Award Date

8-1-2014

Degree Type

Thesis

Degree Name

Master of Science (MS)

Department

Physics and Astronomy

First Committee Member

Kentaro Nagamine

Second Committee Member

Stephen Lepp

Third Committee Member

Daniel Proga

Fourth Committee Member

Balakrishnan Naduvalath

Number of Pages

61

Abstract

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.

Keywords

Galaxies – Formation; Galaxy formation; Mathematical models; Numerical simulations; SPH; Supernova; Supernovae

Disciplines

Astrophysics and Astronomy | External Galaxies | Physics

Language

English


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