IS THERE A HIDDEN HOLE IN TYPE Ia SUPERNOVA REMNANTS?

Journal Article · Fri Jan 20 04:00:00 EST 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/745/1/75· OSTI ID:22011973

Garcia-Senz, D ^[1]; Badenes, C ^[2]; Serichol, N ^[3]

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1. Departament de Fisica i Enginyeria Nuclear, UPC, Compte d'Urgell 187, 08036 Barcelona (Spain)
2. School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978 (Israel)
3. Departament de Matematica Aplicada III, Sor Eulalia d'Anzizu, 08034 Barcelona (Spain)

In this paper, we report on the bulk features of the hole carved by the companion star in the material ejected during a Type Ia supernova (SN Ia) explosion. In particular we are interested in the long-term evolution of the hole as well as in its fingerprint in the geometry of the supernova remnant (SNR) after several centuries of evolution, which is a hot topic in current SN Ia studies. We use an axisymmetric smoothed particle hydrodynamics code to characterize the geometric properties of the SNR resulting from the interaction of this ejected material with the ambient medium. Our aim is to use SNR observations to constrain the single degenerate scenario for SN Ia progenitors. Our simulations show that the hole will remain open during centuries, although its partial or total closure at later times due to hydrodynamic instabilities is not excluded. Close to the edge of the hole, the Rayleigh-Taylor instability grows faster, leading to plumes that approach the edge of the forward shock. We also discuss other geometrical properties of the simulations, like the evolution of the contact discontinuity.

• OSTI ID: 22011973
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 745; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
AXIAL SYMMETRY
COMPUTERIZED SIMULATION
EXPLOSIONS
GALACTIC EVOLUTION
HYDRODYNAMICS
RAYLEIGH-TAYLOR INSTABILITY
STAR EVOLUTION
SUPERNOVA REMNANTS
SUPERNOVAE