2026-09-18T22:30:37Zhttps://dspace.mit.edu/server/oai/requestoai:dspace.mit.edu:1721.1/1003372022-01-13T07:54:07Zcom_1721.1_7582com_1721.1_7581col_1721.1_131024
David Kaiser.
Guardado, Karla (Karla M.)
Massachusetts Institute of Technology. Department of Physics.
Massachusetts Institute of Technology. Department of Physics
2015-12-16T16:32:58Z
2015-12-16T16:32:58Z
2015
2015
http://hdl.handle.net/1721.1/100337
930616159
Thesis: S.B., Massachusetts Institute of Technology, Department of Physics, 2015.
Cataloged from PDF version of thesis.
Includes bibliographical references (pages 37-38).
Cosmological inflation describes the phenomenon in the early universe when spacetime underwent a rapid, exponential expansion right after the Big Bang. Inflation solves the so-called "horizon problem," "flatness problem," and "monopole problem" of standard Big Bang cosmology. Furthermore, New Inflation solves the "graceful exit problem" of the original theory. In inflation, the energy density of a patch of the early universe becomes dominated by the potential energy of a scalar field in a state of false vacuum. This particular form of energy leads to a negative pressure, creating a repulsive gravitational force, driving the region into a period of exponential expansion. Soon after the end of inflation, the field oscillates, leading to the creation of particles in a process called reheating. If reheating begins with parametric resonance, the process is called preheating. New Higgs Inflation presumes that the Higgs field is the scalar field in question, involving a characteristic non-minimal "derivative" coupling. The equation of motion for the field evolves like a damped harmonic oscillator, so we expect it to oscillate near the end of inflation. We study the dynamics of the Higgs field during and after inflation and find that preheating should be efficient in this model.
by Karla Guardado.
S.B.
38 pages
eng
Massachusetts Institute of Technology
M.I.T. theses are protected by copyright. They may be viewed from this source for any purpose, but reproduction or distribution in any format is prohibited without written permission. See provided URL for inquiries about permission.
http://dspace.mit.edu/handle/1721.1/7582
Physics.
Preheating in new Higgs inflation
Thesis
application/pdf
Publication
unknown
unknown
<Publication xmlns="https://www.openaire.eu/cerif-profile/1.1/" id="7ee4368b-048d-4989-a70f-a7d0237f86ad">
<Type xmlns="https://www.openaire.eu/cerif-profile/vocab/COAR_Publication_Types">http://purl.org/coar/resource_type/c_1843</Type>
<Language>eng</Language>
<Title>Preheating in new Higgs inflation</Title>
<PublishedIn>
<Publication>
</Publication>
</PublishedIn>
<PublicationDate>2015</PublicationDate>
<Authors>
<Author>
<DisplayName>Guardado, Karla (Karla M.)</DisplayName>
<Affiliation>
<OrgUnit>
</OrgUnit>
</Affiliation>
</Author>
</Authors>
<Editors>
</Editors>
<Publishers>
<Publisher>
<DisplayName>Massachusetts Institute of Technology</DisplayName>
<OrgUnit />
</Publisher>
</Publishers>
<License>http://dspace.mit.edu/handle/1721.1/7582</License>
<Keyword>Physics.</Keyword>
<Abstract>Cosmological inflation describes the phenomenon in the early universe when spacetime underwent a rapid, exponential expansion right after the Big Bang. Inflation solves the so-called "horizon problem," "flatness problem," and "monopole problem" of standard Big Bang cosmology. Furthermore, New Inflation solves the "graceful exit problem" of the original theory. In inflation, the energy density of a patch of the early universe becomes dominated by the potential energy of a scalar field in a state of false vacuum. This particular form of energy leads to a negative pressure, creating a repulsive gravitational force, driving the region into a period of exponential expansion. Soon after the end of inflation, the field oscillates, leading to the creation of particles in a process called reheating. If reheating begins with parametric resonance, the process is called preheating. New Higgs Inflation presumes that the Higgs field is the scalar field in question, involving a characteristic non-minimal "derivative" coupling. The equation of motion for the field evolves like a damped harmonic oscillator, so we expect it to oscillate near the end of inflation. We study the dynamics of the Higgs field during and after inflation and find that preheating should be efficient in this model.</Abstract>
<Access xmlns="http://purl.org/coar/access_right"
>
</Access>
</Publication>