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Small-Scale Dynamics of Dust in the Interstellar Medium
Small-Scale Dynamics of Dust in the Interstellar Medium
상세정보
- 자료유형
- 학위논문 서양
- 최종처리일시
- 20250211152134
- ISBN
- 9798384466499
- DDC
- 523
- 저자명
- Moseley, Eric R.
- 서명/저자
- Small-Scale Dynamics of Dust in the Interstellar Medium
- 발행사항
- [Sl] : Princeton University, 2024
- 발행사항
- Ann Arbor : ProQuest Dissertations & Theses, 2024
- 형태사항
- 212 p
- 주기사항
- Source: Dissertations Abstracts International, Volume: 86-04, Section: B.
- 주기사항
- Advisor: Teyssier, Romain.
- 학위논문주기
- Thesis (Ph.D.)--Princeton University, 2024.
- 초록/해제
- 요약The interstellar medium is replete with microscopic, sub-micron-sized dust grains. These grains obscure and adulterate a wide variety of astrophysical observations. Thus, understanding their properties is critical for understanding essentially all astrophysical objects. Furthermore, this same dust is what eventually coalesces into planetesimals, and eventually planets. Historically however, dust is most often assumed to be perfectly coupled to gas in the interstellar medium. In order to understand the dynamics of marginally coupled dusty interstellar plasma, we have implemented novel magnetohydrodynamic(MHD)-particle-in-cell(PIC) methods into the astrophysical fluid code RAMSES. We treat dust grains as a set of massive "superparticles'' that experience aerodynamic drag and Lorentz force. We subject our code to a range of numerical tests designed to validate our method in different physical conditions, as well as to illustrate possible mechanisms by which grains can be accelerated. Having demonstrated the accuracy and stability of our MHD-PIC implementation, we turn our attention to understanding the velocity distributions of charged dust grains in generic conditions. We obtain a simple power-law relationship that quantifies the root-mean-square dust velocities as a function of the properties of the turbulence. Finally, we present the results of a high-resolution driven MHD turbulence simulation meant to represent as accurately as possible a small, parsec sized patch of cold neutral medium in order to understand dust-to-gas mass ratio fluctuations in this environment. We find that the dust density is roughly proportional to the square root of the gas density, with variations of factors of around 3 about this line. This work has wide-reaching implications, ranging from models for grain growth and destruction to the distribution of stellar metallicities.
- 일반주제명
- Astrophysics
- 일반주제명
- Plasma physics
- 일반주제명
- Physics
- 일반주제명
- Astronomy
- 키워드
- Dust
- 키워드
- Turbulence
- 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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■00520250211152134
■006m o d
■007cr#unu||||||||
■020 ▼a9798384466499
■035 ▼a(MiAaPQ)AAI31484051
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aMoseley, Eric R.▼0(orcid)0000-0001-8558-5009
■24510▼aSmall-Scale Dynamics of Dust in the Interstellar Medium
■260 ▼a[Sl]▼bPrinceton University▼c2024
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2024
■300 ▼a212 p
■500 ▼aSource: Dissertations Abstracts International, Volume: 86-04, Section: B.
■500 ▼aAdvisor: Teyssier, Romain.
■5021 ▼aThesis (Ph.D.)--Princeton University, 2024.
■520 ▼aThe interstellar medium is replete with microscopic, sub-micron-sized dust grains. These grains obscure and adulterate a wide variety of astrophysical observations. Thus, understanding their properties is critical for understanding essentially all astrophysical objects. Furthermore, this same dust is what eventually coalesces into planetesimals, and eventually planets. Historically however, dust is most often assumed to be perfectly coupled to gas in the interstellar medium. In order to understand the dynamics of marginally coupled dusty interstellar plasma, we have implemented novel magnetohydrodynamic(MHD)-particle-in-cell(PIC) methods into the astrophysical fluid code RAMSES. We treat dust grains as a set of massive "superparticles'' that experience aerodynamic drag and Lorentz force. We subject our code to a range of numerical tests designed to validate our method in different physical conditions, as well as to illustrate possible mechanisms by which grains can be accelerated. Having demonstrated the accuracy and stability of our MHD-PIC implementation, we turn our attention to understanding the velocity distributions of charged dust grains in generic conditions. We obtain a simple power-law relationship that quantifies the root-mean-square dust velocities as a function of the properties of the turbulence. Finally, we present the results of a high-resolution driven MHD turbulence simulation meant to represent as accurately as possible a small, parsec sized patch of cold neutral medium in order to understand dust-to-gas mass ratio fluctuations in this environment. We find that the dust density is roughly proportional to the square root of the gas density, with variations of factors of around 3 about this line. This work has wide-reaching implications, ranging from models for grain growth and destruction to the distribution of stellar metallicities.
■590 ▼aSchool code: 0181.
■650 4▼aAstrophysics
■650 4▼aPlasma physics
■650 4▼aPhysics
■650 4▼aAstronomy
■653 ▼aDust
■653 ▼aInterstellar medium
■653 ▼aMagnetohydrodynamics
■653 ▼aNumerical methods
■653 ▼aParticle kinetics
■653 ▼aTurbulence
■690 ▼a0596
■690 ▼a0759
■690 ▼a0606
■690 ▼a0605
■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=T17163096▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
