IOP  Select  IOP Journals  For Authors  For Referees
Collected Articles from the Institute of Physics Login | Create account
HomeSearchPersonalization:E-mail AlertsFeedback
-> Display content by:SUBJECTJOURNALMONTH
ApJ 668 (2007 October 20) 1132-1139   doi: 10.1086/521347

A Three-Dimensional Deflagration Model for Type Ia Supernovae Compared with Observations


F. K. Röpke1,2,3, W. Hillebrandt1,3, W. Schmidt4, J. C. Niemeyer4, S. I. Blinnikov1,5 and P. A. Mazzali1,3,6
1 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, D-85741 Garching, Germany
2 Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064
3 Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106
4 Lehrstuhl für Astronomie und Astrophysik, Universität Würzburg, Am Hubland, D-97074 Würzburg, Germany
5 SSC RF ITEP, Bolshaya Cheremushkinskaya 25, 117218 Moscow, Russia
6 Istituto Nazionale di Astrofisica, OATs, via Tiepolo, 11, 34131 Trieste, Italy

ABSTRACT. A simulation of the thermonuclear explosion of a Chandrasekhar-mass C+O white dwarf, the most popular scenario of a Type Ia supernova (SN Ia), is presented. The underlying modeling is pursued in a self-consistent way, treating the combustion wave as a turbulent deflagration using well tested methods developed for laboratory combustion and based on the concept of "large-eddy simulations" (LESs). Such consistency requires to capture the onset of the turbulent cascade on resolved scales. This is achieved by computing the dynamical evolution on a 10243 moving grid, which resulted in the best-resolved three-dimensional SN Ia simulation carried out thus far, reaching the limits of what can be done on present supercomputers. Consequently, the model has no free parameters other than the initial conditions at the onset of the explosion, and therefore it has considerable predictive power. Our main objective is to determine to which extent such a simulation can account for the observations of normal SNe Ia. Guided by previous simulations with less resolution and a less sophisticated flame model, initial conditions were chosen that yield a reasonably strong explosion and a sufficient amount of radioactive nickel for a bright display. We show that observables are indeed matched to a reasonable degree. In particular, good agreement is found with the light curves of normal SNe Ia. Moreover, the model reproduces the general features of the abundance stratification as inferred from the analysis of spectra. This indicates that it captures the main features of the explosion mechanism of SNe Ia. However, we also show that even a seemingly best-choice pure deflagration model has shortcomings that indicate the need for a different mode of nuclear burning at late times, perhaps the transition to a detonation at low density.

Subject headings: hydrodynamics; instabilities; methods: numerical; supernovae: general; turbulence

Print publication: Issue 2 (2007 October 20)
Received 16 March 2007, accepted for publication 3 July 2007

   PDF (558 KB) | References | Articles citing this article
Setup information is available for Adobe Acrobat.
EndNote, ProCite ® and Reference Manager ® are registered trademarks of ISI Researchsoft.

Find related articles





 
Copyright © Institute of Physics and IOP Publishing Limited 2009.
Use of this service implies that the user has read and agrees to the terms and conditions of use.
Systematic downloading of files is prohibited.