Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4303k&link_type=abstract
American Astronomical Society Meeting 208, #43.03; Bulletin of the American Astronomical Society, Vol. 38, p.117
Astronomy and Astrophysics
Astronomy
Scientific paper
Dust is one of the important ingredients in the universe; dust grains control the energy balance in a gas cloud through the interaction with radiation and gas, and play a crucial role in formation and evolution of stars and galaxies. Supernovae have been considered to be one of the sources of interstellar dust and the observations have confirmed formation of dust grains in the electa of core-collapsed supernovae. Also the detailed analysis of isotopic anomalies in presolar grains have suggested that dust grains form in the ejecta of SN Ia. How much amount and what kind of dust grains form in the ejecta of SNe have been still under debate and is the subject to be pursued to investigate the inventory of dust grains in the interstellar space. We present the results of the calculation of dust formation in the ejecta of supernovae, based on the models of Type II SN (Umeda and Nomoto, 2003) and Type Ia SN (Nomoto, 1997). In the ejecta of Type II SN with progenitor mass M_pr = 20 M_\odot, a variety of dust grains form in the electa according to the elemental composition at the site of formation; C grains in the He layer, Al_2O_3, MgO, MgSiO_3, Mg_2SiO_4 and SiO_2 grains in the O-Mg-Si layer, and Si, FeS, and Fe grains in the Si-S-Fe layer. The total mass of dust grains formed in the ejecta is 2-3 % of the progenitor mass. In the ejecta of Type Ia SN, the formation of dust grains is not feasible because of the large expansion velocity and the low gas density at the time of dust formation; C and Si grains could be condense but the efficiency of condensation be very low. We shall discuss the possibility of dust formation in the ejecta of Type Ia SNe.
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