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Quantum Effects Inside Rotating, Accreting Black Holes
Quantum Effects Inside Rotating, Accreting Black Holes
상세정보
- 자료유형
- 학위논문 서양
- 최종처리일시
- 20250211152646
- ISBN
- 9798384054696
- DDC
- 523
- 서명/저자
- Quantum Effects Inside Rotating, Accreting Black Holes
- 발행사항
- [Sl] : University of Colorado at Boulder, 2024
- 발행사항
- Ann Arbor : ProQuest Dissertations & Theses, 2024
- 형태사항
- 298 p
- 주기사항
- Source: Dissertations Abstracts International, Volume: 86-03, Section: B.
- 주기사항
- Advisor: Hamilton, Andrew J. S.
- 학위논문주기
- Thesis (Ph.D.)--University of Colorado at Boulder, 2024.
- 초록/해제
- 요약Models of black holes in general relativity have a problem. Rotating spacetimes like the Kerr metric do incredibly well at predicting observed phenomena outside of the event horizon, despite the fact that these models assume that the spacetime is completely empty and stationary, or at the least that any added matter or radiation will not contribute any gravity of its own. However, if this matter or radiation falls below the event horizon into a black hole's interior, counter-propagating streams will grow in energy and eventually diverge before they even reach the central singularity, at a special surface called the inner horizon. This divergence will trigger an inflationary instability that calls into question the self-consistency of the Kerr metric and the very stability of black holes as astrophysical (and especially as quantum mechanical) objects.In this thesis, the astrophysically relevant effects of rotation and accretion are examined in detail to understand how they contribute self-consistently to the spacetime geometry of a black hole near its inner horizon. First, a model is developed (which I call the inflationary Kasner metric) that reproduces and generalizes the aforementioned inflationary instability within the framework of general relativity. Then, the effects of a quantum field near an inner horizon are explored. In particular, Hawking radiation emanating from the past horizon will accumulate and eventually diverge in temperature as the inner horizon is approached, and more numerically intensive calculations of the renormalized stress-energy tensor reveal that this diverging radiation plays a substantial role in modifying the black hole's interior geometry and replacing the inner horizon with a strong, chaotic, spacelike singularity. By analyzing the effects of both classical and quantum fields within black holes, one can thus come to a closer understanding of how astrophysically realistic black holes should appear in the context of semiclassical gravity.
- 일반주제명
- Astrophysics
- 일반주제명
- Quantum physics
- 일반주제명
- Physics
- 키워드
- Black holes
- 키워드
- Quantum gravity
- 기타저자
- University of Colorado at Boulder Physics
- 기본자료저록
- Dissertations Abstracts International. 86-03B.
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
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■020 ▼a9798384054696
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■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aMcMaken, Tyler Christian.▼0(orcid)0000-0003-3189-8565
■24510▼aQuantum Effects Inside Rotating, Accreting Black Holes
■260 ▼a[Sl]▼bUniversity of Colorado at Boulder▼c2024
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2024
■300 ▼a298 p
■500 ▼aSource: Dissertations Abstracts International, Volume: 86-03, Section: B.
■500 ▼aAdvisor: Hamilton, Andrew J. S.
■5021 ▼aThesis (Ph.D.)--University of Colorado at Boulder, 2024.
■520 ▼aModels of black holes in general relativity have a problem. Rotating spacetimes like the Kerr metric do incredibly well at predicting observed phenomena outside of the event horizon, despite the fact that these models assume that the spacetime is completely empty and stationary, or at the least that any added matter or radiation will not contribute any gravity of its own. However, if this matter or radiation falls below the event horizon into a black hole's interior, counter-propagating streams will grow in energy and eventually diverge before they even reach the central singularity, at a special surface called the inner horizon. This divergence will trigger an inflationary instability that calls into question the self-consistency of the Kerr metric and the very stability of black holes as astrophysical (and especially as quantum mechanical) objects.In this thesis, the astrophysically relevant effects of rotation and accretion are examined in detail to understand how they contribute self-consistently to the spacetime geometry of a black hole near its inner horizon. First, a model is developed (which I call the inflationary Kasner metric) that reproduces and generalizes the aforementioned inflationary instability within the framework of general relativity. Then, the effects of a quantum field near an inner horizon are explored. In particular, Hawking radiation emanating from the past horizon will accumulate and eventually diverge in temperature as the inner horizon is approached, and more numerically intensive calculations of the renormalized stress-energy tensor reveal that this diverging radiation plays a substantial role in modifying the black hole's interior geometry and replacing the inner horizon with a strong, chaotic, spacelike singularity. By analyzing the effects of both classical and quantum fields within black holes, one can thus come to a closer understanding of how astrophysically realistic black holes should appear in the context of semiclassical gravity.
■590 ▼aSchool code: 0051.
■650 4▼aAstrophysics
■650 4▼aQuantum physics
■650 4▼aPhysics
■653 ▼aBlack holes
■653 ▼aQuantum gravity
■653 ▼aStress-energy tensor
■690 ▼a0596
■690 ▼a0599
■690 ▼a0605
■71020▼aUniversity of Colorado at Boulder▼bPhysics.
■7730 ▼tDissertations Abstracts International▼g86-03B.
■790 ▼a0051
■791 ▼aPh.D.
■792 ▼a2024
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T17163269▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
