2026-09-19T04:41:37Zhttps://ecommons.cornell.edu/server/oai/requestoai:ecommons.cornell.edu:1813/1030452026-05-15T19:47:57Zcom_1813_35col_1813_47
Kozakis, Thea
Kaltenegger, Lisa
Hayes, Alexander G.
Lloyd, James
Stacey, Gordon John
2021-03-12T17:41:51Z
2021-03-12T17:41:51Z
2020-08
ProQuest Submission ID: 12088
ProQuest Publication ID: 28024189
https://hdl.handle.net/1813/103045
https://doi.org/10.7298/4zk8-9661
13277834
172 pages
As a star evolves, the orbital distance where liquid water is possible on the surface of an Earth-like planet, the habitable zone, evolves as well. While stellar properties are relatively stable on the main sequence, post-main sequence evolution of a star involves significant changes in stellar temperature and radius, which is reflected in the changing irradiation at a specific orbital distance when the star becomes a red giant, and then later a white dwarf. To search planets in these systems for signs of life it is essential that we understand how stellar evolution influences atmospheric photochemistry along with detectable biosignatures. We use EXO-Prime, which consists of a 1D coupled climate/photochemistry and a line-by-line radiative transfer code, to model the atmospheres and spectra of habitable zone planets around red giants and white dwarfs, and assess the time dependency of detectable biosignatures.
en
Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/
Astrobiology
Biosignatures
Extraterrestrial life
Habitability
Stellar Evolution
Last Call for Life: Habitability of Terrestrial Planets Orbiting Red Giants and White Dwarfs
dissertation or thesis
https://catalog.library.cornell.edu/catalog/13277834
application/pdf
Astronomy and Space Sciences
Cornell University
Doctor of Philosophy
Ph. D., Astronomy and Space Sciences
https://hdl.handle.net/1813/59810
Publication
Cornell Theses and Dissertations
Kozakis, Thea
5893a6ea-7af3-41d7-abc6-04bcd26ab5df
open.access
open.access
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<Keyword>Astrobiology</Keyword>
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<Abstract>As a star evolves, the orbital distance where liquid water is possible on the surface of an Earth-like planet, the habitable zone, evolves as well. While stellar properties are relatively stable on the main sequence, post-main sequence evolution of a star involves significant changes in stellar temperature and radius, which is reflected in the changing irradiation at a specific orbital distance when the star becomes a red giant, and then later a white dwarf. To search planets in these systems for signs of life it is essential that we understand how stellar evolution influences atmospheric photochemistry along with detectable biosignatures. We use EXO-Prime, which consists of a 1D coupled climate/photochemistry and a line-by-line radiative transfer code, to model the atmospheres and spectra of habitable zone planets around red giants and white dwarfs, and assess the time dependency of detectable biosignatures.</Abstract>
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