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Cosmic Ray Electrons in the Multiphase Interstellar Medium
Cosmic Ray Electrons in the Multiphase Interstellar Medium
상세정보
- 자료유형
- 학위논문 서양
- 최종처리일시
- 20260202104804
- ISBN
- 9798293894468
- DDC
- 523
- 저자명
- Linzer, Nora B.
- 서명/저자
- Cosmic Ray Electrons in the Multiphase Interstellar Medium
- 발행사항
- [Sl] : Princeton University, 2025
- 발행사항
- Ann Arbor : ProQuest Dissertations & Theses, 2025
- 형태사항
- 152 p
- 주기사항
- Source: Dissertations Abstracts International, Volume: 87-04, Section: B.
- 주기사항
- Advisor: Ostriker, Eve C.;Quataert, Eliot.
- 학위논문주기
- Thesis (Ph.D.)--Princeton University, 2025.
- 초록/해제
- 요약Cosmic rays (CRs) make up a significant pressure component of the interstellar medium (ISM), on the order of the thermal, turbulent, and magnetic pressures. Therefore, these particles can substantially impact galactic dynamics. Direct observations show that protons make up the majority of the CR population and that there are significantly fewer CR electrons (CREs), so the physical impact of CREs is negligible. Beyond the solar neighborhood, however, CRs cannot be directly measured, and we must rely on indirect probes, primarily radio synchrotron emission produced by the interaction of CREs with local magnetic fields. It is therefore of great importance to understand the evolution of CREs in realistic simulations of the ISM to interpret indirect measurements of the CR population.In this work, we present a scheme for modeling the transport and spectral evolution of CREs in the magnetized, multiphase ISM which we use to post-process TIGRESS simulations of multiple galactic environments. In Chapter 2, we lay out our two-moment transport method which includes advection, streaming, and diffusion, as well as various energetic loss mechanisms. We post-process TIGRESS models representative of solar neighborhood conditions and find the simulated CRE spectrum to be consistent with direct observations. In Chapter 3, we produce synthetic synchrotron emission which we use to test common observational methods including the extraction of the CRE spectrum from radio observations, as well as the estimation of magnetic field strength through the equipartition assumption. In Chapter 4, we apply our CR modeling scheme to TIGRESS simulations representative of inner galaxy conditions to understand how CRE transport may differ as a function of environment. Finally, we present opportunities for future analysis in Chapter 5.
- 일반주제명
- Astrophysics
- 일반주제명
- Applied physics
- 일반주제명
- Astronomy
- 키워드
- Cosmic rays
- 키워드
- Protons
- 기타저자
- Princeton University Astrophysical Sciences
- 기본자료저록
- Dissertations Abstracts International. 87-04B.
- 전자적 위치 및 접속
- 로그인 후 원문을 볼 수 있습니다.
MARC
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■00520260202104804
■006m o d
■007cr#unu||||||||
■020 ▼a9798293894468
■035 ▼a(MiAaPQ)AAI32164960
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aLinzer, Nora B.▼0(orcid)0000-0001-8840-2538
■24510▼aCosmic Ray Electrons in the Multiphase Interstellar Medium
■260 ▼a[Sl]▼bPrinceton University▼c2025
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2025
■300 ▼a152 p
■500 ▼aSource: Dissertations Abstracts International, Volume: 87-04, Section: B.
■500 ▼aAdvisor: Ostriker, Eve C.;Quataert, Eliot.
■5021 ▼aThesis (Ph.D.)--Princeton University, 2025.
■520 ▼aCosmic rays (CRs) make up a significant pressure component of the interstellar medium (ISM), on the order of the thermal, turbulent, and magnetic pressures. Therefore, these particles can substantially impact galactic dynamics. Direct observations show that protons make up the majority of the CR population and that there are significantly fewer CR electrons (CREs), so the physical impact of CREs is negligible. Beyond the solar neighborhood, however, CRs cannot be directly measured, and we must rely on indirect probes, primarily radio synchrotron emission produced by the interaction of CREs with local magnetic fields. It is therefore of great importance to understand the evolution of CREs in realistic simulations of the ISM to interpret indirect measurements of the CR population.In this work, we present a scheme for modeling the transport and spectral evolution of CREs in the magnetized, multiphase ISM which we use to post-process TIGRESS simulations of multiple galactic environments. In Chapter 2, we lay out our two-moment transport method which includes advection, streaming, and diffusion, as well as various energetic loss mechanisms. We post-process TIGRESS models representative of solar neighborhood conditions and find the simulated CRE spectrum to be consistent with direct observations. In Chapter 3, we produce synthetic synchrotron emission which we use to test common observational methods including the extraction of the CRE spectrum from radio observations, as well as the estimation of magnetic field strength through the equipartition assumption. In Chapter 4, we apply our CR modeling scheme to TIGRESS simulations representative of inner galaxy conditions to understand how CRE transport may differ as a function of environment. Finally, we present opportunities for future analysis in Chapter 5.
■590 ▼aSchool code: 0181.
■650 4▼aAstrophysics
■650 4▼aApplied physics
■650 4▼aAstronomy
■653 ▼aInterstellar medium
■653 ▼aCosmic rays
■653 ▼aProtons
■690 ▼a0596
■690 ▼a0215
■690 ▼a0606
■71020▼aPrinceton University▼bAstrophysical Sciences.
■7730 ▼tDissertations Abstracts International▼g87-04B.
■790 ▼a0181
■791 ▼aPh.D.
■792 ▼a2025
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T17358876▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
