Journal Article

Abundance stratification in Type Ia supernovae – III. The normal SN 2003du

Masaomi Tanaka, Paolo A. Mazzali, Vallery Stanishev, Immanuel Maurer, Wolfgang E. Kerzendorf and Ken'ichi Nomoto

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 410, issue 3, pages 1725-1738
Published in print January 2011 | ISSN: 0035-8711
Published online January 2011 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2010.17556.x
Abundance stratification in Type Ia supernovae – III. The normal SN 2003du

More Like This

Show all results sharing this subject:

  • Astronomy and Astrophysics

GO

Show Summary Details

Preview

The element abundance distributions in the ejecta of Type Ia supernova (SN) is studied by modelling a time series of optical spectra of SN 2003du until ∼1 yr after the explosion. Since SN 2003du is a very normal Type Ia SN both photometrically and spectroscopically, the abundance distribution derived for it can be considered as representative of normal Type Ia SNe. We find that the innermost layers are dominated by stable Fe-group elements, with a total mass of ∼0.2 M, which are synthesized through electron capture. Above the core of stable elements there are thick 56Ni-rich layers. The total mass of 56Ni is 0.65 M. The Si- and S-rich layers are located above the 56Ni-rich layers. The dominant element in the outermost layers (Mr > 1.1 M, v > 13 000 km s−1) is O, with a small amount of Si. Little unburned C remains, with an upper limit of 0.016 M. The element distributions in the ejecta are moderately mixed, but not fully mixed as seen in three-dimensional deflagration models.

Keywords: supernovae: general; supernovae: individual: SN 2003du; nuclear reactions, nucleosynthesis, abundances

Journal Article.  9624 words.  Illustrated.

Subjects: Astronomy and Astrophysics

Full text: subscription required

How to subscribe Recommend to my Librarian

Users without a subscription are not able to see the full content. Please, subscribe or login to access all content.