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Black Hole Populations and Escape Dynamics in Globular Clusters
Black Hole Populations and Escape Dynamics in Globular Clusters
상세정보
- 자료유형
- 학위논문 서양
- 최종처리일시
- 20250211152022
- ISBN
- 9798384018728
- DDC
- 523
- 서명/저자
- Black Hole Populations and Escape Dynamics in Globular Clusters
- 발행사항
- [Sl] : Northwestern University, 2024
- 발행사항
- Ann Arbor : ProQuest Dissertations & Theses, 2024
- 형태사항
- 280 p
- 주기사항
- Source: Dissertations Abstracts International, Volume: 86-02, Section: B.
- 주기사항
- Advisor: Rasio, Frederic A.
- 학위논문주기
- Thesis (Ph.D.)--Northwestern University, 2024.
- 초록/해제
- 요약In this dissertation, I explore dynamics of globular clusters (GCs) essential to interpreting recent observations of gravitational-wave (GW) events and stellar streams, two of the most feverishly studied topics in astrophysics this decade. In particular, a significant fraction of GW events from merging black holes (BHs) are likely attributable to dynamics in the dense cores of GCs, whose gradual dissolution also contributes many stellar streams to the complex tapestry of substructure in the halo of our Galaxy. After introducing key concepts in GC dynamics and modeling (Part 1), I present in Part 2 highly robust measures of BH content in our Galaxy's GCs and demonstrate they likely retain dozens of BHs on average at present. This is a key piece of evidence supporting the GC-modeling community's recent assertions, formerly undermined by significant modeling uncertainties, that GCs retain enough BHs to contribute strongly to the observed BH merger rate. I then analyze how variations in the high-mass slope of the stellar initial mass function, a key modeling uncertainty, impact their BH populations, production of BH mergers, and GC evaporation. In Part 3, I branch towards Galactic archeology by thoroughly reviewing and studying the mechanisms of escape from GCs relevant to production of both runaway/hypervelocity stars and stellar streams in the Milky Way. I show how the regulation of GC core collapse by BHs has a significant impact on production of these phenomena and present a new method of modeling stellar streams from GCs that carries a unique balance of speed and accuracy. This work may eventually be helpful in efforts to apply observed stellar stream morphology as a probe of dark matter's identity, one of the most pressing mysteries in astrophysics.
- 일반주제명
- Astrophysics
- 일반주제명
- Astronomy
- 일반주제명
- Computational physics
- 키워드
- Black holes
- 키워드
- Stellar dynamics
- 키워드
- Stellar streams
- 키워드
- Tidal tails
- 기타저자
- Northwestern University Physics and Astronomy
- 기본자료저록
- Dissertations Abstracts International. 86-02B.
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
008250123s2024 us c eng d■001000017162519
■00520250211152022
■006m o d
■007cr#unu||||||||
■020 ▼a9798384018728
■035 ▼a(MiAaPQ)AAI31332368
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aWeatherford, Newlin C.▼0(orcid)0000-0002-9660-9085
■24510▼aBlack Hole Populations and Escape Dynamics in Globular Clusters
■260 ▼a[Sl]▼bNorthwestern University▼c2024
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2024
■300 ▼a280 p
■500 ▼aSource: Dissertations Abstracts International, Volume: 86-02, Section: B.
■500 ▼aAdvisor: Rasio, Frederic A.
■5021 ▼aThesis (Ph.D.)--Northwestern University, 2024.
■520 ▼aIn this dissertation, I explore dynamics of globular clusters (GCs) essential to interpreting recent observations of gravitational-wave (GW) events and stellar streams, two of the most feverishly studied topics in astrophysics this decade. In particular, a significant fraction of GW events from merging black holes (BHs) are likely attributable to dynamics in the dense cores of GCs, whose gradual dissolution also contributes many stellar streams to the complex tapestry of substructure in the halo of our Galaxy. After introducing key concepts in GC dynamics and modeling (Part 1), I present in Part 2 highly robust measures of BH content in our Galaxy's GCs and demonstrate they likely retain dozens of BHs on average at present. This is a key piece of evidence supporting the GC-modeling community's recent assertions, formerly undermined by significant modeling uncertainties, that GCs retain enough BHs to contribute strongly to the observed BH merger rate. I then analyze how variations in the high-mass slope of the stellar initial mass function, a key modeling uncertainty, impact their BH populations, production of BH mergers, and GC evaporation. In Part 3, I branch towards Galactic archeology by thoroughly reviewing and studying the mechanisms of escape from GCs relevant to production of both runaway/hypervelocity stars and stellar streams in the Milky Way. I show how the regulation of GC core collapse by BHs has a significant impact on production of these phenomena and present a new method of modeling stellar streams from GCs that carries a unique balance of speed and accuracy. This work may eventually be helpful in efforts to apply observed stellar stream morphology as a probe of dark matter's identity, one of the most pressing mysteries in astrophysics.
■590 ▼aSchool code: 0163.
■650 4▼aAstrophysics
■650 4▼aAstronomy
■650 4▼aComputational physics
■653 ▼aBlack holes
■653 ▼aGlobular clusters
■653 ▼aN-body simulations
■653 ▼aStellar dynamics
■653 ▼aStellar streams
■653 ▼aTidal tails
■690 ▼a0596
■690 ▼a0606
■690 ▼a0216
■71020▼aNorthwestern University▼bPhysics and Astronomy.
■7730 ▼tDissertations Abstracts International▼g86-02B.
■790 ▼a0163
■791 ▼aPh.D.
■792 ▼a2024
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T17162519▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
