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Topics on Planet-Disk Interaction an...

Dempsey, Adam Mahlon.

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Topics on Planet-Disk Interaction and Solar Convection.

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	Topics on Planet-Disk Interaction and Solar Convection./
作者:	Dempsey, Adam Mahlon.
出版者:	Ann Arbor : ProQuest Dissertations & Theses, : 2020,
面頁冊數:	177 p.
附註:	Source: Dissertations Abstracts International, Volume: 81-10, Section: B.
Contained By:	Dissertations Abstracts International81-10B.
標題:	Astrophysics. -
電子資源:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=27670403
ISBN:	9781658485289

Topics on Planet-Disk Interaction and Solar Convection.
Dempsey, Adam Mahlon.

Topics on Planet-Disk Interaction and Solar Convection. - Ann Arbor : ProQuest Dissertations & Theses, 2020 - 177 p.

Source: Dissertations Abstracts International, Volume: 81-10, Section: B.

Thesis (Ph.D.)--Northwestern University, 2020.

This item must not be sold to any third party vendors.

In this thesis I focus on two topics: planet-disk interaction and solar convection. These two seemingly separate topics are connected via a similar separation of timescales. Planets excite spiral waves in their disks on fast timescales compared to the time for the disk to viscously adjust to the angular momentum deposited by those waves. Similarly, in Solar convection, convective motions transport heat throughout the convective layer of the Sun on a much faster timescale than the entire entropy profile of the Sun adjusts to maintain a steady-state total heat flux. On the topic of planet-disk interaction I develop and simulate a slowly evolving steady-state solution which consists of a pileup of material behind the planet and a fully connected inner and outer disk -- despite the presence of a deep gap. The magnitude of this pileup sets the slow migration rate of the planet such that planet and pileup migrate together, always maintaining an overflowing solution. Moreover, I develop and implement a new angular momentum preserving sink prescription allowing Lagrangian hydrodynamics codes to attain this steady-state solution without the need for a cumbersome inner boundary. I also apply planet migration models to constrain the progenitor disk of the exoplanetary system GJ876 with a suite of N-body simulations, while taking advantage of adaptive mesh refinement methods to efficiently explore the large parameter space. On the topic of Solar convection, I calculate through simplified simulations the depth and thermal properties of the overshooting layer of the Sun, which is the region where convective motions penetrate into the stable layers.

ISBN: 9781658485289Subjects--Topical Terms:

535904
Astrophysics.
Subjects--Index Terms:

Accretion disks

Topics on Planet-Disk Interaction and Solar Convection.
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300 $a 177 p.
500 $a Source: Dissertations Abstracts International, Volume: 81-10, Section: B.
500 $a Advisor: Lithwick, Yoram.
502 $a Thesis (Ph.D.)--Northwestern University, 2020.
506 $a This item must not be sold to any third party vendors.
520 $a In this thesis I focus on two topics: planet-disk interaction and solar convection. These two seemingly separate topics are connected via a similar separation of timescales. Planets excite spiral waves in their disks on fast timescales compared to the time for the disk to viscously adjust to the angular momentum deposited by those waves. Similarly, in Solar convection, convective motions transport heat throughout the convective layer of the Sun on a much faster timescale than the entire entropy profile of the Sun adjusts to maintain a steady-state total heat flux. On the topic of planet-disk interaction I develop and simulate a slowly evolving steady-state solution which consists of a pileup of material behind the planet and a fully connected inner and outer disk -- despite the presence of a deep gap. The magnitude of this pileup sets the slow migration rate of the planet such that planet and pileup migrate together, always maintaining an overflowing solution. Moreover, I develop and implement a new angular momentum preserving sink prescription allowing Lagrangian hydrodynamics codes to attain this steady-state solution without the need for a cumbersome inner boundary. I also apply planet migration models to constrain the progenitor disk of the exoplanetary system GJ876 with a suite of N-body simulations, while taking advantage of adaptive mesh refinement methods to efficiently explore the large parameter space. On the topic of Solar convection, I calculate through simplified simulations the depth and thermal properties of the overshooting layer of the Sun, which is the region where convective motions penetrate into the stable layers.
590 $a School code: 0163.
650 4 $a Astrophysics. $3 535904
650 4 $a Computational physics. $3 3343998
650 4 $a Theoretical physics. $3 2144760
653 $a Accretion disks
653 $a Convection
653 $a Exoplanets
653 $a Planet-disk interaction
653 $a Protoplanetary disks
653 $a Solar physics
690 $a 0596
690 $a 0216
690 $a 0753
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793 $a English
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