Binary Star System Modeling of a Double White Dwarf System in the Planetary Nebula PN G012.1-11.2
Faculty Sponsor
Todd Hillwig
College
Arts and Sciences
Department/Program
Physics and Astronomy
Presentation Type
Poster Presentation
Symposium Date
Summer 7-24-2024
Abstract
Planetary nebulae are the ejected outer layers of dying stars. At the center of these planetary nebulae remains the cores of the dead stars that created them. These remaining cores eventually become what we call white dwarfs. In order to understand planetary nebulae, white dwarfs, and their origins we can study the remaining core, or central star, inside the planetary nebula. We can do this by determining the physical properties of these central stars. One way to do this is if the central star has a companion and thus is in a binary star system. So I modeled the central star of the planetary nebula PN G012.1-11.2 which has a binary star system at its center. Using the PHOEBE modeling software I was able to create models that I qualitatively matched to the light curve (brightness variations) of this system. These models allowed me to find a range of radii, masses and temperatures for the stars along with the inclination of the system's orbit. I will present the results of my modeling as well as discuss what it tells us about this particular object and how it helps us understand planetary nebulae and white dwarfs more broadly.
Recommended Citation
Shafer, Leah, "Binary Star System Modeling of a Double White Dwarf System in the Planetary Nebula PN G012.1-11.2" (2024). Summer Interdisciplinary Research Symposium. 189.
https://scholar.valpo.edu/sires/189
