Physics – Plasma Physics
Scientific paper
Nov 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..dppf3i103k&link_type=abstract
American Physical Society, Division of Plasma Physics Meeting, November 16-20, 1998 New Orleans, LA, abstract #F3I.1.03
Physics
Plasma Physics
Scientific paper
The role of hydrodynamic instabilities in core-collapse supernovae (SN) was dramatically highlighted 12 years ago when the night sky lit up in the southern hemisphere with the explosion of SN1987A in the Large Magellanic Cloud ( Arnett, D, Fryxell, B A, and Muller, E, ApJ 341), L63, (1989); Astron. Astrophys. 251, 505 (1991). . The radioactive core of the exploding star was observed to penetrate to the surface nearly a factor of two sooner than expected, and the astrophysics community turned an accusing eye to deep nonlinear hydrodynamic mixing. Subsequently, 2D modeling of the hydrodynamics of SN1987A has proceeded at a rapid pace, but little attention has been focused on testing whether the simulations were actually `correct'. In a new twist on high energy astrophysics, we are developing a SN hydrodynamics experimental testbed on the Nova laser ( Kane, J, et al.), ApJ 478, L75, (1997); Remington, B A et al., Phys. Plasmas 4, 1994 (1997). [See Kane et al., Electronic ApJ Letters, 478 (April 1, 1997)] with plans to extend this new capability to the Omega laser and to the NIF laser, when it becomes operational. In this talk, we will review the status of our `SN test stand', covering how we design the laser experiments, the scale transformation that links the laboratory experiments to the actual SN ( Ryutov, D et al)., submitted to ApJ (1998). , and the implications of our results for an improved understanding of core-collapse SN. A recurring theme in our talk will be the need for 3D modeling in the nonlinear regime ( Marinak, M M, et al)., PRL 75, 3677 (1995); PRL 80, 4426 (1998); Hecht J. et al., Laser Part. Beams 13, 423 (1995); Shvarts, D et al., Phys. Plasmas 2, 2465 (1995). for a quantitative understanding of the effects of hydrodynamic instabilities on SN evolution.
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