The density structure surrounding the iron core of a massive star when it dies is known to
have a major effect on whether or not the star explodes. Here we repeat previous surveys of …

Classical novae are fascinating stellar explosions at the crossroads of stellar astrophysics,
nuclear physics, and cosmochemistry. In this review, we briefly summarize 30 years of …

Context. We have known for a long time that many of the measured white dwarf (WD)
masses in cataclysmic variables (CVs) significantly exceed the mean mass of single WDs …

Recent observations suggest our understanding of mass loss in classical novae is
incomplete, motivating a new theoretical examination of the physical processes responsible …

FLASH is a flexible, modular and parallel application code capable of simulating the
compressible, reactive flows found in many astrophysical environments. It is a collection of …

We report the discovery of a detached double white dwarf binary with an orbital period of≈
20.6 minutes, PTF J053332. 05+ 020911.6. The visible object in this binary, PTF J0533+ …

Context. High-resolution spectroscopy has revealed large concentrations of CNO and
sometimes other intermediate-mass elements (eg, Ne, Na, Mg, or Al, for ONe novae) in the …

Abstract We have simulated 2.5× 10 3 s of the late evolution of a 23 M☉ star with full
hydrodynamic behavior. We present the first simulations of a multiple-shell burning epoch …

Novae are cataclysmic variables driven by accretion of H-rich material onto a white dwarf
(WD) star from its low-mass main-sequence binary companion. New time-domain …

We present a study of Eulerian and Lagrangian statistics from a high-resolution numerical
simulation of isotropic and homogeneous turbulence using the FLASH code, with an …