Modeling of Solar-Stellar Connections and the Heliophysics of Exoplanet Systems
| dc.contributor.advisor | Alexander, David | en_US |
| dc.creator | Farrish, Alison O. | en_US |
| dc.date.accessioned | 2021-05-03T20:53:59Z | en_US |
| dc.date.available | 2021-05-03T20:53:59Z | en_US |
| dc.date.created | 2021-05 | en_US |
| dc.date.issued | 2021-04-28 | en_US |
| dc.date.submitted | May 2021 | en_US |
| dc.date.updated | 2021-05-03T20:54:00Z | en_US |
| dc.description.abstract | In the past two and a half decades, advances in the field of exoplanet detection have confirmed more than 4,000 known planets outside of our Solar System \cite{exoplanets}. With this wealth of data, the field is now poised to transition from a phase of detection to one of more in-depth characterization of planetary processes and evolution. Exoplanet systems are of interest not only for the potential for habitability, but also in the opportunity they provide for the study of comparative heliophysics - the similarities and differences in physical interactions between the central host star and any associated planets. In applying solar- and heliophysics-based knowledge and tools to the study of exoplanet systems, we can expand our understanding of the breadth of possible star-planet interactions and the influence of stellar behavior on planetary environments and processes such as atmospheric loss, planetary magnetosphere dynamics, ionospheric emission, and more. We present here a series of studies of solar-stellar connections and the heliophysics of exoplanet systems, employing a surface flux transport treatment of photospheric flux emergence, migration, and dispersal, and the application of this solar-based modeling framework to exoplanet host stars. In Chapter 1, we describe the state of the field of exoplanet characterization, relevant solar physics concepts, and the context for making solar-stellar comparisons. Chapter 2 comprises the methodology employed in modeling stellar photospheres, coronae, and asterospheres with relevance to exoplanet space weather environments. Chapter 3 expands upon the solar-stellar connection, demonstrating the application of magnetic flux transport modeling to the simulation of stellar activity across a broad population of cool stars. Chapter 4 details our modeling of magnetic and energetic environments driving star-planet interaction. In Chapter 5, we present examples of applications of this work to planetary response modeling, detailed investigations of stellar extreme ultraviolet (EUV) emission, and young Sun analogs. Future applications of our integrated modeling approach, particularly in comparisons with solar dynamo models and upcoming observing campaigns from Parker Solar Probe and James Webb Space Telescope, are discussed in Chapter 6. | en_US |
| dc.format.mimetype | application/pdf | en_US |
| dc.identifier.citation | Farrish, Alison O.. "Modeling of Solar-Stellar Connections and the Heliophysics of Exoplanet Systems." (2021) Diss., Rice University. <a href="https://hdl.handle.net/1911/110394">https://hdl.handle.net/1911/110394</a>. | en_US |
| dc.identifier.uri | https://hdl.handle.net/1911/110394 | en_US |
| dc.language.iso | eng | en_US |
| dc.rights | Copyright is held by the author, unless otherwise indicated. Permission to reuse, publish, or reproduce the work beyond the bounds of fair use or other exemptions to copyright law must be obtained from the copyright holder. | en_US |
| dc.subject | solar physics | en_US |
| dc.subject | stellar physics | en_US |
| dc.subject | exoplanets | en_US |
| dc.subject | heliophysics | en_US |
| dc.title | Modeling of Solar-Stellar Connections and the Heliophysics of Exoplanet Systems | en_US |
| dc.type | Thesis | en_US |
| dc.type.material | Text | en_US |
| thesis.degree.department | Physics and Astronomy | en_US |
| thesis.degree.discipline | Natural Sciences | en_US |
| thesis.degree.grantor | Rice University | en_US |
| thesis.degree.level | Doctoral | en_US |
| thesis.degree.major | Solar and Space Physics | en_US |
| thesis.degree.name | Doctor of Philosophy | en_US |
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