Master of Science (MS)
Physics and Astronomy
First Committee Member
Second Committee Member
Third Committee Member
Fourth Committee Member
Number of Pages
We implement and test a core-collapse Type II SN feedback that is physically motivated and produces good agreement with observations in galaxy formation simulations. The model includes both kinetic and thermal feedback, allowing wind particles to receive a velocity kick that mimics galactic winds and distributes mass and metallicity to the interstellar and intergalactic medium. We also include a phenomenological stellar feedback to study a possible enhancement of the efficiency of the SN-II feedback by creating lower-density ambient gas medium of the stellar populations by distribution of thermal energy. Our SN-II model is unique in the sense that it computes the wind velocity and the lifetime of a supernova remnant by considering its evolution with the Sedov-Taylor solution rather than taking them as constant values. We find that by combining SN-II and stellar feedback the model alleviates overcooling and missing satellites problems. The model also produces outflows without a need for turning off hydrodynamical interactions, cooling and star formation by hand. Our preliminary results with cosmological zoom-in simulations imply the new model successfully reproduces the stellar-to-halo mass ratio. We conclude that the Sedov-Taylor solution can be used to reasonably approximate the physical properties and evolutional time scales of supernova remnants in the galaxy formation numerical simulations.
Galaxies – Formation; Galaxy formation; Mathematical models; Numerical simulations; SPH; Supernova; Supernovae
Astrophysics and Astronomy | External Galaxies | Physics
Todoroki, Keita, "A Physically-Based Type II Supernova Feedback Model in SPH Simulations" (2014). UNLV Theses, Dissertations, Professional Papers, and Capstones. 2219.