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Toward Self-Consistent Models of High-Energy Transients from Stellar Remnants- [electronic resource]
Toward Self-Consistent Models of High-Energy Transients from Stellar Remnants- [electronic resource]
상세정보
- 자료유형
- 학위논문파일 국외
- 최종처리일시
- 20240214101659
- ISBN
- 9798380416207
- DDC
- 523
- 저자명
- Halevi, Goni.
- 서명/저자
- Toward Self-Consistent Models of High-Energy Transients from Stellar Remnants - [electronic resource]
- 발행사항
- [S.l.]: : Princeton University., 2023
- 발행사항
- Ann Arbor : : ProQuest Dissertations & Theses,, 2023
- 형태사항
- 1 online resource(181 p.)
- 주기사항
- Source: Dissertations Abstracts International, Volume: 85-03, Section: B.
- 주기사항
- Advisor: Stone, James M.
- 학위논문주기
- Thesis (Ph.D.)--Princeton University, 2023.
- 사용제한주기
- This item must not be sold to any third party vendors.
- 초록/해제
- 요약The universe is vast and mostly empty, but it is not static or dull. All massive stars collapse quickly, and some explode, releasing more energy in a few seconds than our own sun has over its entire lifetime. The cores of these stars form compact objects-- neutron stars and black holes-- that can spiral toward one another, emitting gravitational waves, ejecting mass, and producing light as they collide. Black holes swallow material by accreting from gaseous disks, sometimes launching relativistic, collimated outflows as they spin, tangling up the magnetic fields that are carried toward them. These luminous, fast events are responsible for making the heaviest elements in our universe and lighting up the sky as brief, bright sources that have captivated humans for over a millennium. Today, they are observable in huge numbers, not just with telescopes that are sensitive to light across the electromagnetic spectrum, from radio waves to gamma rays, but also with interferometers that detect gravitational waves. With upcoming observatories, we will soon be inundated with data in the field of time-domain astronomy, rendering the pursuit of complex, multi-physics models for stellar collapse, accretion, and mergers timely. In this dissertation, I study a range of high-energy astrophysical transients powered by massive stars and their remnants by numerically solving the equations that govern fluids in regions of strong gravity. I improve upon current state-of-the-art models that use idealized initial conditions or explore a limited region of parameter space to gain insight into the progenitor systems that drive luminous transients and their evolution. I begin by summarizing the observational and theoretical state of the field and providing an overview of the fundamental physical processes of relevance. I then present results from three studies I led, two of which deal with collapsing massive stars as progenitors for bursts of gamma-ray emission, and a third exploring magnetic fields with applications to stellar encounters with black holes. I conclude with a discussion of future work I intend to carry out, focusing on the synthesis of elements in these events, and preliminary results related to it.
- 일반주제명
- Astrophysics.
- 일반주제명
- Computational physics.
- 일반주제명
- Astronomy.
- 키워드
- Black holes
- 키워드
- Gamma ray bursts
- 기타저자
- Princeton University Astrophysical Sciences
- 기본자료저록
- Dissertations Abstracts International. 85-03B.
- 기본자료저록
- Dissertation Abstract International
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
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■00520240214101659
■006m o d
■007cr#unu||||||||
■020 ▼a9798380416207
■035 ▼a(MiAaPQ)AAI30635542
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aHalevi, Goni.
■24510▼aToward Self-Consistent Models of High-Energy Transients from Stellar Remnants▼h[electronic resource]
■260 ▼a[S.l.]:▼bPrinceton University. ▼c2023
■260 1▼aAnn Arbor :▼bProQuest Dissertations & Theses, ▼c2023
■300 ▼a1 online resource(181 p.)
■500 ▼aSource: Dissertations Abstracts International, Volume: 85-03, Section: B.
■500 ▼aAdvisor: Stone, James M.
■5021 ▼aThesis (Ph.D.)--Princeton University, 2023.
■506 ▼aThis item must not be sold to any third party vendors.
■520 ▼aThe universe is vast and mostly empty, but it is not static or dull. All massive stars collapse quickly, and some explode, releasing more energy in a few seconds than our own sun has over its entire lifetime. The cores of these stars form compact objects-- neutron stars and black holes-- that can spiral toward one another, emitting gravitational waves, ejecting mass, and producing light as they collide. Black holes swallow material by accreting from gaseous disks, sometimes launching relativistic, collimated outflows as they spin, tangling up the magnetic fields that are carried toward them. These luminous, fast events are responsible for making the heaviest elements in our universe and lighting up the sky as brief, bright sources that have captivated humans for over a millennium. Today, they are observable in huge numbers, not just with telescopes that are sensitive to light across the electromagnetic spectrum, from radio waves to gamma rays, but also with interferometers that detect gravitational waves. With upcoming observatories, we will soon be inundated with data in the field of time-domain astronomy, rendering the pursuit of complex, multi-physics models for stellar collapse, accretion, and mergers timely. In this dissertation, I study a range of high-energy astrophysical transients powered by massive stars and their remnants by numerically solving the equations that govern fluids in regions of strong gravity. I improve upon current state-of-the-art models that use idealized initial conditions or explore a limited region of parameter space to gain insight into the progenitor systems that drive luminous transients and their evolution. I begin by summarizing the observational and theoretical state of the field and providing an overview of the fundamental physical processes of relevance. I then present results from three studies I led, two of which deal with collapsing massive stars as progenitors for bursts of gamma-ray emission, and a third exploring magnetic fields with applications to stellar encounters with black holes. I conclude with a discussion of future work I intend to carry out, focusing on the synthesis of elements in these events, and preliminary results related to it.
■590 ▼aSchool code: 0181.
■650 4▼aAstrophysics.
■650 4▼aComputational physics.
■650 4▼aAstronomy.
■653 ▼aBlack holes
■653 ▼aGamma ray bursts
■653 ▼aHigh-energy astrophysics
■653 ▼aMagnetohydrodynamics
■690 ▼a0596
■690 ▼a0216
■690 ▼a0606
■71020▼aPrinceton University▼bAstrophysical Sciences.
■7730 ▼tDissertations Abstracts International▼g85-03B.
■773 ▼tDissertation Abstract International
■790 ▼a0181
■791 ▼aPh.D.
■792 ▼a2023
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T16934834▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
■980 ▼a202402▼f2024
