, 2025
- 형태사항
- 221 p
- 주기사항
- Source: Dissertations Abstracts International, Volume: 87-05, Section: B.
- 주기사항
- Advisor: Samra, Jenna.
- 학위논문주기
- Thesis (Ph.D.)--Harvard University, 2025.
- 초록/해제
- 요약Energetic flares are observed across magnetized astrophysical systems, from stellar coronae to the inner regions of black hole accretion flows. Interpreting their emission remains a challenge, as the underlying physics spans a vast range of spatial and temporal scales-from kinetic-scale particle acceleration to large-scale magnetic structures that govern global energy release. On the observational side, I present the development and first flight of a high-cadence soft X-ray imaging system flown in the 2024 NASA Solar Flare Sounding Rocket Campaign. The instrument leverages delta-doped, back-illuminated CMOS sensors to achieve sub-second imaging in the 0.5-10 keV band, enabling improved temporal resolution of flare dynamics in the solar corona. On the theoretical side, I present fully three-dimensional general relativistic particle-in-cell (GRPIC) simulations of magnetic reconnection in relativistic, high-guide field plasmas, motivated by flares from the supermassive black hole at the center of our galaxy. Through analysis of particle acceleration and synchrotron emission, we offer a physical explanation for the observed diversity in infrared and X-ray flares from Sagittarius A*. Taken together, these efforts demonstrate how new observational tools and high-fidelity simulations can jointly advance our understanding of reconnection-driven energy release across astrophysical environments.
- 일반주제명
- Astrophysics
- 일반주제명
- Electromagnetics
- 일반주제명
- Plasma physics
- 키워드
- Energetic flares
- 키워드
- X-ray imaging
- 키워드
- Diversity
- 기타저자
- Harvard University Astronomy
- 기본자료저록
- Dissertations Abstracts International. 87-05B.
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
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■00520260202105145
■006m o d
■007cr#unu||||||||
■020 ▼a9798265408013
■035 ▼a(MiAaPQ)AAI32241101
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aSanchez-Maes, Sophia Araceli.
■24510▼aReconnection-Driven Flares in Magnetized Astrophysical Plasmas: From the Solar Atmosphere to Sagittarius A*
■260 ▼a[Sl]▼bHarvard University▼c2025
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2025
■300 ▼a221 p
■500 ▼aSource: Dissertations Abstracts International, Volume: 87-05, Section: B.
■500 ▼aAdvisor: Samra, Jenna.
■5021 ▼aThesis (Ph.D.)--Harvard University, 2025.
■520 ▼aEnergetic flares are observed across magnetized astrophysical systems, from stellar coronae to the inner regions of black hole accretion flows. Interpreting their emission remains a challenge, as the underlying physics spans a vast range of spatial and temporal scales-from kinetic-scale particle acceleration to large-scale magnetic structures that govern global energy release. On the observational side, I present the development and first flight of a high-cadence soft X-ray imaging system flown in the 2024 NASA Solar Flare Sounding Rocket Campaign. The instrument leverages delta-doped, back-illuminated CMOS sensors to achieve sub-second imaging in the 0.5-10 keV band, enabling improved temporal resolution of flare dynamics in the solar corona. On the theoretical side, I present fully three-dimensional general relativistic particle-in-cell (GRPIC) simulations of magnetic reconnection in relativistic, high-guide field plasmas, motivated by flares from the supermassive black hole at the center of our galaxy. Through analysis of particle acceleration and synchrotron emission, we offer a physical explanation for the observed diversity in infrared and X-ray flares from Sagittarius A*. Taken together, these efforts demonstrate how new observational tools and high-fidelity simulations can jointly advance our understanding of reconnection-driven energy release across astrophysical environments.
■590 ▼aSchool code: 0084.
■650 4▼aAstrophysics
■650 4▼aElectromagnetics
■650 4▼aPlasma physics
■653 ▼aEnergetic flares
■653 ▼aAstrophysical systems
■653 ▼aX-ray imaging
■653 ▼aDiversity
■653 ▼aGlobal energy release
■690 ▼a0596
■690 ▼a0607
■690 ▼a0759
■71020▼aHarvard University▼bAstronomy.
■7730 ▼tDissertations Abstracts International▼g87-05B.
■790 ▼a0084
■791 ▼aPh.D.
■792 ▼a2025
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T17359607▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
