We present the first detailed study of the Electron Capture Supernova Channel ( ECSN Channel ) \added for a primary star in a close binary star system .
Progenitors of ECSN occupy the lower end of the mass spectrum of supernovae progenitors and are thought to form the transition between white dwarfs progenitors \deleted ( lower initial masses ) and core collapse progenitors \deleted ( higher initial masses ) . \deleted For single stars the mass range for ECSN is thought to be only 0.25 { M } _ { \odot } wide and located at an initial stellar mass of 8 - 10 { M } _ { \odot } .The mass range for ECSN from close binary systems is thought to be wider \added than the range for single stars , because of the effects of mass \replaced losstransfer on the helium core .
Using the MESA stellar evolution code \added we explored the parameter space of initial primary masses between 8 { M } _ { \odot } and 17 { M } _ { \odot } , using a large grid of models \deleted calculated a large grid of stellar models in the relevant parameter space various initial primary masses , secondary masses , periods and mass transfer efficiencies . \replaced We find that , in addition to the initial primary mass , the mass loss history is the most important factor in the final fate of stars in this mass range.We find that the initial primary mass and the mass transfer evolution are important factors in the final fate of stars in this mass range .
Mass \replaced losstransfer due to Roche Lobe overflow during and after carbon burning causes the core to cool down so that it avoids neon ignition , even in helium-free cores with masses up to 1.52 { M } _ { \odot } , which in single stars would \deleted certainly ignite neon . \replaced If the core is not able to recover from the effects of late mass \replaced losstransfer , it will continue to cool down and form a super-Chandrasekhar mass oxygen-neon white dwarf .
However , if the core is able to reverse the downward temperature trend , and to contract to high enough densities for electron captures to commence , If the core is able to contract to high enough densities for electron captures to commence , we find that , for the adopted Ledoux convection criterion , the initial mass range for the primary to evolve into an ECSN is between 13.5 { M } _ { \odot } and 17.6 { M } _ { \odot } \deleted with the range between 13.5 { M } _ { \odot } and 15.4 { M } _ { \odot } ( 1.9 { M } _ { \odot } wide ) consisting primarily of Case B systems and the range between 15.4 { M } _ { \odot } and 17.6 { M } _ { \odot } ( 2.2 { M } _ { \odot } wide ) consisting primarily of much less abundant Case A systems..
The mass ratio , initial period , and mass loss efficiency only marginally affect the predicted ranges .