Thesis (Ph. D.)--University of Rochester. Department of Physics and Astronomy, 2018.
Binary stars consist of more than 50 percent of the population of all-stars. Low-mass binary
systems may be the progenitors of many interesting objects, such as type Ia supernovae, luminous
red novae, planetary nebulae, and etc. For distant binary stars, they will evolve like two single
stars, for close binary stars, they may come into interaction if one or both of the stars grow in size
as they enter the giant branch. The giant stars can eject dense stellar wind that is slow in speed.
Some of the ejected materials can be captured by the companion under the influence of the
gravity and the other ejected materials leave the binary system also influenced - the morphology
of the ejecta is always asymmetric. Observations reveal that circumbinary disks, spiral structure,
and bipolar shaped outflows can be found in the different evolved binary systems. On the other
hand, the binary stars may get closer with the on-going mass transfer process and trigger more
violent orbital evolution and finally lead to the merging of the binaries. We aim to study the
mass ejection, mass transfer, morphology, and orbital evolution of the low-mass binary systems.
We mainly use AstroBEAR to carry out the 3-D numerical calculation.
