Surface Hydrogen-burning Modeling of Supersoft X-Ray Binaries: Are They Type Ia Supernova Progenitors?

摘要: Nova explosions occur on the white dwarf (WD) component of a cataclysmic variable stellar system that is accreting matter lost by companion. A Type Ia supernova (SN Ia) explosion thought to result when WD, in similar binary configuration, grows mass Chandrasekhar limit. Here, we present calculations accretion solar matter, at variety rates, onto hot (2.3 × 105 K), luminous (30 L☉), massive (1.25, 1.35 M☉) carbon-oxygen WDs. In contrast our nova simulations, where WD has low initial luminosity and thermonuclear runaway (TNR) occurs ejects material, these simulations do not eject material (or only small fraction accreted material), mass. hydrogen TNR does because fuses helium surface layers, call this process burning (SHB). As layer mass, it gradually either carbon oxygen or more nuclei, depending rate. If such were explode SN event, therefore, would show neither nor its spectrum as observed. Moreover, luminosities effective temperatures agree with observations some supersoft X-ray sources, results strengthen previous speculation them (CAL 83 CAL 87, for example) are probably progenitors explosions. Finally, have achieved SHB values rate almost span observed variables.