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The Magellanic Corona and Its Role in the Evolution of the Magellanic Stream- [electronic resource]
The Magellanic Corona and Its Role in the Evolution of the Magellanic Stream- [electronic resource]
상세정보
- 자료유형
- 학위논문파일 국외
- 최종처리일시
- 20240214101511
- ISBN
- 9798379795764
- DDC
- 523
- 저자명
- Lucchini, Scott.
- 서명/저자
- The Magellanic Corona and Its Role in the Evolution of the Magellanic Stream - [electronic resource]
- 발행사항
- [S.l.]: : The University of Wisconsin - Madison., 2023
- 발행사항
- Ann Arbor : : ProQuest Dissertations & Theses,, 2023
- 형태사항
- 1 online resource(134 p.)
- 주기사항
- Source: Dissertations Abstracts International, Volume: 85-01, Section: B.
- 주기사항
- Advisor: D'Onghia, Elena.
- 학위논문주기
- Thesis (Ph.D.)--The University of Wisconsin - Madison, 2023.
- 사용제한주기
- This item must not be sold to any third party vendors.
- 초록/해제
- 요약The Magellanic System is the perfect opportunity to explore many aspects of astrophysics right on our Galaxy's doorstep. Two dwarf galaxies, the Large and Small Magellanic Clouds (LMC, SMC) are interacting with each other and with the Milky Way to form the Magellanic Stream, a multiphase gaseous tail of intertwined filaments trailing behind the Clouds. Here we can study galactic dynamics, gas dynamics, turbulent processes, gas cooling and mixing, metal transport, and more. However, there are two outstanding mysteries as to how the Magellanic System came to be -- its large amount of ionized gas, and the high mass of the LMC. To solve both these discrepancies simultaneously, we introduce the Magellanic Corona. This warm, ionized circumgalactic medium should surround the LMC as it interacts with the SMC and the Milky Way. Throughout my thesis work, I have used high-resolution numerical simulations of the formation of the Magellanic Stream to test this new model including the Magellanic Corona. We can account for both the neutral and ionized components of the Stream while also reproducing the present-day positions and velocities of the LMC and the SMC. We have also found a new family of orbital histories for the Clouds that result in the neutral Stream being significantly closer than previous models predicted. The Magellanic Corona seems to be the key to the formation of the Magellanic Stream and has many implications throughout galaxy evolution.
- 일반주제명
- Astrophysics.
- 일반주제명
- Astronomy.
- 일반주제명
- Computational physics.
- 일반주제명
- Physics.
- 키워드
- Galaxies
- 키워드
- Galaxy evolution
- 키워드
- Milky Way
- 키워드
- Simulations
- 기타저자
- The University of Wisconsin - Madison Physics
- 기본자료저록
- Dissertations Abstracts International. 85-01B.
- 기본자료저록
- Dissertation Abstract International
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
008240612s2023 us |||||||||||||||c||eng d■001000016933954
■00520240214101511
■006m o d
■007cr#unu||||||||
■020 ▼a9798379795764
■035 ▼a(MiAaPQ)AAI30568248
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aLucchini, Scott.
■24510▼aThe Magellanic Corona and Its Role in the Evolution of the Magellanic Stream▼h[electronic resource]
■260 ▼a[S.l.]:▼bThe University of Wisconsin - Madison. ▼c2023
■260 1▼aAnn Arbor :▼bProQuest Dissertations & Theses, ▼c2023
■300 ▼a1 online resource(134 p.)
■500 ▼aSource: Dissertations Abstracts International, Volume: 85-01, Section: B.
■500 ▼aAdvisor: D'Onghia, Elena.
■5021 ▼aThesis (Ph.D.)--The University of Wisconsin - Madison, 2023.
■506 ▼aThis item must not be sold to any third party vendors.
■520 ▼aThe Magellanic System is the perfect opportunity to explore many aspects of astrophysics right on our Galaxy's doorstep. Two dwarf galaxies, the Large and Small Magellanic Clouds (LMC, SMC) are interacting with each other and with the Milky Way to form the Magellanic Stream, a multiphase gaseous tail of intertwined filaments trailing behind the Clouds. Here we can study galactic dynamics, gas dynamics, turbulent processes, gas cooling and mixing, metal transport, and more. However, there are two outstanding mysteries as to how the Magellanic System came to be -- its large amount of ionized gas, and the high mass of the LMC. To solve both these discrepancies simultaneously, we introduce the Magellanic Corona. This warm, ionized circumgalactic medium should surround the LMC as it interacts with the SMC and the Milky Way. Throughout my thesis work, I have used high-resolution numerical simulations of the formation of the Magellanic Stream to test this new model including the Magellanic Corona. We can account for both the neutral and ionized components of the Stream while also reproducing the present-day positions and velocities of the LMC and the SMC. We have also found a new family of orbital histories for the Clouds that result in the neutral Stream being significantly closer than previous models predicted. The Magellanic Corona seems to be the key to the formation of the Magellanic Stream and has many implications throughout galaxy evolution.
■590 ▼aSchool code: 0262.
■650 4▼aAstrophysics.
■650 4▼aAstronomy.
■650 4▼aComputational physics.
■650 4▼aPhysics.
■653 ▼aGalaxies
■653 ▼aGalaxy evolution
■653 ▼aMagellanic Clouds
■653 ▼aMilky Way
■653 ▼aSimulations
■690 ▼a0596
■690 ▼a0606
■690 ▼a0216
■690 ▼a0605
■71020▼aThe University of Wisconsin - Madison▼bPhysics.
■7730 ▼tDissertations Abstracts International▼g85-01B.
■773 ▼tDissertation Abstract International
■790 ▼a0262
■791 ▼aPh.D.
■792 ▼a2023
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T16933954▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
■980 ▼a202402▼f2024
