자료유형  

 학위논문

Control Number  

0016934280

International Standard Book Number  

9798380167536

Dewey Decimal Classification Number  

530

Main Entry-Personal Name  

Hankla, Amelia M.

Publication, Distribution, etc. (Imprint  

[S.l.] : University of Colorado at Boulder., 2023

Publication, Distribution, etc. (Imprint  

Ann Arbor : ProQuest Dissertations & Theses, 2023

Physical Description  

1 online resource(233 p.)

General Note  

Source: Dissertations Abstracts International, Volume: 85-03, Section: B.

General Note  

Advisor: Uzdensky, Dmitri.

Dissertation Note  

Thesis (Ph.D.)--University of Colorado at Boulder, 2023.

Restrictions on Access Note  

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

Summary, Etc.  

요약The accretion disks and hot X-ray coronae surrounding black holes host plasmas spanning a wide range of parameter space. The plasma can be collisional or collisionless, depending on its location relative to the black hole and properties such as the accretion rate of surrounding material onto the black hole. In these plasmas, Coulomb collisions between electrons and protons can become inefficient, resulting in a two-temperature flow. In collisionless plasmas, magnetic turbulence and reconnection can accelerate particles to Lorentz factors of 1000 or more. Modeling these processes on scales of an entire disk/corona system is difficult computationally.In this thesis, I examine the large and small scales of black hole accretion disks and their collisionless coronae. I first study the fundamental process of how turbulence in a collisionless, magnetized coronal plasma changes in the context of an accretion disk/corona system. By driving turbulence with asymmetric energy injection, I show that the timescales for nonthermal particle acceleration depend on the injected energy's imbalance. I also propose a relativistic momentum-coupling mechanism that efficiently converts the driven electromagnetic energy into bulk kinetic energy of the plasma. Then, I demonstrate that nonthermal electrons should exist in the plunging region of a black hole. I use prescriptions from particle-in-cell simulations to build the electron distribution function within the plunging region. By ray-tracing the emission from these electrons, I show that nonthermal electrons within the plunging region create an observable power-law compatible with observations of black hole binaries in the soft spectral state. Finally, I examine two-temperature effects on the accretion disk as a whole. I probe how Coulomb collisions between protons and electrons can alter accretion disk structure, either through efficient collisions leading to disk collapse or through inefficient collisions leading to disk inflation. I contextualize these results in the framework of the disk truncation model for black hole binaries and examine the thick-to-thin disk transition as a function of accretion rate.

Subject Added Entry-Topical Term  

Plasma physics.

Subject Added Entry-Topical Term  

Astrophysics.

Subject Added Entry-Topical Term  

Physics.

Index Term-Uncontrolled  

Accretion disks

Index Term-Uncontrolled  

Black holes

Index Term-Uncontrolled  

Numerical simulations

Index Term-Uncontrolled  

Turbulence

Added Entry-Corporate Name  

University of Colorado at Boulder Physics

Host Item Entry  

Dissertations Abstracts International. 85-03B.

Host Item Entry  

Dissertation Abstract International

Electronic Location and Access  

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Control Number  

joongbu:641630