| Issue |
J. Phys. Colloques
Volume 41, Number C2, Mars 1980
Physique de la Matière Dense / The Physics of Dense Matter
|
|
|---|---|---|
| Page(s) | C2-155 - C2-157 | |
| DOI | https://doi.org/10.1051/jphyscol:1980225 | |
J. Phys. Colloques 41 (1980) C2-155-C2-157
DOI: 10.1051/jphyscol:1980225
RAYLEIGH-TAYLOR CONVECTIVE OVERTURN AS A POSSIBLE SOLUTION TO THE SUPERNOVA PUZZLE
Mario Livio1, 2 et J. Robert Buchler1, 21 Department of physics and Astronomy University of Florida Gainesville, FL 32611
2 University of California Los Alamos Scienific Laboratory Los Alamos, NM 87545
Résumé
Au cours du collapse stellaire, la neutronisation intense au-dessus de la neutrinosphère crée un gradient de la concentration des électrons qui cause une instabilité de Rayleigh-Taylor d'ordre l=2. Il en résulte un chamboulement qui libère les neutrini emprisonnés dans le coeur de l'étoile qui eux à leur tour causent l'explosion violente de l'enveloppe stellaire.
Abstract
Strong neutronization above the neutrinosphere produces a convectively unstable gradient of the electron to baryon ratio Ye. An l = 2 Rayleigh-Taylor overturn of the whole core is expected to ensue. As a result the trapped neutrini are released on a short timescale, thus providing the necessary boost to cause a violent explosion. The final word for the growth of this instability calls for a full two-dimensional calculation. Such a study is now in progress. A one-dimensional hydrodynamic parametrization of the overturn shows that explosion results whenever mixing occurs significantly beyond the neutrinosphere. The main cause for explosion is energy deposition in the mantle by Comptonization as well as by absorption and re-emission. The Rayleigh-Taylor overturn of the core could thus well resolve the present puzzle of only marginally exploding supernova models.