Instabilities and clumping in SN 1987A. I - Early evolution in two dimensions

Explosive Nucleosynthesis

“…The excitement induced by the above mentioned gamma-ray observations (together with many other observations at other wavelength ranges) has led the theorists to suggest different possibilities for mixing both during the explosion and the ejection phases (to quote only a few of the early works, see e.g., Arnett, Fryxell and Müller 1989, Benz and Thielemann 1990, Fryxell, Arnett and Müller 1991, and also the general reviews of SN 1987A from McCray 1993 andreferences therein (Georgii et al 2000). Although no detection has been obtained, these limits are restrictive enough to constrain some of the available models of SNeIa nucleosynthesis (like a sub-Chandrasekhar mass model from Nomoto et al 1997).…”

Supernova hydrodynamics experiments on Nova

“…This situation is unstable to the R.ayleigh-Taylor (RT) instability and perturbations at the interface grow in time. (Fryxell et al 1991;Miiller et al 1991) The experimental configuration adopted for these laser experiments is illustrated in F]g. 2a and is described in more depth eIaewhere (Remington et al 1995;Kane et al 199~Peyser et al 1995). Eight of the ten Nova laser beams at a duration of 1 ns and total energy of 12 kJ are focused into a 3.0 mm long, 1.6 mmdiameterAu hohlraum (cylindrical rrdation cavity) converting to a .-u 190 eV thermal x-ray drive.…”

“…2b we show the results of modeling in ID with HYADES, (Larsen & Lane 1994) and PROMETHEUS. (Fryxell et al 1991;Miiller et al 1991) HYADES is a lD Lagrangian code with multigroup ra&ation transport and tabular equation of state (EOS), and PROMETHEUS is a 3D Eulerian Piecewise Parabolic Method (PPM) code using (here) an ideal gas EOS. We use a measured radiation temperature, Tr(t)~as the source input to HYADES, and achieve an impulsive shock acceleration, followed by a protracted dderation, qualitatively similar to the He-H interface in the SN.…”

“…Eq. 6 of Miiller et al 1991), with total duration Ak of the growth: l/rein-< Attif or both cases. We intend to use this experiment to test the theories and models being used to pre&ct the behavior of SN 1987A, well in advance of the upcoming SN ejects-ring nebula impact.…”

Instabilities and Mixing in Type II-P and II-b Supernovae

“…This has stimulated 2D and 3D hydrodynamical calculations of the Rayleigh-Taylor (R-T) instabilities during supernova explosions for SN1987A (Arnett et al 1989;Hachisu et al 1990Hachisu et al , 1992Fryxell et al 1991;Miiller et al 1991;Den et al 1990;Yamada et al 1990;Yamada & Sato 1991;Herant & Benz 1991, type Ib/Ic supernovae (Hachisu et al , 1994a, type II-P supernovae (Herant &: Woosley 1994;Hachisu et al 1994b), and the type Il-b supernova 1993J (Iwamoto et al 1994). In particular, Hachisu et al ( , 1994a found that development of the R-T instabilities depend sensitively on the presupernova structure, so that the comparison between hydrodynamical simulations and observations can provide a new clue to the understanding of supernova progenitors, their structure, and the explosion mechanism.…”