On the evolution of rapidly rotating massive white dwarfs towards supernovae or collapses

Free access article

Issue		A&A Volume 435, Number 3, June I 2005


Page(s)		967 - 985
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361:20042542

A&A 435, 967-985 (2005)
DOI: 10.1051/0004-6361:20042542

On the evolution of rapidly rotating massive white dwarfs towards supernovae or collapses

S.-C. Yoon and N. Langer

Astronomical Institute, Utrecht University, Princetonplein 5, 3584 CC, Utrecht, The Netherlands
e-mail: scyoon@science.uva.nl; n.langer@astro.uu.nl

(Received 15 December 2004 / Accepted 1 February 2005 )

Abstract
A recent study indicated that the inner cores of rapidly accreting ( $\dot M > 10^{-7}~M_\odot~{\rm yr}^{-1}$ ) CO white dwarfs may rotate differentially, with a shear rate near the threshold value for the onset of the dynamical shear instability. Such differentially rotating white dwarfs have critical masses for thermonuclear explosion or electron-capture induced collapse that significantly exceed the canonical Chandrasekhar limit. Here, we construct two-dimensional differentially rotating white dwarf models with rotation laws resembling those of the one-dimensional models of the previous work. We derive analytic relations between the white dwarf mass, its angular momentum, and its rotational-, gravitational- and binding energy. We show that these relations are applicable for a wide range of angular velocity profiles, including solid body rotation. Taken at a central density of 2 $\times$ $10^9~{\rm g~cm}^{-3}$ they specify initial models for the thermonuclear explosion of rotating CO white dwarfs. At $\rho_{\rm c} = 10^{10}~{\rm g~cm}^{-3}$ and 4 $\times$ $10^9~{\rm g~cm}^{-3}$ , they give criteria for the electron-capture induced collapse of rotating CO and ONeMg white dwarfs, respectively. We demonstrate that pre-explosion and pre-collapse conditions of both rigidly and differentially rotating white dwarfs are well established by the present work, which may facilitate future multi-dimensional simulations of type Ia supernova explosions and studies of the formation of millisecond pulsars and gamma-ray bursts from collapsing white dwarfs. Our results lead us to suggest various possible evolutionary scenarios for progenitors of type Ia supernovae, leading to a new paradigm of a variable mass of exploding white dwarfs, at values well above the classical Chandrasekhar mass. Based on our 2D-models, we argue that the supernova peak brightness is proportional to the white dwarf mass, which could explain various aspects of the diversity of type Ia supernovae, such as their variation in brightness, the dependence of their mean luminosity on the host galaxy type, and the weak correlation between ejecta velocity and peak brightness.

Key words: stars: rotation -- stars: white dwarfs -- stars: neutron -- stars: supernovae: general -- gamma rays: bursts

SIMBAD Objects

What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access. An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.

If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
You can define your own OpenURL resolver with your EDPS Account. In this case your choice will be given priority over that of your library.
You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.