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Plasma Effects in Black Hole Accretion
Plasma Effects in Black Hole Accretion
상세정보
- 자료유형
- 학위논문 서양
- 최종처리일시
- 20250211152822
- ISBN
- 9798384463740
- DDC
- 523
- 서명/저자
- Plasma Effects in Black Hole Accretion
- 발행사항
- [Sl] : Princeton University, 2024
- 발행사항
- Ann Arbor : ProQuest Dissertations & Theses, 2024
- 형태사항
- 179 p
- 주기사항
- Source: Dissertations Abstracts International, Volume: 86-04, Section: B.
- 주기사항
- Advisor: Quataert, Eliot.
- 학위논문주기
- Thesis (Ph.D.)--Princeton University, 2024.
- 초록/해제
- 요약Supermassive black holes exert powerful influences on nearby stars, entire galaxies, and even the intergalactic medium, despite having event horizons that are smaller than the Solar System. Recent observations by the Event Horizon Telescope revealed asymmetric ring-like structures around M87* and Sgr A*, produced by a relativistic plasma consisting of ions, electrons, and possibly positrons. The characteristics of this extremely energetic plasma on microscopic scales fundamentally shape the system's large-scale dynamics. With such unprecedentedly detailed images, we require better models of the accretion flow. I have developed and applied first-principles models of relativistic plasmas around black holes, necessary for interpreting and predicting the results of observations across the electromagnetic spectrum. Microscopic plasma effects not only affect the overall state of accretion but also alter the way we observe these systems by changing the distribution function of synchrotron-emitting electrons. Hot accretion flows, which are believed to operate around low-luminosity galactic nuclei, are the focus of this work. Such systems are often associated with strong outflows, winds, and jets. Nevertheless, the closest low-luminosity supermassive black hole, Sagittarius A*, located in the center of our galaxy, appears to lack a powerful jet. A simplified model of spherical accretion demonstrates why such systems might be unable to produce strong jets.
- 일반주제명
- Astrophysics
- 일반주제명
- Astronomy
- 일반주제명
- Physics
- 일반주제명
- Plasma physics
- 키워드
- Black holes
- 기타저자
- Princeton University Astrophysical Sciences
- 기본자료저록
- Dissertations Abstracts International. 86-04B.
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
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■006m o d
■007cr#unu||||||||
■020 ▼a9798384463740
■035 ▼a(MiAaPQ)AAI31559736
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aGalishnikova, Alisa.
■24510▼aPlasma Effects in Black Hole Accretion
■260 ▼a[Sl]▼bPrinceton University▼c2024
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2024
■300 ▼a179 p
■500 ▼aSource: Dissertations Abstracts International, Volume: 86-04, Section: B.
■500 ▼aAdvisor: Quataert, Eliot.
■5021 ▼aThesis (Ph.D.)--Princeton University, 2024.
■520 ▼aSupermassive black holes exert powerful influences on nearby stars, entire galaxies, and even the intergalactic medium, despite having event horizons that are smaller than the Solar System. Recent observations by the Event Horizon Telescope revealed asymmetric ring-like structures around M87* and Sgr A*, produced by a relativistic plasma consisting of ions, electrons, and possibly positrons. The characteristics of this extremely energetic plasma on microscopic scales fundamentally shape the system's large-scale dynamics. With such unprecedentedly detailed images, we require better models of the accretion flow. I have developed and applied first-principles models of relativistic plasmas around black holes, necessary for interpreting and predicting the results of observations across the electromagnetic spectrum. Microscopic plasma effects not only affect the overall state of accretion but also alter the way we observe these systems by changing the distribution function of synchrotron-emitting electrons. Hot accretion flows, which are believed to operate around low-luminosity galactic nuclei, are the focus of this work. Such systems are often associated with strong outflows, winds, and jets. Nevertheless, the closest low-luminosity supermassive black hole, Sagittarius A*, located in the center of our galaxy, appears to lack a powerful jet. A simplified model of spherical accretion demonstrates why such systems might be unable to produce strong jets.
■590 ▼aSchool code: 0181.
■650 4▼aAstrophysics
■650 4▼aAstronomy
■650 4▼aPhysics
■650 4▼aPlasma physics
■653 ▼aBlack holes
■653 ▼aIntergalactic medium
■653 ▼aMicroscopic plasma effects
■690 ▼a0596
■690 ▼a0606
■690 ▼a0605
■690 ▼a0759
■71020▼aPrinceton University▼bAstrophysical Sciences.
■7730 ▼tDissertations Abstracts International▼g86-04B.
■790 ▼a0181
■791 ▼aPh.D.
■792 ▼a2024
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T17164027▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
