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Modeling the Three-Dimensional Atmospheric Structure and Emission Spectra of Hot Gaseous Planets.
Modeling the Three-Dimensional Atmospheric Structure and Emission Spectra of Hot Gaseous Planets.
상세정보
- 자료유형
- 학위논문
- Control Number
- 0017164544
- International Standard Book Number
- 9798384045748
- Dewey Decimal Classification Number
- 523
- Main Entry-Personal Name
- Malsky, Isaac.
- Publication, Distribution, etc. (Imprint
- [S.l.] : University of Michigan., 2024
- Publication, Distribution, etc. (Imprint
- Ann Arbor : ProQuest Dissertations & Theses, 2024
- Physical Description
- 241 p.
- General Note
- Source: Dissertations Abstracts International, Volume: 86-03, Section: B.
- General Note
- Advisor: Rauscher, Emily.
- Dissertation Note
- Thesis (Ph.D.)--University of Michigan, 2024.
- Summary, Etc.
- 요약Although thousands of exoplanets have been discovered, a relatively rare class of planets known as hot Jupiters has historically been critical to the advancement of the field. Hot Jupiters---massive gaseous planets with orbital semi-major axes less than ~0.05 au---are among the brightest and best candidates for atmospheric characterization. They are expected to be tidally locked, with constant day sides and constant night sides. Extreme temperature gradients drive supersonic winds, chemically diverse clouds form and dissipate in homogeneously, and hazes may blanket their atmospheres.In tandem with observations, simulations are critical to interpreting measurements, breaking degeneracies between different atmospheric physical and chemical structures, and showing how physical processes influence atmospheric circulation. The most comprehensive physics-driven models simulate full atmospheres and self-consistently show the resulting 3D chemical and physical structures. These models, known as General Circulation Models (GCMs), simulate radiative transfer, fluid dynamics, and other phenomena in planetary atmospheres.This thesis focuses on using numerical methods to characterize exoplanet atmospheres and expanding the physics within a GCM. Background to the field and an overview of GCMs is given in Chapter 1. In Chapter 2, I characterize how clouds and non-edge-on inclinations manifest in hot Jupiter emission spectra. In Chapter 3, I show that multiwavelength radiative transfer and clouds increase day-night temperature differences in hot Jupiters and result in non-isothermal upper atmospheres. In Chapter 4, I quantify how clouds and multiwavelength radiative transfer affect emission spectra and benchmark these differences against a new analysis of Spitzer phase curves of two canonical hot Jupiters. In Chapter 5, I model a warm Neptune with clouds and hazes to characterize the first ever JWST thermal phase curve. Finally, in Chapter 6 I conclude with a discussion of the future direction of the field of exoplanet atmospheric modeling. Additionally, I include two supplementary works that were completed concurrently with the above research on the helium enhancement of sub-Neptune mass atmospheres through fractionated mass loss.
- Subject Added Entry-Topical Term
- Astrophysics.
- Subject Added Entry-Topical Term
- Astronomy.
- Subject Added Entry-Topical Term
- Planetology.
- Index Term-Uncontrolled
- Exoplanet atmospheres
- Index Term-Uncontrolled
- General Circulation Models
- Index Term-Uncontrolled
- Emission spectra
- Index Term-Uncontrolled
- Jupiter
- Index Term-Uncontrolled
- Neptune
- Added Entry-Corporate Name
- University of Michigan Astronomy and Astrophysics
- Host Item Entry
- Dissertations Abstracts International. 86-03B.
- Electronic Location and Access
- 로그인을 한후 보실 수 있는 자료입니다.
- Control Number
- joongbu:656812
MARC
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■035 ▼a(MiAaPQ)umichrackham005683
■040 ▼aMiAaPQ▼cMiAaPQ
■0820 ▼a523
■1001 ▼aMalsky, Isaac.
■24510▼aModeling the Three-Dimensional Atmospheric Structure and Emission Spectra of Hot Gaseous Planets.
■260 ▼a[S.l.]▼bUniversity of Michigan. ▼c2024
■260 1▼aAnn Arbor▼bProQuest Dissertations & Theses▼c2024
■300 ▼a241 p.
■500 ▼aSource: Dissertations Abstracts International, Volume: 86-03, Section: B.
■500 ▼aAdvisor: Rauscher, Emily.
■5021 ▼aThesis (Ph.D.)--University of Michigan, 2024.
■520 ▼aAlthough thousands of exoplanets have been discovered, a relatively rare class of planets known as hot Jupiters has historically been critical to the advancement of the field. Hot Jupiters---massive gaseous planets with orbital semi-major axes less than ~0.05 au---are among the brightest and best candidates for atmospheric characterization. They are expected to be tidally locked, with constant day sides and constant night sides. Extreme temperature gradients drive supersonic winds, chemically diverse clouds form and dissipate in homogeneously, and hazes may blanket their atmospheres.In tandem with observations, simulations are critical to interpreting measurements, breaking degeneracies between different atmospheric physical and chemical structures, and showing how physical processes influence atmospheric circulation. The most comprehensive physics-driven models simulate full atmospheres and self-consistently show the resulting 3D chemical and physical structures. These models, known as General Circulation Models (GCMs), simulate radiative transfer, fluid dynamics, and other phenomena in planetary atmospheres.This thesis focuses on using numerical methods to characterize exoplanet atmospheres and expanding the physics within a GCM. Background to the field and an overview of GCMs is given in Chapter 1. In Chapter 2, I characterize how clouds and non-edge-on inclinations manifest in hot Jupiter emission spectra. In Chapter 3, I show that multiwavelength radiative transfer and clouds increase day-night temperature differences in hot Jupiters and result in non-isothermal upper atmospheres. In Chapter 4, I quantify how clouds and multiwavelength radiative transfer affect emission spectra and benchmark these differences against a new analysis of Spitzer phase curves of two canonical hot Jupiters. In Chapter 5, I model a warm Neptune with clouds and hazes to characterize the first ever JWST thermal phase curve. Finally, in Chapter 6 I conclude with a discussion of the future direction of the field of exoplanet atmospheric modeling. Additionally, I include two supplementary works that were completed concurrently with the above research on the helium enhancement of sub-Neptune mass atmospheres through fractionated mass loss.
■590 ▼aSchool code: 0127.
■650 4▼aAstrophysics.
■650 4▼aAstronomy.
■650 4▼aPlanetology.
■653 ▼aExoplanet atmospheres
■653 ▼aGeneral Circulation Models
■653 ▼aEmission spectra
■653 ▼aJupiter
■653 ▼aNeptune
■690 ▼a0596
■690 ▼a0606
■690 ▼a0590
■71020▼aUniversity of Michigan▼bAstronomy and Astrophysics.
■7730 ▼tDissertations Abstracts International▼g86-03B.
■790 ▼a0127
■791 ▼aPh.D.
■792 ▼a2024
■793 ▼aEnglish
■85640▼uhttp://www.riss.kr/pdu/ddodLink.do?id=T17164544▼nKERIS▼z이 자료의 원문은 한국교육학술정보원에서 제공합니다.
