2010/04/15 by K. Pan, Kuo-Chuan Pan, P. M. Ricker +2 · 66 citations
Engineering · Mathematics · Physics and Astronomy · #Arithmetic #Astronomy #Astrophysics #Atomic physics #Binary number #Ejecta #Gamma-ray bursts and supernovae #Geology #Helium #Magnetic confinement fusion research #Mathematics #Nuclear reactor physics and engineering #Paleontology #Physics #Star (game theory) #Supernova #Type (biology) #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/715/1/78
published in The Astrophysical Journal 715(1), 78-85 (IOP Publishing) · Accepted in ApJ, 9 pages, 9 figures
arxiv created 2010/04/15 · openalex publication_date 2010/04/23 · arxiv updated 2015/05/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The impact of Type Ia supernova (SN) ejecta on a helium-star companion is investigated via high-resolution, two-dimensional hydrodynamic simulations. For a range of helium-star models and initial binary separations, it is found that the mass unbound in the interaction, δ M ub , is related to the initial binary separation, a , by a power law of the form δ M ub ∝ a m . This power-law index is found to vary from −3.1 to −4.0, depending on the mass of the helium star. The small range of this index brackets values found previously for hydrogen-rich companions, suggesting that the dependence of the unbound mass on orbital separation is not strongly sensitive to the nature of the binary companion. The kick velocity is also related to the initial binary separation by a power law with an index in a range from −2.7 to −3.3, but the power-law index differs from those found in previous studies for hydrogen-rich companions. The space motion of the companion after the SN is dominated by its orbital velocity in the pre-SN binary system. The level of Ni/Fe contamination of the companion resulting from the passage of the SN ejecta is difficult to estimate, but an upper limit on the mass of bound nickel is found to be ∼5 × 10 −4 M ☉ .