Nickel bubble instability and mixing in SN 1987A

Details Nickel bubble instability and mixing in SN 1987A Nickel bubble instability and mixing in SN 1987A

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...425..264b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 425, no. 1, p. 264-273

Statistics

Computation

23

Bubbles, Computational Astrophysics, Dynamic Stability, Hydrodynamics, Nickel, Nuclear Fusion, Radioactive Decay, Supernova 1987A, Abundance, Emission Spectra, Line Spectra, Mathematical Models, Numerical Analysis, Stellar Models

Scientific paper

At least three stages where dynamical instabilities can cause macroscopic mixing have been identified in the hydrodynamics of SN 1987A. With a specific aim to investigate the mixing of Ni-56, we consider the latest stage which occurs in nickel bubbles inflated by heating due to the Ni-56 yields Co-56 yields Fe-56 radioactive decays. One-dimensional hydrodynamics simulations show that a snowplowed shell around each inflating blob of Ni-56 is Rayleigh-Taylor unstable and, after t approximately equals 3-5 days, should be broken and mixed into the expanding nickel in the form of O-C-He-H clumps. To evaluate the additional acceleration of nickel resulting from its percolation through the ruptured shell, we adopt a simple model based on the thin-shell snowplow approximation and a relaxation-type equation for the mass transfer by mixing. Our calculations indicate that, despite the beneficial role of mixing, the increase in the nickel radial velocity at the stage of nickel bubble instability is relatively modest and, when combined with the published results for the preceding stage of instabilities in SN 1987A, not sufficient to explain the observed Ni/Co/Fe velocities of approximately equal to 3000 km/s. The observed velocities could however be explained if the preceding stage ended (at t approximately equal to 104 s) by ejection of a few nickel clumps with masses Mn approximately equal to 0.1 MNi approximately equal to 0.007 solar mass and radial velocities approximately equal to 1800 km/s. The values of the Ni/Co/Fe volume filling factor, fn = 0.3-0.9, that we calculate with our model agree very well with those inferred by Li, McCray, & Sunyaev (1993) from the emission-line data.

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