Stellar Accretion Disks
Presenter(s)
Sarah E Krug
Files
Description
Many stars are found in binary systems. If the two stars' orbits are close enough together the more massive, or primary, star can pull matter from the less massive companion star. The stream of matter falling toward the primary forms an accretion disk around the star. The accretion disk, the matter that hits the star, and the orbital cycle of the system cause fluctuations in brightness that can be detected by telescope observations. A computer model of an accretion disk is presented that simulates some of the parameters that may affect brightness. The results will be compared to existing measurements of binary systems.
Publication Date
4-5-2017
Project Designation
Course Project - Graduate
Primary Advisor
Ivan Sudakov
Primary Advisor's Department
Physics
Keywords
Stander Symposium project
Recommended Citation
"Stellar Accretion Disks" (2017). Stander Symposium Projects. 1021.
https://ecommons.udayton.edu/stander_posters/1021
Comments
This poster reflects research conducted as part of a course project designed to give students experience in the research process.