자료유형  

 학위논문

Control Number  

0017165027

International Standard Book Number  

9798384462484

Dewey Decimal Classification Number  

523

Main Entry-Personal Name  

Vasquez, Gabriel.

Publication, Distribution, etc. (Imprint  

[S.l.] : The Ohio State University., 2024

Publication, Distribution, etc. (Imprint  

Ann Arbor : ProQuest Dissertations & Theses, 2024

Physical Description  

163 p.

General Note  

Source: Dissertations Abstracts International, Volume: 86-04, Section: B.

General Note  

Advisor: Hirata, Christopher.

Dissertation Note  

Thesis (Ph.D.)--The Ohio State University, 2024.

Summary, Etc.  

요약Hawking radiation sets stringent constraints on Primordial Black Holes (PBHs) as a dark matter candidate in the M~1016 g regime based on the evaporation products such as photons, electrons, and positrons. This motivates the need for rigorous modeling of the Hawking emission spectrum. Using semi-classical arguments, Page [Phys. Rev. D 16, 2402 (1977) showed that the emission of electrons and positrons is altered due to the black hole acquiring an equal and opposite charge to the emitted particle. The Poisson fluctuations of emitted particles cause the charge Z lel to random walk, but since acquisition of charge increases the probability of the black hole emitting another charged particle of the same sign as the charge of the black hole, the walk is biased toward Z=0, and P(Z) approaches an equilibrium probability distribution with finite variance (Z2). This thesis explores how this "stochastic charge" phenomenon arises from quantum electrodynamics (QED) on a Schwarzschild spacetime. We prove that (except for a small Fermi blocking term) the semi-classical variance (Z2) agrees with the variance of a quantum operator (Z2), where Z may be thought of as an "atomic number" that includes the black hole as well as charge near it (weighted by a factor of 2M/r). In QED, the fluctuations in Z do not arise from the black hole itself (whose charge remains fixed), but rather as a collective effect in the Hawking-emitted particles mediated by the long-range electromagnetic interaction. The rms charge (22)1/2 asymptotes to 3.44 at small PBH masses M ≤ 2 x 1016g, declining to 2.42 at M = 5.2 x 1017 g. Our construction also identifies which terms in the full QED Hamiltonian give rise to the stochastic charge effect, so that we can avoid "double counting as we work toward a full calculation of the corrections to Hawking radiation at order O (α), where α≈ 1/137 is the fine structure constant.As a secondary topic, we explore if resonances, quasi-bound states where the electron or positron is gravitationally bound to the black hole, alter the O (α) emission rate for both the photon and the electron/positron spectrum. We discovered transitions involving two resonant states, categorized colloquially as a bound-bound transition, are insignificant and are unable to be resolved when performing our integration across photon frequencies in order to derive the O (α) photon emission rate for dissipative interactions, processes that change the number of photons by one. We leave bound- free transitions, processes involving one resonant state and the other in a continuum, for future work. Additionally, we discovered the tunneling of resonant electrons and positrons through the potential barrier of the black hole plays a significant role towards altering the semi-classical electron and positron emission rate only for black holes within 6 x 1021 Mplanck where Mplanck is the Planck mass. The next step of our work is to incorporate this absorption process and numerically calculate the change to the semi-classical emission rate as first derived.

Subject Added Entry-Topical Term  

Astrophysics.

Subject Added Entry-Topical Term  

Physics.

Subject Added Entry-Topical Term  

Quantum physics.

Index Term-Uncontrolled  

Primordial Black Holes

Index Term-Uncontrolled  

Dark matter

Index Term-Uncontrolled  

Hawking radiation

Index Term-Uncontrolled  

Positron

Index Term-Uncontrolled  

Semi-classical electron

Added Entry-Corporate Name  

The Ohio State University Physics

Host Item Entry  

Dissertations Abstracts International. 86-04B.

Electronic Location and Access  

로그인을 한후 보실 수 있는 자료입니다.

Control Number  

joongbu:658528