Two Talks

astronomy logo

Calendar

Two Talks

Wednesday, May 04, 2022, 12:00pm - 01:00pm

This repeat is an exception to the normal repeat pattern

Nina Filippova, The University of Texas at Austin
Probing Multiscale Star Formation Theory Using Numerical Simulations

Abstract

Star formation involves a complex interplay of supersonic turbulence, magnetic fields, stellar feedback, and gravity. While observations yield empirical rules, it is difficult to formulate a comprehensive theory of star formation. Open questions include the inefficiency of star formation, as well as the origins of stellar clustering. Numerical simulations present a bridge between theory and observations. In this talk, I will present previous results from a suite of magnetohydrodynamics (MHD) simulations of star formation from giant molecular clouds (GMCs), aimed at quantifying the influence of turbulent and magnetic support on star formation efficiency and molecular cloud destruction. I will then discuss my current research on protostellar disk fragmentation as a possible mechanism for the formation of bound multiple stellar systems.

Margot Fitz Axen, The University of Texas at Austin
The Progenitors of Superluminous Type 1a Supernovae

Abstract

Type 1a Supernovae (SNe 1a) are common astrophysical transients and are used as cosmological distance probes because of the relative homogeneity of their light curves. While it is widely accepted that they originate from the thermonuclear explosion of a Carbon-Oxygen white dwarf (WD), the exact nature of their progenitors remains unknown. Recent observations have discovered a subclass of ’superluminous’ SNe 1a whose high luminosities suggest that they originate from the explosions of WDs with masses that exceed the Chandrasekhar mass limit, at which WD degeneracy pressure can no longer withstand gravity. Two models have been proposed to explain the progenitors of these explosions- a ‘magnetized WD’ model and a ‘WD merger’ model. To test the robustness of these models, we conduct a 1D numerical parameter survey of WD explosions using these models as initial conditions. We follow the explosions using the hydrodynamics code Castro and then use a radiative transport code to create light curves and spectra for the models. We compare the results of these simulations to observations and discuss which progenitor model is a better matc

Location: Online and PMA 15.216B