CC-SN ejecta: Dust-formation process.

Pumo M.L., Manicò G.
  Mercoledì 13/09   09:00 - 13:00   Aula A203   III - Astrofisica
One of the most persistent questions relating to dust production in the interstellar medium is whether core-collapse supernovae (CC-SNe) are significant contributors to the universal dust budget. Their role as dust producers has been first suggested about 40 years ago and has been supported in the recent years both by the existence of large amounts ($> 10^{8} M_{\odot}$) of dust in galaxies at redshifts $z >6$ and by the growing number of CC-SNe showing clear evidence of dust. Despite this, basic questions on the amount of dust produced by each event as well as on the nature and location of the dust still remain to be answered. With the aim of clarifying such questions and, consequently, of investigating in detail the role of the CC-SN events as dust producers, we have developed a specifically tailored numerical tool. This latter enables us to simulate the dust formation process in CC-SN ejecta in a "self-consistent" way, through the inclusion of the dust formation process following the theory of non-steady-state nucleation and grain growth developed by T. Nozawa $et al.$ in our new, general-relativistic, radiation-hydrodynamics, Lagrangian code. This latter is able to compute the "whole" evolution ($i.e.$, from the breakout of the shock wave at the stellar surface up to the so-called nebular stage) of the CC-SN ejecta and their luminosity. The tool features and some test case simulations will be discussed.